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Sample records for two-frequency ruby maser

  1. Energy levels and transition probability matrix elements of ruby for maser applications

    Science.gov (United States)

    Berwin, R. W.

    1971-01-01

    Program computes fine structure energy levels of ruby as a function of magnetic field. Included in program is matrix formulation, each row of which contains a magnetic field and four corresponding energy levels.

  2. Room-temperature solid-state maser.

    Science.gov (United States)

    Oxborrow, Mark; Breeze, Jonathan D; Alford, Neil M

    2012-08-16

    The invention of the laser has resulted in many innovations, and the device has become ubiquitous. However, the maser, which amplifies microwave radiation rather than visible light, has not had as large an impact, despite being instrumental in the laser's birth. The maser's relative obscurity has mainly been due to the inconvenience of the operating conditions needed for its various realizations: atomic and free-electron masers require vacuum chambers and pumping; and solid-state masers, although they excel as low-noise amplifiers and are occasionally incorporated in ultrastable oscillators, typically require cryogenic refrigeration. Most realizations of masers also require strong magnets, magnetic shielding or both. Overcoming these various obstacles would pave the way for improvements such as more-sensitive chemical assays, more-precise determinations of biomolecular structure and function, and more-accurate medical diagnostics (including tomography) based on enhanced magnetic resonance spectrometers incorporating maser amplifiers and oscillators. Here we report the experimental demonstration of a solid-state maser operating at room temperature in pulsed mode. It works on a laboratory bench, in air, in the terrestrial magnetic field and amplifies at around 1.45 gigahertz. In contrast to the cryogenic ruby maser, in our maser the gain medium is an organic mixed molecular crystal, p-terphenyl doped with pentacene, the latter being photo-excited by yellow light. The maser's pumping mechanism exploits spin-selective molecular intersystem crossing into pentacene's triplet ground state. When configured as an oscillator, the solid-state maser's measured output power of around -10 decibel milliwatts is approximately 100 million times greater than that of an atomic hydrogen maser, which oscillates at a similar frequency (about 1.42 gigahertz). By exploiting the high levels of spin polarization readily generated by intersystem crossing in photo-excited pentacene and other

  3. The Ruby programming language

    CERN Document Server

    Flanagan, David

    2008-01-01

    This book begins with a quick-start tutorial to the language, and then explains the language in detail from the bottom up: from lexical and syntactic structure to datatypes to expressions and statements and on through methods, blocks, lambdas, closures, classes and modules. The book also includes a long and thorough introduction to the rich API of the Ruby platform, demonstrating -- with heavily-commented example code -- Ruby's facilities for text processing, numeric manipulation, collections, input/output, networking, and concurrency. An entire chapter is devoted to Ruby's metaprogramming capabilities. The Ruby Programming Language documents the Ruby language definitively but without the formality of a language specification. It is written for experienced programmers who are new to Ruby, and for current Ruby programmers who want to challenge their understanding and increase their mastery of the language.

  4. Ruby under a microscope learning Ruby internals through experiment

    CERN Document Server

    Shaughnessy, Pat

    2013-01-01

    How Ruby Works Under the HoodRuby is a powerful programming language with a focus on simplicity, but beneath its elegant syntax it performs countless unseen tasks.Ruby Under a Microscope gives you a hands-on look at Ruby's core, using extensive diagrams and thorough explanations to show you how Ruby is implemented (no C skills required). Author Pat Shaughnessy takes a scientific approach, laying out a series of experiments with Ruby code to take you behind the scenes of how programming languages work. You'll even find information on JRuby and Rubinius (two alternative implementations of Ruby),

  5. Haystack-Ruby

    Energy Technology Data Exchange (ETDEWEB)

    2017-03-31

    The open source Project Haystack initiative defines meta data and communication standards related to data from buildings and intelligent devices. The Project Haystack REST API defines standard formats and operations for exchanging Haystack tagged data over HTTP. The HaystackRuby gem wraps calls to this REST API to enable Ruby application to easily integrate data hosted on a Project Haystack compliant server. The HaystackRuby gem was developed at the National Renewable Energy Lab to support applications related to campus energy. We hope that this tool may be useful to others.

  6. BioRuby: bioinformatics software for the Ruby programming language.

    Science.gov (United States)

    Goto, Naohisa; Prins, Pjotr; Nakao, Mitsuteru; Bonnal, Raoul; Aerts, Jan; Katayama, Toshiaki

    2010-10-15

    The BioRuby software toolkit contains a comprehensive set of free development tools and libraries for bioinformatics and molecular biology, written in the Ruby programming language. BioRuby has components for sequence analysis, pathway analysis, protein modelling and phylogenetic analysis; it supports many widely used data formats and provides easy access to databases, external programs and public web services, including BLAST, KEGG, GenBank, MEDLINE and GO. BioRuby comes with a tutorial, documentation and an interactive environment, which can be used in the shell, and in the web browser. BioRuby is free and open source software, made available under the Ruby license. BioRuby runs on all platforms that support Ruby, including Linux, Mac OS X and Windows. And, with JRuby, BioRuby runs on the Java Virtual Machine. The source code is available from http://www.bioruby.org/. katayama@bioruby.org

  7. The solid state maser

    CERN Document Server

    Orton, J W; Walling, J C; Ter Haar, D

    1970-01-01

    The Solid State Maser presents readings related to solid state maser amplifier from the first tentative theoretical proposals that appeared in the early 1950s to the successful realization of practical devices and their application to satellite communications and radio astronomy almost exactly 10 years later. The book discusses a historical account of the early developments (including that of the ammonia maser) of solid state maser; the properties of paramagnetic ions in crystals; the development of practical low noise amplifiers; and the characteristics of maser devices designed for communica

  8. Traveling-Wave Maser for 32 GHz

    Science.gov (United States)

    Shell, James; Clauss, Robert

    2009-01-01

    The figure depicts a traveling-wave ruby maser that has been designed (though not yet implemented in hardware) to serve as a low-noise amplifier for reception of weak radio signals in the frequency band of 31.8 to 32.3 GHz. The design offers significant improvements over previous designs of 32-GHz traveling-wave masers. In addition, relative to prior designs of 32-GHz amplifiers based on high-electron-mobility transistors, this design affords higher immunity to radio-frequency interference and lower equivalent input noise temperature. In addition to the basic frequency-band and low-noise requirements, the initial design problem included a requirement for capability of operation in a closed-cycle helium refrigerator at a temperature .4 K and a requirement that the design be mechanically simplified, relative to prior designs, in order to minimize the cost of fabrication and assembly. Previous attempts to build 32- GHz traveling-wave masers involved the use of metallic slow-wave structures comprising coupled transverse electromagnetic (TEM)-mode resonators that were subject to very tight tolerances and, hence, were expensive to fabricate and assemble. Impedance matching for coupling signals into and out of these earlier masers was very difficult. A key feature of the design is a slow-wave structure, the metallic portions of which would be mechanically relatively simple in that, unlike in prior slow-wave structures, there would be no internal metal steps, irises, or posts. The metallic portions of the slow-wave structure would consist only of two rectangular metal waveguide arms. The arms would contain sections filled with the active material (ruby) alternating with evanescent-wave sections. This structure would be transparent in both the signal-frequency band (the aforementioned range of 31.8 to 32.3 GHz) and the pump-frequency band (65.75 to 66.75 GHz), and would impose large slowing factors in both frequency bands. Resonant ferrite isolators would be placed in the

  9. Class I methanol masers: Masers with EGOs

    CERN Document Server

    Chen, Xi; Shen, Zhi-Qiang

    2009-01-01

    We have compared the results of a number of published class I methanol maser surveys with the catalogue of high-mass outflow candidates identified from the GLIMPSE survey (known as extended green objects or EGOs). We find class I methanol masers associated with approximately two-thirds of EGOs. Although the association between outflows and class I methanol masers has long been postulated on the basis of detailed studies of a small number of sources, this result demonstrates the relationship for the first time on a statistical basis. Despite the publication of a number of searches for class I methanol masers, a close physical association with another astrophysical object which could be targeted for the search is still lacking. The close association between class I methanol masers and EGOs therefore provides a large catalogue of candidate sources, most of which have not previously been searched for class I methanol masers. Interstellar masers and outflows have both been proposed to trace an evolutionary sequenc...

  10. BioRuby: Bioinformatics software for the Ruby programming language

    NARCIS (Netherlands)

    Goto, N.; Prins, J.C.P.; Nakao, M.; Bonnal, R.; Aerts, J.; Katayama, A.

    2010-01-01

    The BioRuby software toolkit contains a comprehensive set of free development tools and libraries for bioinformatics and molecular biology, written in the Ruby programming language. BioRuby has components for sequence analysis, pathway analysis, protein modelling and phylogenetic analysis; it suppor

  11. BioRuby : bioinformatics software for the Ruby programming language

    NARCIS (Netherlands)

    Goto, Naohisa; Prins, Pjotr; Nakao, Mitsuteru; Bonnal, Raoul; Aerts, Jan; Katayama, Toshiaki

    2010-01-01

    The BioRuby software toolkit contains a comprehensive set of free development tools and libraries for bioinformatics and molecular biology, written in the Ruby programming language. BioRuby has components for sequence analysis, pathway analysis, protein modelling and phylogenetic analysis; it suppor

  12. MacRuby Ruby and Cocoa on OS X

    CERN Document Server

    Aimonetti, Matt

    2011-01-01

    Want to build native Mac OS X applications with a sleek, developer-friendly alternative to Objective-C? MacRuby is an ideal choice. This in-depth guide shows you how Apple's implementation of Ruby gives you access to all the features available to Objective-C programmers. You'll get clear, detailed explanations of MacRuby, including quick programming techniques such as prototyping. Perfect for programmers at any level, this book is packed with code samples and complete project examples. If you use Ruby, you can tap your skills to take advantage of Interface Builder, Cocoa libraries, the Objec

  13. Ruby on Rails for dummies

    CERN Document Server

    Burd

    2007-01-01

    Quickly create Web sites with this poweful tool Use this free and easy programming language for e-commerce sites and blogs If you need to build Web and database applications quickly but you don''t dream in computer code, take heart! Ruby on Rails was created for you, and this book will have you up and running in no time. The Ruby scripting language and the Rails framework let you create full-featured Web applications fast. It''s even fun! Discover how toInstall and run Ruby and RailsUse the RadRails IDECreate a blog with RubyConnect your Web site to a databaseBuild a shopping cartExplore Ruby'

  14. Management plan : Ruby Lake National Wildlife refuge : Ruby Valley Nevada

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — The Ruby Lake NWR Management Plan (1986) consists of two parts; background information (location, history, environment, resources, administration, land status,...

  15. Hello Ruby adventures in coding

    CERN Document Server

    Liukas, Linda

    2015-01-01

    "Code is the 21st century literacy and the need for people to speak the ABCs of Programming is imminent." --Linda Liukas Meet Ruby--a small girl with a huge imagination. In Ruby's world anything is possible if you put your mind to it. When her dad asks her to find five hidden gems Ruby is determined to solve the puzzle with the help of her new friends, including the Wise Snow Leopard, the Friendly Foxes, and the Messy Robots. As Ruby stomps around her world kids will be introduced to the basic concepts behind coding and programming through storytelling. Learn how to break big problems into small problems, repeat tasks, look for patterns, create step-by-step plans, and think outside the box. With hands-on activities included in every chapter, future coders will be thrilled to put their own imaginations to work.

  16. Masers and VSOP-2

    Science.gov (United States)

    Elitzur, M.

    2009-08-01

    Maser studies where VSOP-2 can make its strongest impact involve proper motion measurements. In this talk I review outstanding issues in topics ranging from star forming regions to active galactic nuclei in which VSOP-2 proper motion measurements offer the promise of seminal contributions.

  17. Ruby on Rails: Up and Running

    CERN Document Server

    Tate, Bruce A

    2008-01-01

    This compact guide from O'Reilly teaches you the basics of Ruby on Rails, the super-productive new way to develop full-featured web applications. Discover how to install and use both the Ruby scripting language and the Rails framework. More advanced material shows you just how fast Ruby on Rails can go.

  18. FAST Maser Surveys

    Indian Academy of Sciences (India)

    J. S. Zhang

    2014-09-01

    FAST, the Five-hundred meter Aperture Spherical radio Telescope, will become the largest operating single-dish telescope in the coming years. It has many advantages: much better sensitivity for its largest collecting area; large sky coverage due to its innovative design of the active primary surface; extremely radio quiet from its unique location, etc. In this work, I will highlight the future capabilities of FAST to discover and observe both galactic and extragalactic masers.

  19. Recent Developments in Maser Theory

    CERN Document Server

    Elitzur, Moshe

    2007-01-01

    This review covers selected developments in maser theory since the previous meeting, "Cosmic Masers: From Proto-Stars to Black Holes" (Migenes & Reid 2002). Topics included are time variability of fundamental constants, pumping of OH megamasers and indicators for differentiating disks from bi-directional outflows.

  20. Passive maser development at NRL

    Science.gov (United States)

    White, J. D.; Frank, A.; Folen, V.

    1981-01-01

    The application of passive hydrogen masers to satellites was investigated. The NRL maser is of compact design suitable for the space environment. It is based on a dielectrically loaded sapphire cavity and uses a computer optimized set of four shields. The servo design is a phase sensitive method which directly measures the phase dispersion of the interrogating signal as it passes through the cavity.

  1. Studies of methanol maser rings

    CERN Document Server

    Bartkiewicz, A; van Langevelde, H J; De Buizer, J M; Pihlström, Y

    2011-01-01

    We present the results of studies of a new class of 6.7 GHz methanol maser sources with a ring-like emission structure discovered recently with the EVN. We have used the VLA to search for water masers at 22 GHz and radio continuum at 8.4 GHz towards a sample of high-mass star forming regions showing a ring-like distribution of methanol maser spots. Using the Gemini telescopes we found mid-infrared (MIR) counterparts of five methanol rings with a resolution of 0."15. The centres of methanol maser rings are located within, typically, only 0."2 of the MIR emission peak, implying their physical relation with a central star. These results strongly support a scenario wherein the ring-like structures appear at the very early stage of massive star formation before either water-maser outflows or H II regions are seen.

  2. Ruby fluorescence pressure scale: Revisited

    Science.gov (United States)

    Liu, Lei; Bi, Yan; Xu, Ji-An

    2013-05-01

    Effect of non-hydrostatic stress on X-ray diffraction in a diamond anvil cell (DAC) is studied. The pressure gradient in the sample chamber leads to the broadening of the diffraction peaks, which increase with the hkl index of the crystal. It is found that the difference between the determined d-spacing compressive ratio d/d0 and the real d-spacing compressive ratio dr/d0 is determined by the yield stress of the pressure transmitting media (if used) and the shear modulus of the sample. On the basis of the corrected experiment data of Mao et al. (MXB86), which was used to calibrate the most widely used ruby fluorescence scale, a new relationship of ruby fluorescence pressure scale is corrected, i.e., P = (1904/9.827)[(1 + Δλ/λ0)9.827-1].

  3. A two-Frequency RF Photocathode Gun

    Energy Technology Data Exchange (ETDEWEB)

    Dowell, D.H. E-mail: dowell@slac.stanford.edu; Ferrario, M.; Kimura, T.; Lewellen, J.; Limborg, C.; Raimondi, P.; Schmerge, J.F.; Serafini, L.; Smith, T.; Young, L

    2004-08-01

    In this paper we resurrect an idea originally proposed by Serafini (Nucl. Instr. and Meth. A 318 (1992) 301) in 1992 for an RF photocathode gun capable of operating simultaneously at the fundamental frequency and a higher frequency harmonic. Driving the gun at two frequencies with the proper field ratio and relative phase produces a beam with essentially no RF emittance and a linear longitudinal phase space distribution. Such a gun allows a completely new range of operating parameters for controlling space charge emittance growth. In addition, the linear longitudinal phase space distribution aids in bunch compression. This paper will compare results of simulations for the two-frequency gun with the standard RF gun and the unique properties of the two-frequency gun will be discussed.

  4. A Two-Frequency RF Photocathode Gun

    Energy Technology Data Exchange (ETDEWEB)

    Dowell, D.

    2004-11-05

    In this paper we resurrect an idea originally proposed by Serafini[1] in 1992 for an RF photocathode gun capable of operating simultaneously at the fundamental frequency and a higher frequency harmonic. Driving the gun at two frequencies with the proper field ratio and relative phase produces a beam with essentially no rf emittance and a linear longitudinal phase space distribution. Such a gun allows a completely new range of operating parameters for controlling space charge emittance growth. In addition, the linear longitudinal phase space distribution aids in bunch compression. This paper will compare results of simulations for the two-frequency gun with the standard rf gun, and the unique properties of the two-frequency gun will be discussed.

  5. CW SOLID-STATE OPTICAL MASER (LASER).

    Science.gov (United States)

    ruby rods, (3) Ruby oscillation linewidth, (4) Investigations of rare-earth spectra in yttrium aliminum garnets, (5) Nonlinear dielectric properties of KTaO3 near its Curie point, (6) The diffraction-limited oscillator. (Author)

  6. Far-infrared lasing in ruby

    Science.gov (United States)

    Lawandy, N. M.

    1979-01-01

    The feasibility of submillimeter wavelength (870 GHz) lasing in Al2O3 is discussed. The proposed scheme is based on the pumping of the 2A level of ruby via a ruby laser operating on its R2 line. Lasing is expected on the 2A to E transition of the split E-2 level.

  7. Water masers in dusty environments

    CERN Document Server

    Babkovskaia, N; Babkovskaia, Natalia; Poutanen, Juri

    2004-01-01

    We study in details a pumping mechanism for the lambda=1.35 cm maser transition 6_16 -> 5_23 in ortho-water based on the difference between gas and dust temperatures. The upper maser level is populated radiatively through 4_14 -> 5_05 and 5_05 -> 6_16 transitions. The heat sink is realized by absorbing the 45 mum photons, corresponding to the 5_23 -> 4_14 transition, by cold dust. We compute the inversion of maser level populations in the optically thick medium as a function of the hydrogen concentration, the gas-to-dust mass ratio, and the difference between the gas and the dust temperatures. The main results of numerical simulations are interpreted in terms of a simplified four-level model. We show that the maser strength depends mostly on the product of hydrogen concentration and the dust-to-water mass ratio but not on the size distribution of the dust particles or their type. We also suggest approximate formulae that describe accurately the inversion and can be used for fast calculations of the maser lumi...

  8. An Analysis of NTSC's Timekeeping Hydrogen Masers

    Science.gov (United States)

    Hui-jie, Song; Shao-wu, Dong; Zheng-ming, Wang; Li-li, Qu; Yue-juan, Jing; Wei, Li

    2016-10-01

    In this article, the hydrogen masers in the NTSC (National Time Service Center) timekeeping laboratory are tested. In order to avoid the impact of larger noise of caesium atomic clocks, TA(k) or UTC(k) is not used as reference, instead, the four hydrogen masers are mutually referred and tested. The frequency stability of hydrogen masers is analyzed using the four-cornered hat method, and the Allan standard deviations of each single hydrogen maser in different sample times are estimated. Then, according to the characteristics of hydrogen masers, by removing the trend term, excluding outliers, and smoothing the data with a mathematical method to separate the Gaussian noises of hydrogen masers, and finally by through the Kolmogorov-Smirnov test, the Gaussian noise of each hydrogen maser is estimated.

  9. Analysis of NTSC's Timekeeping Hydrogen Masers

    Science.gov (United States)

    Song, H. J.; Dong, S. W.; Wang, Z. M.; Qu, L. L.; Jing, Y. J.; Li, W.

    2015-11-01

    In this article, the hydrogen masers were tested in NTSC (National Time Service Center) keeping time laboratory. In order to avoid the impact of larger noise of caesium atomic clocks, TA(k) or UTC(k) was not used as reference, and four hydrogen masers were mutually referred and tested. The frequency stabilities of hydrogen masers were analyzed by using four-cornered hat method, and the Allan standard deviation of single hydrogen maser was estimated in different sampling time. Then according to the characteristics of hydrogen masers, by removing the trend term, excluding outliers, and smoothing data with mathematical methods to separate the Gaussian noise of hydrogen masers, and finally through the normal Kolmogorov-Smirnov test, a single hydrogen maser's Gaussian noise has been estimated.

  10. Ruby on Rails Issue Tracker

    Science.gov (United States)

    Rodriguez, Juan Jared

    2014-01-01

    The purpose of this report is to detail the tasks accomplished as a NASA NIFS intern for the summer 2014 session. This internship opportunity is to develop an issue tracker Ruby on Rails web application to improve the communication of developmental anomalies between the Support Software Computer Software Configuration Item (CSCI) teams, System Build and Information Architecture. As many may know software development is an arduous, time consuming, collaborative effort. It involves nearly as much work designing, planning, collaborating, discussing, and resolving issues as effort expended in actual development. This internship opportunity was put in place to help alleviate the amount of time spent discussing issues such as bugs, missing tests, new requirements, and usability concerns that arise during development and throughout the life cycle of software applications once in production.

  11. Simultaneous observation of water and class I methanol masers toward class II methanol maser sources

    CERN Document Server

    Kang, Hyunwoo; Byun, Do-Young; Lee, Seokho; Park, Yong-Sun

    2015-01-01

    We present a simultaneous single-dish survey of 22 GHz water maser and 44 GHz and 95 GHz class I methanol masers toward 77 6.7 GHz class II methanol maser sources, which were selected from the Arecibo methanol maser Galactic plane survey (AMGPS) catalog.Water maser emission is detected in 39 (51%) sources, of which 15 are new detections. Methanol maser emission at 44 GHz and 95 GHz is found in 25 (32%) and 19 (25%) sources, of which 21 and 13 sources are newly detected, respectively. We find 4 high-velocity (> 30 km/s) water maser sources, including 3 dominant blue- or redshifted outflows.The 95 GHz masers always appear with the 44 GHz maser emission. They are strongly correlated with 44 GHz masers in velocity, flux density, and luminosity, while they are not correlated with either water or 6.7 GHz class II methanol masers. The average peak flux density ratio of 95 GHz to 44 GHz masers is close to unity, which is two times higher than previous estimates. The flux densities of class I methanol masers are more ...

  12. IAU (Maser) Symposium 285 Summary

    CERN Document Server

    Menten, Karl M

    2012-01-01

    I'm trying to summarize the science communicated via oral presentations and by posters at the IAU Symposium 285 "Cosmic Masers - from OH to H_0", which took place from January 29 to February 3, 2012 in Stellenbosch, South Africa.

  13. OH Masers and Supernova Remnants

    CERN Document Server

    Wardle, Mark

    2012-01-01

    OH(1720 MHz) masers are created by the interaction of supernova remnants with molecular clouds. These masers are pumped by collisions in warm, shocked molecular gas with OH column densities in the range 10^{16}--10^{17} cm^{-2}. Excitation calculations suggest that inversion of the 6049 MHz OH line may occur at the higher column densities that have been inferred from main-line absorption studies of supernova remnants with the Green Bank Telescope. OH(6049 MHz) masers have therefore been proposed as a complementary indicator of remnant-cloud interaction. This motivated searches for 6049 MHz maser emission from supernova remnants using the Parkes 63 m and Effelsberg 100 m telescopes, and the Australia Telescope Compact Array. A total of forty-one remnants have been examined by one or more of these surveys, but without success. To check the accuracy of the OH column densities inferred from the single-dish observations we modelled OH absorption at 1667 MHz observed with the Very Large Array towards three supernov...

  14. Ruby Lake National Wildlife Refuge wildlife checklist

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Checklist with habitat, season, and abundance codes for wildlife species at Ruby Lake NWR. Includes bird, mammal, amphibian, reptile, and fish species.

  15. A search for extragalactic methanol masers

    CERN Document Server

    Ellingsen, S P; Whiteoak, J B; Vaile, R A; McCulloch, P M; Price, M

    1994-01-01

    A sensitive search for 6.7--GHz methanol maser emission has been made towards 10 galaxies that have yielded detectable microwave molecular--line transitions. These include several which show OH megamaser or superluminous \\water\\/ maser emission. Within the Galaxy, \\methanol\\/ and OH masers often occur in the same star formation regions and, in most cases, the \\methanol\\/ masers have a greater peak flux density than their OH counterparts. Thus we might expect \\methanol\\/ masers to be associated with extragalactic OH maser sources. We failed to detect any emission or absorption above our 60--mJy detection limit. We conclude that if the physical conditions exist to produce \\methanol\\/ megamaser emission, they are incompatible with the conditions which produce OH megamaser emission.

  16. Hydrogeology and water resources of Ruby Valley northeastern Nevada

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This water-resources evaluation of Ruby Valley was divided into two 3-year phases. Phase 1 was designed to quantify annual evapotranspiration (ET) from the Ruby Lake...

  17. The Ruby UCSC API: accessing the UCSC genome database using Ruby

    Directory of Open Access Journals (Sweden)

    Mishima Hiroyuki

    2012-09-01

    Full Text Available Abstract Background The University of California, Santa Cruz (UCSC genome database is among the most used sources of genomic annotation in human and other organisms. The database offers an excellent web-based graphical user interface (the UCSC genome browser and several means for programmatic queries. A simple application programming interface (API in a scripting language aimed at the biologist was however not yet available. Here, we present the Ruby UCSC API, a library to access the UCSC genome database using Ruby. Results The API is designed as a BioRuby plug-in and built on the ActiveRecord 3 framework for the object-relational mapping, making writing SQL statements unnecessary. The current version of the API supports databases of all organisms in the UCSC genome database including human, mammals, vertebrates, deuterostomes, insects, nematodes, and yeast. The API uses the bin index—if available—when querying for genomic intervals. The API also supports genomic sequence queries using locally downloaded *.2bit files that are not stored in the official MySQL database. The API is implemented in pure Ruby and is therefore available in different environments and with different Ruby interpreters (including JRuby. Conclusions Assisted by the straightforward object-oriented design of Ruby and ActiveRecord, the Ruby UCSC API will facilitate biologists to query the UCSC genome database programmatically. The API is available through the RubyGem system. Source code and documentation are available at https://github.com/misshie/bioruby-ucsc-api/ under the Ruby license. Feedback and help is provided via the website at http://rubyucscapi.userecho.com/.

  18. Ruby Lake National Wildlife Refuge : Ruby Valley Nevada : 1991 Annual water management report 1992 Annual water management plan

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Ruby Lake NWR 1991 Annual Water Management Report 1992 Annual Water Management Plan. Includes Ruby Lake 1991 weather summary, summary of 1991 water levels, water...

  19. Instant RubyMotion app development

    CERN Document Server

    Laborde, Gant

    2013-01-01

    Get to grips with a new technology, understand what it is and what it can do for you, and then get to work with the most important features and tasks. This book is a practical, task-based, step-by-step tutorial that will get you started with using RubyMotion to quickly and efficiently write iOS apps.To make the most of this book, you should understand the basics of programming concepts and have a basic understanding of a language similar to Ruby. If you are an Objective-C programmer, you'll learn the advantages of RubyMotion which can access the benefits of Cocoapods, but takes everything a st

  20. Accurate water maser positions from HOPS

    CERN Document Server

    Walsh, Andrew J; Longmore, Steven N; Breen, Shari L; Green, James A; Harvey-Smith, Lisa; Jordan, Christopher H; Macpherson, Christopher

    2014-01-01

    We report on high spatial resolution water maser observations, using the Australia Telescope Compact Array, towards water maser sites previously identified in the H2O southern Galactic Plane Survey (HOPS). Of the 540 masers identified in the single-dish observations of Walsh et al. (2011), we detect emission in all but 31 fields. We report on 2790 spectral features (maser spots), with brightnesses ranging from 0.06 Jy to 576Jy and with velocities ranging from -238.5 to +300.5km/s. These spectral features are grouped into 631 maser sites. We have compared the positions of these sites to the literature to associate the sites with astrophysical objects. We identify 433 (69 per cent) with star formation, 121 (19 per cent) with evolved stars and 77 (12 per cent) as unknown. We find that maser sites associated with evolved stars tend to have more maser spots and have smaller angular sizes than those associated with star formation. We present evidence that maser sites associated with evolved stars show an increased ...

  1. Practical reporting with Ruby and Rails

    CERN Document Server

    Berube, David

    2008-01-01

    Business intelligence and real time reporting mechanisms play a major role in any of today s forward looking business plans. With many of these solutions being moved to the Web, the popular Rails framework and its underlying Ruby language are playing a major role alongside web services in building the reporting solutions of tomorrow. Practical Reporting with Ruby and Rails is the first book to comprehensively introduce this popular framework, guiding readers through a wide ranging array of features. Note this isn t a staid guide to generating traditional reports, but rather it shows you how th

  2. Testing maser-based evolutionary schemes: A new search for 37.7-GHz methanol masers

    CERN Document Server

    Ellingsen, S P; Voronkov, M A; Dawson, J R

    2012-01-01

    We have used the Australia Telescope National Facility Mopra 22-m antenna to search for 37.7-GHz (7(-2) - 8(-1}E) methanol masers towards a sample of thirty six class II methanol masers. The target sources are the most luminous class II methanol masers not previously searched for this transition, with isotropic peak 12.2-GHz maser luminosity greater than 250 Jy/kpc^2 and isotropic peak 6.7-GHz maser luminosity greater than 800 Jy/kpc^2. Seven new 37.7-GHz methanol masers were detected as a result of the search. The detection rate for 37.7-GHz methanol masers towards a complete sample of all such class II methanol maser sites south of declination -20 deg is at least 30 percent. The relatively high detection rate for this rare methanol transition is in line with previous predictions that the 37.7-GHz transition is associated with a late stage of the class II methanol maser phase of high-mass star formation. We find that there is a modest correlation between the ratio of the 6.7- and 37.7-GHz maser peak intensit...

  3. Ruby Lake National Wildlife Refuge Ruby Valley, Nevada - Annual Narrative Report - Calendar Year 1996

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1996 calendar year. The report begins with a summary...

  4. Ruby Lake National Wildlife Refuge Ruby Valley, Nevada Annual Narrative Report Calendar Year 1981

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake outlines Refuge accomplishments during the 1981 calendar year. The report begins with a summary of the year's highlights...

  5. 1989 Annual water management plan : Ruby Lake National Wildlife Refuge : Ruby Valley Nevada

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Ruby Lake NWR 1988 Annual Water Management Report 1989 Annual Water Management Plan. Includes 1988 weather summary, water availability forecast, summary of 1988...

  6. The interstellar methanol masers and their environments

    Institute of Scientific and Technical Information of China (English)

    MAO; Ruiqing(毛瑞青); PEI; Chunchuan(裴春传); ZENG; Qin(曾琴)

    2003-01-01

    To promote the understanding of massive star formation processes, we have studied the 6.6 GHz methanol (CH3OH) masers and their environments-- the dense cores and the outer regions of the molecular cloud. The physics of the CH3OH maser or the thermal emission formation region is studied by fitting the observational data of the 6.6 GHz 51-60 A+ and the 107 GHz 31-40 A+ CH3OH maser emission, using the radiative transfer calculations. The type II characteristics of the 6.6 GHz CH3OH maser are confirmed by the calculation results. A greater intensity of the radiation field leads to an increase in the peak intensity of the maser; however, high densities tend to turn off the maser. The calculation results show that to be a maser the 6.6 GHz CH3OH emission needs a radiation field of 150-300 K and a density not higher than 107cm-3, while the 107 GHz emission requires a radiation field of 210-300 K and a density not higher than 3×106 cm-3. The 6.6 GHz line is maser towards all six studied sources, while the 107 GHz line is maser towards Cep A only. Moreover, the former's intensity is much stronger than the latter. The radiative transfer calculations also indicate that the 6.6 GHz maser emission is so strong that the requirements of its formation (e.g. The radiation field, the density and the kinetic parameters) can only be satisfied at a certain stage of the processes of the massive star formation. Therefore it is often used as one of the most prominent tracers for the massive star formation regions. The calculation results of the simultaneous observations of (1,1) through (4,4) inversion lines of the ammonia (NH3) indicate that both the temperature and the density in the 6.6 GHz CH3OH maser formation regions are higher than that of the NH3 line formation regions. Furthermore, the common fact of |Vlsr(CO)| > |Vlsr(NH3)| > |Vlsr(CH3OH 6.6GHz maser)| in all six sources implies the ongoing developing trends of those gas flows driven by the masers.

  7. Teaching Financial Literacy with Max and Ruby

    Science.gov (United States)

    Brown, Natalya; Ferguson, Kristen

    2017-01-01

    Teaching financial literacy is important at all stages of life, but is often neglected with elementary students. In this article, the authors describe a strategy for teaching financial literacy using the books about Max and Ruby by Rosemary Wells. These books can help introduce the five key concepts of financial literacy: scarcity, exchange,…

  8. The T-Ruby Design System

    DEFF Research Database (Denmark)

    Sharp, Robin; Rasmussen, Ole Steen

    1997-01-01

    This paper describes the T-Ruby system for designing VLSI circuits, starting from formal specifications in which they are described in terms of relational abstractions of their behaviour. The design process involves correctness-preserving transformations based on proved equivalences between...

  9. The T-Ruby design system

    DEFF Research Database (Denmark)

    Sharp, Robin; Rasmussen, Ole

    1995-01-01

    This paper describes the T-Ruby system for designing VLSI circuits, starting from formal specifications in which they are described in terms of relational abstractions of their behaviour. The design process involves correctness-preserving transformations based on proved equivalences between...

  10. Makit Lld: A Price above Rubies

    DEFF Research Database (Denmark)

    Hockerts, Kai; Jorem, Kaja; Walker Pedersen, Kristina

    2016-01-01

    "Makit Ltd: A Price Above Rubies" describes the development of a social entrepreneurial venture started by three young business school graduates. It follows the start-up process from their first idea identification, via the process of business plan writing, fund raising, to eventual start-up, and...

  11. Teaching Financial Literacy with Max and Ruby

    Science.gov (United States)

    Brown, Natalya; Ferguson, Kristen

    2017-01-01

    Teaching financial literacy is important at all stages of life, but is often neglected with elementary students. In this article, the authors describe a strategy for teaching financial literacy using the books about Max and Ruby by Rosemary Wells. These books can help introduce the five key concepts of financial literacy: scarcity, exchange,…

  12. Water Masers in the Andromeda Galaxy: II. Where Do Masers Arise?

    CERN Document Server

    Amiri, Nikta

    2016-01-01

    We present a comparative multi-wavelength analysis of water maser-emitting regions and non-maser-emitting luminous 24 micron star-forming regions in the Andromeda Galaxy (M31) to identify the sites most likely to produce luminous water masers useful for astrometry and proper motion studies. Included in the analysis are Spitzer 24 micron photometry, Herschel 70 and 160 micron photometry, H$\\alpha$ emission, dust temperature, and star formation rate. We find significant differences between the maser-emitting and non-maser-emitting regions: water maser-emitting regions tend to be more IR-luminous and show higher star formation rates. The five water masers in M31 are consistent with being analogs of water masers in Galactic star-forming regions and represent the high-luminosity tail of a larger (and as yet undetected) population. Most regions likely to produce water masers bright enough for proper motion measurements using current facilities have already been surveyed, but we suggest three ways to detect addition...

  13. Water masers in the Saturnian system

    Science.gov (United States)

    Pogrebenko, S. V.; Gurvits, L. I.; Elitzur, M.; Cosmovici, C. B.; Avruch, I. M.; Montebugnoli, S.; Salerno, E.; Pluchino, S.; Maccaferri, G.; Mujunen, A.; Ritakari, J.; Wagner, J.; Molera, G.; Uunila, M.

    2009-02-01

    Context: The presence of water has long been seen as a key condition for life in planetary environments. The Cassini spacecraft discovered water vapour in the Saturnian system by detecting absorption of UV emission from a background star. Investigating other possible manifestations of water is essential, one of which, provided physical conditions are suitable, is maser emission. Aims: We report detection of water maser emission at 22 GHz associated with several Kronian satellites using Earth-based radio telescopes. Methods: We searched for water maser emission in the Saturnian system in an observing campaign using the Metsähovi and Medicina radio telescopes. Spectral data were Doppler-corrected over orbital phase for the Saturnian satellites, yielding detections of water maser emission associated with the moons Hyperion, Titan, Enceladus, and Atlas. Results: The detection of Saturnian water molecules by remote astronomical observation can be combined with in situ spacecraft measurements to harmonise the physical model of the Saturnian system.

  14. Maser Astrometry with VLBI and the SKA

    CERN Document Server

    Green, James A; Brunthaler, Andreas; Ellingsen, Simon; Imai, Hiroshi; Vlemmings, Wouter; Reid, Mark; Richards, Anita

    2015-01-01

    We discuss the unique opportunities for maser astrometry with the inclusion of the Square Kilometre Array (SKA) in Very Long Baseline Interferometry (VLBI) networks. The first phase of the SKA will enable observations of hydroxyl and methanol masers, positioning the latter to an accuracy of 5 microarcseconds, and the second phase may allow water maser observations. These observations will provide trigonometric distances with errors as small as 1%. The unrivalled sensitivity of the SKA will enable large-scale surveys and, through joint operations, will turn any VLBI network into a fast astrometry device. Both evolved stars and high mass star formation regions will be accessible throughout the (Southern) Milky Way, completing our understanding of the content, dynamics and history of our Galaxy. Maser velocities and proper motions will be measurable in the Local Group of galaxies and beyond, providing new insights into their kinematics and evolution.

  15. Maser Radiation in an Astrophysical Context (Overview)

    CERN Document Server

    Gentry, Eric S

    2013-01-01

    In this paper we will look at the phenomenon of Microwave Amplification by Stimulated Emission of Radiation (a maser system). We begin by deriving amplification by stimulated emission using time-dependent perturbation theory, in which the perturbation provided by external radiation. When this perturbation is applied to an ensemble of particles exhibiting a population inversion, the result is stimulated microwave radiation. We will explore both unsaturated and saturated masers and compare their properties. By understanding their gain, as well as the effect of line broadening, astronomers are to identify astrophysical masers. By studying such masers, we gain new insight into poorly understood physical environments, particularly those around young and old stars, and compact stellar bodies.

  16. New OH Observations toward Northern Class I Methanol Masers

    Science.gov (United States)

    Val'tts, I. E.; Litovchenko, I. D.; Bayandina, O. S.; Alakoz, A. V.; Larionov, G. M.; Mukha, D. V.; Nabatov, A. S.; Konovalenko, A. A.; Zakharenko, V. V.; Alekseev, E. V.; Nikolaenko, V. S.; Kulishenko, V. F.; Odincov, S. A.

    2012-07-01

    Maser emission of OH(1720) is formed, according to modern concepts, under the influence of collisional pumping. Class I methanol masers (MMI) are also formed by a collisional mechanism of the inversion of the molecular levels. It is not excluded in this case that physical conditions in the condensations of the interstellar medium where masers are formed may be similar for MMI and OH(1720) masers, and they can associate with each other. To establish a possible association between these two kinds of masers, and obtain reliable statistical estimates, a survey of class I methanol masers at a frequency of 1720 MHz has been carried out.

  17. Ruby on Rails全景体验

    Institute of Scientific and Technical Information of China (English)

    Fikko

    2005-01-01

    Ruby On Rails是一个在Ruby语言的基础上开发的完整的web应用程序框架。谈到web应用程序框架.也许我们已经知道或熟悉的有很多种.比如著名的Java里的Struts,Spring Framework.Enterprise JavaBeans,C#里的Web Forms.PHP里的Prado等等。可是Ruby On Rails在问世仅仅一年,实际上为众人所知也不到半年的情况下.在web程序开发者中掀起了一场风暴。

  18. 37 GHz methanol masers : Horsemen of the Apocalypse for the class II methanol maser phase?

    CERN Document Server

    Ellingsen, S P; Sobolev, A M; Voronkov, M A; Caswell, J L; Lo, N

    2011-01-01

    We report the results of a search for class II methanol masers at 37.7, 38.3 and 38.5 GHz towards a sample of 70 high-mass star formation regions. We primarily searched towards regions known to show emission either from the 107 GHz class II methanol maser transition, or from the 6.035 GHz excited OH transition. We detected maser emission from 13 sources in the 37.7 GHz transition, eight of these being new detections. We detected maser emission from three sources in the 38 GHz transitions, one of which is a new detection. We find that 37.7 GHz methanol masers are only associated with the most luminous 6.7 and 12.2 GHz methanol maser sources, which in turn are hypothesised to be the oldest class II methanol sources. We suggest that the 37.7 GHz methanol masers are associated with a brief evolutionary phase (of 1000-4000 years) prior to the cessation of class II methanol maser activity in the associated high-mass star formation region.

  19. A gravitationally lensed water maser in the early Universe

    NARCIS (Netherlands)

    Impellizzeri, C. M. Violette; McKean, John P.; Castangia, Paola; Roy, Alan L.; Henkel, Christian; Brunthaler, Andreas; Wucknitz, Olaf

    2008-01-01

    Water masers are found in dense molecular clouds closely associated with supermassive black holes at the centres of active galaxies. On the basis of the understanding of the local water-maser luminosity function, it was expected that masers at intermediate and high redshifts would be extremely rare.

  20. Outward Motions of SiO Masers around VX Sgr

    Indian Academy of Sciences (India)

    J. B. Su; Z.-Q. Shen; X. Chen; D. R. Jiang

    2014-09-01

    We report the proper motions of SiO maser features around VX Sgr from the two-epoch VLBA observations (2006 December 15 and 2007 August 19). The majority of maser feature activities show a trend of outward motions. It is consistent with our previous finding that the outflow may play an important role for SiO maser pumping.

  1. Bolometric Luminosity Correction of H2O Maser AGNs

    Indian Academy of Sciences (India)

    Q. Guo; J. S. Zhang; J. Wang

    2014-09-01

    For the H2O maser host AGN sample, we derived their bolometric luminosity corrections, based on their X-ray data and [O III] emission line luminosities. Our results for maser AGNs is comparable to that of non-maser AGNs.

  2. Physical characteristics of bright Class I methanol masers

    Science.gov (United States)

    Leurini, S.; Menten, K. M.; Walmsley, C. M.

    2016-07-01

    Context. Class I methanol masers are thought to be tracers of interstellar shock waves. However, they have received relatively little attention mostly as a consequence of their low luminosities compared to other maser transitions. This situation has changed recently and Class I methanol masers are now routinely used as signposts of outflow activity especially in high extinction regions. The recent detection of polarisation in Class I lines now makes it possible to obtain direct observational information about magnetic fields in interstellar shocks. Aims: We make use of newly calculated collisional rate coefficients for methanol to investigate the excitation of Class I methanol masers and to reconcile the observed Class I methanol maser properties with model results. Methods: We performed large velocity gradient calculations with a plane-parallel slab geometry appropriate for shocks to compute the pump and loss rates which regulate the interactions of the different maser systems with the maser reservoir. We study the dependence of the pump rate coefficient, the maser loss rate, and the inversion efficiency of the pumping scheme of several Class I masers on the physics of the emitting gas. Results: We predict inversion in all transitions where maser emission is observed. Bright Class I methanol masers are mainly high-temperature (>100 K) high-density (n(H2) ~ 107-108 cm-3) structures with methanol maser emission measures, ξ, corresponding to high methanol abundances close to the limits set by collisional quenching. Our model predictions reproduce reasonably well most of the observed properties of Class I methanol masers. Class I masers in the 25 GHz series are the most sensitive to the density of the medium and mase at higher densities than other lines. Moreover, even at high density and high methanol abundances, their luminosity is predicted to be lower than that of the 44 GHz and 36 GHz masers. Our model predictions also reflect the observational result that the

  3. A novel capsular polysaccharide from Rhizobium rubi strain DSM 30149.

    Science.gov (United States)

    De Castro, Cristina; Fregolino, Eleonora; Gargiulo, Valentina; Lanzetta, Rosa; Parrilli, Michelangelo

    2008-07-07

    Rhizobium rubi, strain DSM 30149, is a Gram negative phytopathogenic bacterium which produces a linear polysaccharide with the following repeating unit: This new structure was determined by spectroscopical and chemical methods. It presents similar lipophilic features reported for another strain of R. rubi. These contrast with features already known for capsular polysaccharide species from symbiontic members of the Rhizobiaceae family, namely highly anionic polymers.

  4. Polarisation of Class II Methanol Masers

    CERN Document Server

    Stack, P D

    2011-01-01

    We have used the University of Tasmania Mt Pleasant 26m radio telescope to investigate the polarisation characteristics of a sample of strong 6.7 GHz methanol masers, the first spectral line polarisation observations to be undertaken with this instrument. As part of this process we have developed a new technique for calibrating linear polarisation spectral line observations. This calibration method gives results consistent with more traditional techniques, but requires much less observing time on the telescope. We have made the first polarisation measurements of a number of 6.7 GHz methanol masers and find linear polarisation at levels of a few - 10% in most of the sources we observed, consistent with previous results. We also investigated the circular polarisation produced by Zeeman splitting in the 6.7 GHz methanol maser G9.62+0.20 to get an estimate of the line of sight magnetic field strength of 35+/-7 mG.

  5. Rubi e safiras de Minas Gerais, Brasil

    Directory of Open Access Journals (Sweden)

    Antonio Liccardo

    2005-09-01

    Full Text Available Rubis e safiras de quatro depósitos em Minas Gerais, denominados Sapucaia, Indaiá e Palmeiras, na região de Caratinga-Manhuaçu, e Malacacheta, mais ao norte, foram caracterizados em termos geológicos, gemológicos, químicos e espectroscópicos, com o objetivo de interpretar causas de cor, gênese, bem como analisar o potencial econômico dos depósitos. Resultados de análises químicas e espectroscopia UV-visível mostram que a provável causa da cor azul é transferência de cargas entre Fe2+ e Ti4+, enquanto Cr3+ causa tonalidades violeta e púrpura, efeito alexandrita e fluorescência. A ausência de Ce e La e o teor relativamente mais alto de Ga distinguem as amostras de Malacacheta das demais. Além de sugerir particularidades genéticas, a diferença em termos de elementos-traços, pode ser utilizada como indicador de proveniência das gemas. Inclusões de um polimorfo de Al2SiO5 e indícios de campo sugerem que o coríndon deve ter sido gerado por processos metamórficos regionais, o que expande as possibilidades para a descoberta de novas ocorrências de rubi e safiras nos terrenos de alto grau metamórfico do leste de Minas Gerais.Rubies and sapphires from four deposits in Minas Gerais named Sapucaia, Indaiá and Palmeiras, in the region of Caratinga-Manhuaçu, and Malacacheta, farther north, were characterized in terms of geology, gemology, chemistry and spectroscopy in order to interpret causes of color and genesis. The economical potential of the deposits was also analyzed. Chemical analyses and UV-visible spectroscopy reveal that the probable cause of the blue color is a charge transfer between Fe2+ e Ti4+, while Cr3+ causes violet and purplish tints, alexandrite effect and fluorescence. Absence of Ce and La and relatively higher Ga-contents distinguish the Malacacheta samples from the others. Besides suggesting genetic particularities, the difference in terms of trace elements might be used as a provenience indicator for the

  6. Quantum electronics maser amplifiers and oscillators

    CERN Document Server

    Fain, V M; Sanders, J H

    2013-01-01

    Quantum Electronics, Volume 2: Maser Amplifiers and Oscillators deals with the experimental and theoretical aspects of maser amplifiers and oscillators which are based on the principles of quantum electronics. It shows how the concepts and equations used in quantum electronics follow from the basic principles of theoretical physics.Comprised of three chapters, this volume begins with a discussion on the elements of the theory of quantum oscillators and amplifiers working in the microwave region, along with the practical achievements in this field. Attention is paid to two-level paramagnetic ma

  7. The Revised Version of Class I Methanol Maser Catalog

    CERN Document Server

    Val'tts, I E; Bayandina, O S

    2010-01-01

    The revised version of the class I methanol maser catalog is presented. It contains 182 sources - new class I methanol masers detected in the direction of EGOs were added to the previous number (~160 sources have been published in the first version of this catalog - see reference in the text). Electronic version has been generated in the form of html file - http://www.asc.rssi.ru/MMI. A statistical analysis was carried out within 2' around a maser position to find an identification of class I methanol masers with any objects typical for star-forming regions - UCHII regions, IRAS sources, bipolar outflows, CS lines as of dense gas tracer, masers (class II methanol masers, OH and H2O) and EGO. None of the bipolar outflow, already registered in the direction of class I methanol maser, did not coincide with EGO. The result is submitted in a form of a diagram.

  8. Zeeman Effect in Ruby at High Pressures

    Science.gov (United States)

    Dan, Ioana

    2012-02-01

    We have developed a versatile fiber-coupled system for magneto-optical spectroscopy measurements at high pressure. The system is based on a miniature Cu-alloy Diamond Anvil Cell (from D'Anvils, Ltd) fitted with a custom-designed He gas-actuated membrane for in-situ pressure control, and coupled with a He transfer cryostat incorporating a superconducting magnet (from Quantum Designs). This system allows optical measurements (Raman, photoluminescence, reflectivity) within wide ranges of pressures (up to 100GPa), temperatures (4.2-300K) and magnetic fields (0-9T). We employ this system to examine the effect of pressure and non-hydrostatic stress on the Zeeman split d-d transitions of Cr^3+ in ruby (Al2O3: Cr^3+). We determine the effect of pressure and non-hydrostaticity on the trigonal crystal field in this material, and discuss the use of the Zeman-split ruby fluorescence as a possible probe for deviatoric stresses in diamond anvil cell experiments.

  9. A search for water masers associated with class II methanol masers - II. Longitude range 341$^{\\circ}$ to 6$^{\\circ}$

    CERN Document Server

    Titmarsh, A M; Breen, S L; Caswell, J L; Voronkov, M A

    2016-01-01

    This is the second paper in a series of catalogues of 22-GHz water maser observations towards the 6.7-GHz methanol masers from the Methanol Multibeam (MMB) Survey. In this paper we present our water maser observations made with the Australia Telescope Compact Array towards the masers from the MMB survey between l = 341$^{\\circ}$ through the Galactic centre to l = 6$^{\\circ}$. Of the 204 6.7-GHz methanol masers in this longitude range we found 101 to have associated water maser emission (~ 50 per cent). We found no difference in the 6.7-GHz methanol maser luminosities of those with and without water masers. In sources where both maser species are observed, the luminosities of the methanol and water masers are weakly correlated. Studying the mid-infrared colours from GLIMPSE we found no differences between the colours of those sources associated with both methanol and water masers and those associated with just methanol. Comparing the column density and dust mass calculated from the 870-micron thermal dust emis...

  10. From Java to Ruby things every manager should know

    CERN Document Server

    Tate, Bruce

    2006-01-01

    As a development team, you want to be productive. You want to write flexible, maintainable web applications. You want to use Ruby and Rails. But can you justify the move away from established platforms such as J2EE? Bruce Tate's From Java to Ruby has the answers, and it expresses them in a language that'll help persuade managers and executives who've seen it all. See when and where the switch makes sense, and see how to make it. If you're trying to adopt Ruby in your organization and need some help, this is the book for you. Based on a decision tree (a concept familiar to managers and executives,) Java to Ruby stays above the low-level technical debate to examine the real benefits and risks to adoption. Java to Ruby is packed with interviews of Ruby customers and developers, so you can see what types of projects are likely to succeed, and which ones are likely to fail. Ruby and Rails may be the answer, but first you need to be sure you're asking the right question. By addressing risk and fitness of purpose, J...

  11. Ruby in a nutshell a desktop quick reference

    CERN Document Server

    Matsumoto, Yukihiro

    2002-01-01

    Ruby is an absolutely pure object-oriented scripting language written in C and designed with Perl and Python capabilities in mind. While its roots are in Japan, Ruby is slowly but surely gaining ground in the US. The goal of Yukihiro Matsumoto, creator of Ruby and author of this book, is to incorporate the strengths of languages like Perl, Python, Lisp and Smalltalk. Ruby is a genuine attempt to combine the best of everything in the scripting world. Since 1993, Ruby mailing lists have been established, Web pages have formed, and a community has grown around it. The language itself is very good at text processing and is notable for its broad object orientation. Ruby is portable and runs under GNU/Linux (and other Unices) as well as DOS, MS Windows and Mac. With Ruby in a Nutshell, Matsumoto offers a practical reference to the features of this new language including the command-line options, syntax, built-in variables, functions, and many commonly used classes and modules. This guide covers the current stable ...

  12. W43A: a Maverick Maser Source

    Science.gov (United States)

    Diamond, P. J.; Nyman, L. Å.

    The authors report on some preliminary results from a multi-epoch monitoring project of the OH and H2O masers in the source W43A. Their results suggest that W43A is a very young stellar object which has just entered a strong stellar wind stage.

  13. OH masers associated with IRAS point sources

    NARCIS (Netherlands)

    Masheder, MRW; Cohen, RJ; Martin-Hernandez, NL; Migenes,; Reid, MJ

    2002-01-01

    We report a search for masers from the Lambda-doublet of the ground-state of OH at 18cm, carried out with the Jodrell Bank Lovell Telescope and with the 25m Dwingeloo telescope. All objects north of delta = -20degrees which appear in the IRAS Point Source Catalog with fluxes > 1000 Jy at 60mum and

  14. Ruby-based inorganic scintillation detectors for 192Ir brachytherapy

    Science.gov (United States)

    Kertzscher, Gustavo; Beddar, Sam

    2016-11-01

    We tested the potential of ruby inorganic scintillation detectors (ISDs) for use in brachytherapy and investigated various unwanted luminescence properties that may compromise their accuracy. The ISDs were composed of a ruby crystal coupled to a poly(methyl methacrylate) fiber-optic cable and a charge-coupled device camera. The ISD also included a long-pass filter that was sandwiched between the ruby crystal and the fiber-optic cable. The long-pass filter prevented the Cerenkov and fluorescence background light (stem signal) induced in the fiber-optic cable from striking the ruby crystal, which generates unwanted photoluminescence rather than the desired radioluminescence. The relative contributions of the radioluminescence signal and the stem signal were quantified by exposing the ruby detectors to a high-dose-rate brachytherapy source. The photoluminescence signal was quantified by irradiating the fiber-optic cable with the detector volume shielded. Other experiments addressed time-dependent luminescence properties and compared the ISDs to commonly used organic scintillator detectors (BCF-12, BCF-60). When the brachytherapy source dwelled 0.5 cm away from the fiber-optic cable, the unwanted photoluminescence was reduced from  >5% to  5% within 10 s from the onset of irradiation and after the source had retracted. The ruby-based ISDs generated signals of up to 20 times that of BCF-12-based detectors. The study presents solutions to unwanted luminescence properties of ruby-based ISDs for high-dose-rate brachytherapy. An optic filter should be sandwiched between the ruby crystal and the fiber-optic cable to suppress the photoluminescence. Furthermore, we recommend avoiding ruby crystals that exhibit significant time-dependent luminescence.

  15. A gravitationally lensed water maser in the early Universe.

    Science.gov (United States)

    Impellizzeri, C M Violette; McKean, John P; Castangia, Paola; Roy, Alan L; Henkel, Christian; Brunthaler, Andreas; Wucknitz, Olaf

    2008-12-18

    Water masers are found in dense molecular clouds closely associated with supermassive black holes at the centres of active galaxies. On the basis of the understanding of the local water-maser luminosity function, it was expected that masers at intermediate and high redshifts would be extremely rare. However, galaxies at redshifts z > 2 might be quite different from those found locally, not least because of more frequent mergers and interaction events. Here we use gravitational lensing to search for masers at higher redshifts than would otherwise be possible, and find a water maser at redshift 2.64 in the dust- and gas-rich, gravitationally lensed type-1 quasar MG J0414+0534 (refs 6-13). The isotropic luminosity is 10,000 (, solar luminosity), which is twice that of the most powerful local water maser and half that of the most distant maser previously known. Using the locally determined luminosity function, the probability of finding a maser this luminous associated with any single active galaxy is 10(-6). The fact that we see such a maser in the first galaxy we observe must mean that the volume densities and luminosities of masers are higher at redshift 2.64.

  16. Ruby and sapphire from Jegdalek, Afghanistan

    Science.gov (United States)

    Bowersox, G.W.; Foord, E.E.; Laurs, B.M.; Shigley, J.E.; Smith, C.P.

    2000-01-01

    This study provides detailed mining and gemological information on the Jegdalek deposit, in east-central Afghanistan, which is hosted by elongate beds of corundum-bearing marble. Some facet-grade ruby has been recovered, but most of the material consists of semitransparent pink sapphire of cabochon or carving quality. The most common internal features are dense concentrations of healed and nonhealed fracture planes and lamellar twin planes. Color zoning is common, and calcite, apatite, zircon, mica, iron sulfide minerals, graphite, rutile, aluminum hydroxide, and other minerals are also present in some samples. Although the reserves appear to be large, future potential will depend on the establishment of a stable government and the introduction of modern mining and exploration techniques. ?? 2000 Gemological Institute of America.

  17. The growth of ruby single crystals

    Directory of Open Access Journals (Sweden)

    ALEKSANDAR GOLUBOVIC

    2005-02-01

    Full Text Available Ruby (Cr:Al2O3 single crystals were grown by the Czochralski technique in an argon atmosphere. The critical crystal diameter dc = 1.0 cm and the critical rate of rotation wc = 20 rpm were calculated by equations of the hydrodynamics of the melt. The rate of crystal growthwas experimentally obtained to be 2.7 mm/h. For chemical polishing, conc. H3PO4 at 593 K for an exposure of 3 hours was determined. Conc. H3PO4 at 523 K for an exposure of 3 h was found to be a suitable etching solution. The lattice parameters a = 0.47627(6 nm and c = 1.301(1 nm were determined by X-ray powder diffraction. The obtained results are discussed and compared with published data.

  18. Continuum emission associated with 6.7-GHz methanol masers

    CERN Document Server

    Ellingsen, S P; McCulloch, P M

    1995-01-01

    We have used the Australia Telescope Compact Array (ATCA) to search for continuum emission toward three strong 6.7-GHz methanol maser sources. For two of the sources, G339.88-1.26 and NGC 6334F (G351.42+0.64), we detect continuum emission closely associated with the methanol masers. A further three clusters of masers showed no radio continuum emission above our sensitivity limit of 1-5 mJy. We find the position of the 6.7-GHz methanol masers in G339.88-1.26 to be consistent with the hypothesis that the masers lie in the circumstellar disc surrounding a massive star. We also argue that one of the clusters of methanol masers in NGC 6334F provides indirect observational support for the circumstellar disc hypothesis.

  19. Investigating high-mass star formation through maser surveys

    CERN Document Server

    Ellingsen, S P; Cragg, D M; Sobolev, A M; Breen, S L; Godfrey, P D

    2007-01-01

    Interstellar masers are unique probes of the environments in which they arise. In studies of high-mass star formation their primary function has been as signposts of these regions and they have been used as probes of the kinematics and physical conditions in only a few sources. With a few notable exceptions, we know relatively little about the evolutionary phase the different maser species trace, nor their location with respect to other star formation tracers. While detailed studies of a small number of maser regions can reveal much about them, other information can only be obtained through large, systematic searches. In particular, such surveys are vital in efforts to determine an evolutionary sequence for the common maser species, and there is growing evidence that methanol masers may trace an earlier phase than the other common maser species of OH and water.

  20. Ground-state OH maser distributions in the Galactic Centre region

    CERN Document Server

    Qiao, Hai-Hua; Shen, Zhi-Qiang; Dawson, Joanne R

    2016-01-01

    Ground-state OH masers identified in the Southern Parkes Large-Area Survey in Hydroxyl were observed with the Australia Telescope Compact Array to obtain positions with high accuracy ($\\sim$1\\,arcsec). We classified these OH masers into evolved star OH maser sites, star formation OH maser sites, supernova remnant OH maser sites, planetary nebula OH maser sites and unknown maser sites using their accurate positions. Evolved star and star formation OH maser sites in the Galactic Centre region (between Galactic longitudes of $-5^{\\circ}$ to $+5^{\\circ}$ and Galactic latitudes of $-2^{\\circ}$ and $+2^{\\circ}$) were studied in detail to understand their distributions.

  1. Ruby Lake National Wildlife Refuge Narrative report: September - December, 1959

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1959. The report begins by...

  2. Ruby Lake National Wildlife Refuge Narrative report: September - December, 1961

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1961. The report begins by...

  3. The Trail Inventory of Ruby Lake NWR [Cycle 3

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — The purpose of this report is to create a baseline inventory of all non-motorized trails on Ruby Lake National Wildlife Refuge. Trails in this inventory are eligible...

  4. Ruby Lake National Wildlife Refuge Narrative report: January - April, 1953

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1953. The report begins by summarizing the weather...

  5. Ruby Lake National Wildlife Refuge Narrative Report January - April 1960

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1960. The report begins by summarizing the weather...

  6. Ruby Lake National Wildlife Refuge Narrative report: January - April, 1949

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1949. The report begins by summarizing the weather...

  7. [Ruby Lake National Wildlife Refuge Narrative report: September - December, 1943

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1943. The report begins by...

  8. Ruby Lake National Wildlife Refuge Narrative report: January - April, 1954

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1954. The report begins by summarizing the weather...

  9. Ruby Lake National Wildlife Refuge Narrative report: January - April, 1962

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1962. The report begins by summarizing the weather...

  10. Ruby Lake National Wildlife Refuge : Narrative Report : FY - 1976

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1976 calendar year. The report begins with an introduction to...

  11. Narrative report Ruby Lake National Wildlife Refuge: October - December, 1944

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from October through December of 1944. The report begins by summarizing...

  12. Ruby Lake National Wildlife Refuge Narrative Report January -- April 1955

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1955. The report begins by summarizing the weather...

  13. Ruby Lake National Wildlife Refuge Narrative Report May - August, 1950

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1950. The report begins by summarizing the...

  14. Ruby Lake National Wildlife Refuge Narrative Report September - December, 1945

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake outlines Refuge accomplishments during the 1945 quarterly year. The report begins with a summary of the weather and water...

  15. Ruby Lake National Wildlife Service Annual Report Fiscal Year 1941

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake outlines Refuge accomplishments during the 1941 fiscal year. The report begins with a summary of the bird observations and...

  16. Ruby Lake National Wildlife Refuge Narrative Report September - December, 1963

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1963 quarterly year. The report begins by summarizing...

  17. Ruby Lake National Wildlife Refuge Narrative Report January -- April 1957

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1957. The report begins by summarizing the weather...

  18. Ruby Lake National Wildlife Refuge Narrative Report January - April 1956

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1956. The report begins by summarizing the weather...

  19. Narrative report Ruby Lake National Wildlife Refuge: September - December, 1945

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1945. The report begins by...

  20. Ruby Lake National Wildlife Refuge Narrative report: September - December, 1942

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1942. The report begins by...

  1. Ruby Lake National Wildlife Refuge Narrative Report May - August 1958

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1958. The report begins by summarizing the...

  2. Ruby Lake National Wildlife Refuge Narrative Report September - December 1964

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake outlines Refuge accomplishments during the 1964 quarterly year. The report begins with a summary of the weather and water...

  3. On Ruby's solid angle formula and some of its generalizations

    CERN Document Server

    Friot, Samuel

    2014-01-01

    Using the Mellin-Barnes representation, we show that Ruby's solid angle formula and some of its generalizations may be expressed in a compact way in terms of the Appell F4 and Lauricella Fc functions.

  4. Water Resource Inventory and Assessment: Ruby Lake National Wildlife Refuge

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This Water Resource Inventory and Assessment report for Ruby Lake National Wildlife Refuge describes current hydrologic information, provides an assessment of water...

  5. Ruby Lake National Wildlife Refuge Narrative Report September - December 1955

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1955. The report begins by...

  6. Ruby Lake National Wildlife Refuge Narrative Report September - December 1960

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1960 quarterly year. The report begins by summarizing...

  7. Ruby Lake National Wildlife Refuge Narrative report: 1970

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments for calendar year 1970. The report begins by summarizing the weather...

  8. Ruby Lake National Wildlife Refuge Narrative report: May - August, 1949

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1949. The report begins by summarizing the...

  9. Ruby Lake National Wildlife Refuge Narrative report: May - August, 1946

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1946. The report begins by summarizing the...

  10. Ruby Lake National Wildlife Refuge Narrative Report September -- December 1954

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1954. The report begins by...

  11. Ruby Lake National Wildlife Refuge Narrative report: September -- December, 1951

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from September through December of 1951. The report begins by...

  12. Ruby Lake National Wildlife Refuge Narrative Report May -- August 1954

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1954. The report begins by summarizing the...

  13. The Trail Inventory of Ruby Lake NWR [Cycle 2

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — The purpose of this report is to create a baseline inventory of all non-motorized trails on Ruby Lake National Wildlife Refuge. Trails in this inventory are eligible...

  14. Ruby Lake National Wildlife Refuge Narrative report: May - August, 1963

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1963. The report begins by summarizing the...

  15. Ruby Lake National Wildlife Refuge Narrative Report January - April 1958

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from January through April of 1958. The report begins by summarizing the weather...

  16. Ruby Lake National Wildlife Refuge Narrative report: May - August, 1948

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1948. The report begins by summarizing the...

  17. Ruby Lake National Wildlife Refuge Narrative report: May - August, 1951

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1951. The report begins by summarizing the...

  18. Ruby Lake National Wildlife Refuge Narrative report: May - August, 1962

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1962. The report begins by summarizing the...

  19. Ruby Lake National Wildlife Refuge : Narrative Report : FY - 1975

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1975 fiscal year. The report begins by summarizing the...

  20. Ruby Lake National Wildlife Refuge : Narrative Report : FY - 1974

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1974 fiscal year. The report begins by summarizing the...

  1. Ruby Lake National Wildlife Refuge : Narrative Report : 1972

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1972 calendar year. The report begins by summarizing...

  2. Ruby Lake National Wildlife Refuge Narrative Report May -- August 1955

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from May through August of 1955. The report begins by summarizing the...

  3. Ruby Lake National Wildlife Refuge Narrative report for 1967

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments for calendar year 1967. The report begins by summarizing the weather...

  4. Monitoring water masers in star-forming regions

    CERN Document Server

    Brand, J; Comoretto, G; Felli, M; Palagi, F; Palla, F; Valdettaro, R

    2004-01-01

    An overview is given of the analysis of more than a decade of H2O maser data from our monitoring program. We find the maser emission to generally depend on the luminosity of the YSO as well as on the geometry of the SFR. There appears to be a threshold luminosity of a few times 10**4 Lsol above and below which we find different maser characteristics.

  5. Portace knihovny Prawn z Ruby do Pythonu 3

    OpenAIRE

    Molhanec, Michal

    2017-01-01

    This work focuses on automatic translation of code written in Ruby programming language into Python 3. First part investigates principles of computer programming languages translation as is described in the literature. Second part compares elements of these two programming languages and suggests ways how these elements can be translated. Based on this theory I developed Ruby-to-Python translator. Its working is demonstrated on the translation of the Prawn library for generating PDF files.

  6. Functional metagenomic selection of RubisCOs from uncultivated bacteria

    Science.gov (United States)

    Varaljay, Vanessa A; Satagopan, Sriram; North, Justin A.; Witteveen, Briana; Dourado, Manuella N.; Anantharaman, Karthik; Arbing, Mark A.; McCann, Shelley; Oremland, Ronald S.; Banfield, Jillian F.; Wrighton, Kelly C.; Tabita, F. Robert

    2016-01-01

    Ribulose 1,5-bisphosphate carboxylase/oxygenase (RubisCO) is a critical yet severely inefficient enzyme that catalyses the fixation of virtually all of the carbon found on Earth. Here, we report a functional metagenomic selection that recovers physiologically active RubisCO molecules directly from uncultivated and largely unknown members of natural microbial communities. Selection is based on CO2-dependent growth in a host strain capable of expressing environmental deoxyribonucleic acid (DNA), precluding the need for pure cultures or screening of recombinant clones for enzymatic activity. Seventeen functional RubisCO-encoded sequences were selected using DNA extracted from soil and river autotrophic enrichments, a photosynthetic biofilm and a subsurface groundwater aquifer. Notably, three related form II RubisCOs were recovered which share high sequence similarity with metagenomic scaffolds from uncultivated members of theGallionellaceae family. One of the Gallionellaceae RubisCOs was purified and shown to possessCO2/O2 specificity typical of form II enzymes. X-ray crystallography determined that this enzyme is a hexamer, only the second form II multimer ever solved and the first RubisCO structure obtained from an uncultivated bacterium. Functional metagenomic selection leverages natural biological diversity and billions of years of evolution inherent in environmental communities, providing a new window into the discovery of CO2-fixing enzymes not previously characterized.

  7. New Maser Emission from Nonmetastable Ammonia in NGC 7538

    CERN Document Server

    Hoffman, Ian M

    2011-01-01

    We present the first interferometric observations at 18.5 GHz of IRS 1 in NGC 7538. These observations include images of the nonmetastable ^{14}NH_3 (9,6) masers with a synthesized beam of 2 arcseconds and images of the continuum emission with a synthesized beam of 150 milliarcseconds. Of the maser emission, the previously known feature near v_LSR = -60 km/s is spectrally resolved into at least two components and we observe several new maser emission features near v_LSR = -57 km/s. The new maser emission near -57 km/s lies 250 +/- 90 milliarcseconds northwest of the maser emission near -60 km/s. All of the masers are angularly unresolved indicating brightness temperatures T_B > 2000 K. We are also able to conclusively associate the ammonia masers with the position of IRS 1. The excitation of these rare ammonia masers is discussed in the context of the rich maser environment of IRS 1.

  8. Survey of Outer Galaxy Molecular Lines Associated with Water Masers

    Science.gov (United States)

    Mochizuki, N.; Hachisuka, K.; Umemoto, T.

    2009-08-01

    H_2O masers in Young stellar objects (YSOs) in our Galaxy are one of the targets of the VSOP-2 science. The advantage of VSOP-2 observation is the highest angular resolution which can detect a proper motion of H_2O masers for distant objects over short time intervals. To find candidate sources, we observed H2O maser sources in the outer Galaxy using the VLA, and we surveyed the molecular lines toward these sources to understand the environment of YSOs. Higher H2 column densities of YSOs were found for objects with active H2O masers.

  9. Pumping Mechanisms for SiO Masers around VX Sgr

    Indian Academy of Sciences (India)

    J. B. Su; Z.-Q. Shen; X. Chen; Jiyune Yi; D. R. Jiang; Y. J. Yun

    2011-03-01

    VX Sgr, a semi-regular variable, is a red giant star with intense SiO maser emission at 43 GHz. The pumping mechanism of the circumstellar SiO masers has been controversial for decades since its discovery. In order to pursue this long-standing problem further, we have carried out simultaneous VLBA observations of two 7 mm SiO masers at five epochs in about two years. We present relatively aligned = 1 and = 2, = 1-0 SiO maser maps and discuss the dominant pumping mechanism, which may be epoch dependent or a combination of both mechanisms.

  10. Pumping Mechanisms for SiO Masers around VX Sgr

    Science.gov (United States)

    Su, J. B.; Shen, Z.-Q.; Chen, X.; Yi, Jiyune; Jiang, D. R.; Yun, Y. J.

    2011-06-01

    VX Sgr, a semi-regular variable, is a red giant star with intense SiO maser emission at 43 GHz. The pumping mechanism of the circumstellar SiO masers has been controversial for decades since its discovery. In order to pursue this long-standing problem further, we have carried out simultaneous VLBA observations of two 7 mm SiO masers at five epochs in about two years. We present relatively aligned υ = 1 and υ = 2, J = 1-0 SiO maser maps and discuss the dominant pumping mechanism, which may be epoch dependent or a combination of both mechanisms.

  11. 1990 Annual water management report 1991 Annual water management plan : Ruby Lake National Wildlife Refuge : Ruby Valley Nevada

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Ruby Lake NWR 1990 Annual Water Management Report 1991 Annual Water Management Plan. Includes 1990 weather summary, water availability forecast, summary of 1990...

  12. Ruby Lake National Wildlife Refuge : Ruby Valley Nevada : 1993 Annual water management report 1994 Annual water management plan

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Although the winter of 1992/93 brought above average snow pack water content to the Ruby Mountains and above average precipitation, the surface water elevations of...

  13. Ruby Lake National Wildlife Refuge : Ruby Valley Nevada : 1992 Annual water management report 1993 Annual water management plan

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Ruby Lake NWR 1992 Annual Water Management Report 1993 Annual Water Management Plan. Includes summary of 1992 weather, 1992 water levels, water availability forecast...

  14. 1989 Annual water management report 1990 Annual water management plan : Ruby Lake National Wildlife Refuge : Ruby Valley Nevada

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Ruby Lake NWR 1989 Annual Water Management Report 1990 Annual Water Management Plan. Includes 1989 weather summary, water availability forecast, summary of 1989...

  15. Synchrotron masers and fast radio bursts

    CERN Document Server

    Ghisellini, Gabriele

    2016-01-01

    Fast Radio Bursts (FRBs), with a typical duration of 1 ms and 1 Jy flux density at GHz frequencies, have brightness temperatures exceeding 1e33 K, requiring a coherent emission process. This can be achieved by bunching particles in volumes smaller than the typical wavelength, but this may be challenging. Alternatively, we can have maser emission. Under certain conditions, the synchrotron stimulated emission process can be more important than true absorption, and a synchrotron maser can be created. This occurs when the emitting electrons have a very narrow distribution of pitch angles and energies. This process overcomes the difficulties of having extremely dense bunches of particles and relaxes the light crossing time limits, since there is no simple relation between the actual size of the source and the observed variability timescale.

  16. Maser Astrometry with VERA and VSOP-2

    Science.gov (United States)

    Honma, M.; Bushimata, T.; Choi, Y. K.; Hirota, T.; Imai, H.; Iwadate, K.; Jike, T.; Kameno, S.; Kameya, O.; Kamohara, R.; Kawaguchi, N.; Kijima, M.; Kim, M.; Kobayashi, H.; Kuji, S.; Kurayama, T.; Manabe, S.; Matsui, M.; Matsumoto, N.; Miyaji, T.; Nagayama, T.; Nakagawa, A.; Nakamura, K.; Oh, C. S.; Omodaka, T.; Oyama, T.; Sakai, S.; Sato, K.; Sato, M.; Sasao, T.; Shibata, K. M.; Tamura, Y.; Yamashita, K.

    2009-08-01

    We present recent results of maser astrometry obtained with VERA (VLBI Exploration of Radio Astrometry), which is a Japanese VLBI array dedicated to phase-referencing astrometry to explore the 3-D structure of the Milky Way Galaxy. Since 2004 we have been conducting regular monitoring of maser sources with VERA, and we have already detected parallaxes for several sources, ranging from a few 100 pc to 5 kpc. These results include measurements for Galactic star-forming regions such as ORI-KL, S269, NGC 281 as well as those for late type stars such as VY CMa. We also discuss the VERA---VSOP-2 connection in the near future, and propose astrometric observations with VSOP-2.

  17. Synchrotron masers and fast radio bursts

    Science.gov (United States)

    Ghisellini, G.

    2017-02-01

    Fast radio bursts, with a typical duration of 1 ms and 1 Jy flux density at gigahertz frequencies, have brightness temperatures exceeding 1033 K, requiring a coherent emission process. This can be achieved by bunching particles in volumes smaller than the typical wavelength, but this may be challenging. Maser emission is a possibility. Under certain conditions, the synchrotron-stimulated emission process can be more important than true absorption, and a synchrotron maser can be created. This occurs when the emitting electrons have a very narrow distribution of pitch angles and energies. This process overcomes the difficulties of having extremely dense bunches of particles and relaxes the light-crossing time limits, since there is no simple relation between the actual size of the source and the observed variability time-scale.

  18. Improved VLBI astrometry of OH maser stars

    CERN Document Server

    Vlemmings, W H T

    2007-01-01

    Aims: Accurate distances to evolved stars with high mass loss rates are needed for studies of many of their fundamental properties. However, as these stars are heavily obscured and variable, optical and infrared astrometry is unable to provide enough accuracy. Methods: Astrometry using masers in the circumstellar envelopes can be used to overcome this problem. We have observed the OH masers of a number of Asymptotic Giant Branch (AGB) stars for approximately 1 year with the Very Long Baseline Array (VLBA). We have used the technique of phase referencing with in-beam calibrators to test the improvements this technique can provide to Very Long Baseline Interferometry (VLBI) OH maser astrometric observations. Results: We have significantly improved the parallax and proper motion measurements of the Mira variable stars U Her, S CrB and RR Aql. Conclusions: It is shown that both in-beam phase-referencing and a decrease in solar activity during the observations significantly improves the accuracy of the astrometric...

  19. Water Masers in AGN Accretion Disks

    Science.gov (United States)

    Braatz, J. A.; Reid, M. J.; Greenhill, L. J.; Kuo, C.-Y.; Condon, J. J.; Lo, K.-Y.; Henkel, C.

    2009-08-01

    Water vapor masers at 22 GHz have been detected in over 100 galaxies, most of them AGNs. High resolution VLBI observations of these masers provide the only opportunity for direct imaging of sub-parsec structure in AGN accretion disks. The key science goals associated with such observations are concentrated in two areas. First, observations of nearby, bright sources, exemplified by NGC 4258, enable unique investigations of accretion disk geometry, substructure, thickness, and rotation properties. Second, when combined with spectral line monitoring, VLBI imaging and subsequent disk modeling enables the estimation of a distance to the host galaxy independent of standard candle arguments. In this contribution we present VLBI observations of two maser disk systems in galaxies well into the Hubble flow, UGC 3789 and NGC 6323. A long term goal in these studies is to measure the Hubble constant with high precision and, as a complement to CMB observations, constrain several key cosmological parameters, including the equation of state for dark energy. Observations with VSOP-2 at 22 GHz will have the resolution critical for mapping substructure in these accretion disks and will contribute to reducing systematic errors in the measurement of distances to galaxies.

  20. Insights into high mass star formation from methanol maser observations

    Science.gov (United States)

    Farmer, Hontas Freeman

    2013-06-01

    We present high angular resolution data on Class I and Class II methanol masers, together with other tracers of star formation like H2O masers, ultracompact (UC) ionized hydrogen (H II) regions, and 4.5 um infrared sources, taken from the literature. The aim is to study what these data tell us about the process of high mass star formation; in particular, whether disk-outflow systems are compatible with the morphology exhibited by Class I and Class II methanol masers. Stars form in the dense cores inside molecular clouds, and while the process of the formation of stars like our Sun is reasonably well understood, details of the formation of stars with masses eight times that of our Sun or greater, the so-called high mass stars, remain a mystery. Being compact and bright sources, masers provide an excellent way to observe high mass star forming regions. In particular, Class II methanol masers are found exclusively in high mass star forming regions. Based on the positions of the Class I and II methanol and H2O masers, UCHII regions and 4.5 um infrared sources, and the center velocities (vLSR) of the Class I methanol and H2O masers, compared to the vLSR of the Class II methanol masers, we propose three disk-outflow models that may be traced by methanol masers. In all three models, we have located the Class II methanol maser near the protostar, and the Class I methanol maser in the outflow, as is known from observations during the last twenty years. In our first model, the H2O masers trace the linear extent of the outflow. In our second model, the H2O masers are located in a circumstellar disk. In our third model, the H2O masers are located in one or more outflows near the terminating shock where the outflow impacts the ambient interstellar medium. Together, these models reiterate the utility of coordinated high angular resolution observations of high mass star forming regions in maser lines and associated star formation tracers.

  1. Investigation of two-frequency Paul traps for antihydrogen production

    Energy Technology Data Exchange (ETDEWEB)

    Leefer, Nathan; Krimmel, Kai, E-mail: kkrimmel@students.uni-mainz.de [Helmholtz-Institut Mainz (Germany); Bertsche, William [University of Manchester (United Kingdom); Budker, Dmitry [Helmholtz-Institut Mainz (Germany); Fajans, Joel [University of California at Berkeley, Department of Physics (United States); Folman, Ron [Ben-Gurion University of the Negev, Department of Physics (Israel); Häffner, Hartmut [University of California at Berkeley, Department of Physics (United States); Schmidt-Kaler, Ferdinand [Helmholtz-Institut Mainz (Germany)

    2017-11-15

    Radio-frequency (rf) Paul traps operated with multifrequency rf trapping potentials provide the ability to independently confine charged particle species with widely different charge-to-mass ratios. In particular, these traps may find use in the field of antihydrogen recombination, allowing antiproton and positron clouds to be trapped and confined in the same volume without the use of large superconducting magnets. We explore the stability regions of two-frequency Paul traps and perform numerical simulations of small samples of multispecies charged-particle mixtures of up to twelve particles that indicate the promise of these traps for antihydrogen recombination.

  2. Vanadium-rich ruby and sapphire within Mogok Gemfield, Myanmar: implications for gem color and genesis

    Science.gov (United States)

    Zaw, Khin; Sutherland, Lin; Yui, Tzen-Fu; Meffre, Sebastien; Thu, Kyaw

    2015-01-01

    Rubies and sapphires are of both scientific and commercial interest. These gemstones are corundum colored by transition elements within the alumina crystal lattice: Cr3+ yields red in ruby and Fe2+, Fe3+, and Ti4+ ionic interactions color sapphires. A minor ion, V3+ induces slate to purple colors and color change in some sapphires, but its role in coloring rubies remains enigmatic. Trace element and oxygen isotope composition provide genetic signatures for natural corundum and assist geographic typing. Here, we show that V can dominate chromophore contents in Mogok ruby suites. This raises implications for their color quality, enhancement treatments, geographic origin, exploration and exploitation and their comparison with rubies elsewhere. Precise LA-ICP-MS analysis of ruby and sapphire from Mogok placer and in situ deposits reveal that V can exceed 5,000 ppm, giving V/Cr, V/Fe and V/Ti ratios up to 26, 78, and 97 respectively. Such values significantly exceed those found elsewhere suggesting a localized geological control on V-rich ruby distribution. Our results demonstrate that detailed geochemical studies of ruby suites reveal that V is a potential ruby tracer, encourage comparisons of V/Cr-variation between ruby suites and widen the scope for geographic typing and genesis of ruby. This will allow more precise comparison of Asian and other ruby fields and assist confirmation of Mogok sources for rubies in historical and contemporary gems and jewelry.

  3. Case study : project in Ruby, Alaska

    Energy Technology Data Exchange (ETDEWEB)

    NONE

    2008-07-01

    This paper described a 5 kW hydrokinetic turbine installed within a micro-grid electricity system in Ruby, Alaska. Designed by Calgary-based New Energy Corporation, the system was installed to help the remote community utilize its river resources and lower its energy costs. Located on the Yukon River, electricity generation for the community was provided by diesel generators at a cost of approximately $0.98 per kWh. The turbine system was developed as a complete water-to-wire unit. Anchor points were installed on a rock face on the riverbank as well as directly on the river bottom. Chains were place from each of the anchor points to a buoy located in the center a deflector boom placed in front of the boat to deflect floating debris. The turbine was installed using a pontoon boat with an aluminum frame and a cradle system designed to transfer the torque generated by the turbine onto the pontoon boat. A grid-tie inverter was installed and interconnected to the local micro-grid. Output from the generator was then tied into a junction box on the pontoon boat. Electrical underwater cables were then attached to the junction box on the boat. The turbine was then rotated into the water in order to generate electricity. It was concluded that the system is now being monitored for its performance as well as its impact on the surrounding environment. 5 figs.

  4. The Eddington Ratio of H2O Maser Host AGN

    Indian Academy of Sciences (India)

    Q. Guo; J. S. Zhang; J. Wang

    2011-03-01

    The Eddington ratio was derived for the entire maser host AGN sample, based on the intrinsic X-ray luminosity, the X-ray bolometric correction X and the mass of central black hole. Further the [O III] bolometric correction [O III] was estimated for our sample. Possible relations were also investigated between the maser luminosity and the bolometric luminosity – the Eddington ratio.

  5. Statistical Properties of 6.7 GHz Methanol Maser Sources

    Institute of Scientific and Technical Information of China (English)

    2003-01-01

    We present a statistical analysis of 482 6.7 GHz methanol maser sourcesfrom the available literature, on their maser emission and the characteristics oftheir associated infrared sources. On the color-color diagram, more than 70% ofthe objects fall within a very small region (0.57 ≤ [25 - 12] ≤ 1.30 and 1.30 ≤[60 - 12] ≤ 2.50). This suggests that 6.7 GHz methanol maser emission occurs onlywithin a very short evolutionary phase during the earliest stage of star formation.The velocity ranges of the masers belong to two main groups: one from 1 to 10km s-1, and one from about 11 to 20 km s-1. These velocity ranges indicate thatthe masers are probably associated with both disks and outflows. The correlationsbetween the maser and infrared flux densities, and between the maser and infraredluminosities, suggest that far-infrared radiation is a possible pumping mechanismfor the masers which most probably originate from some outer molecular envelopesor disks.

  6. Physical characteristics of bright Class I methanol masers

    CERN Document Server

    Leurini, S; Walmsley, C M

    2016-01-01

    Class I CH$_3$OH masers trace interstellar shocks. They have received little attention mostly as a consequence of their low luminosities; this situation has changed recently and Class I masers are now routinely used as signposts of outflows. The recent detection of polarisation in Class I lines now makes it possible to obtain information on magnetic fields in shocks. We make use of newly calculated collisional rates to investigate the excitation of Class I masers and to reconcile their observed properties with model results. We performed LVG calculations with a plane-parallel slab geometry to compute the pump and loss rates which regulate the interactions of the different maser systems with the maser reservoir. We study the dependence of the pump rate, the loss rate, and the inversion efficiency of the pumping scheme of Class I masers on the physics of the gas. Bright Class I masers are mainly high-temperature high-density structures with maser emission measures corresponding to high CH$_3$OH abundances close...

  7. Marble-hosted ruby deposits of the Morogoro Region, Tanzania

    Science.gov (United States)

    Balmer, Walter A.; Hauzenberger, Christoph A.; Fritz, Harald; Sutthirat, Chakkaphan

    2017-10-01

    The ruby deposits of the Uluguru and Mahenge Mts, Morogoro Region, are related to marbles which represent the cover sequence of the Eastern Granulites in Tanzania. In both localities the cover sequences define a tectonic unit which is present as a nappe structure thrusted onto the gneissic basement in a north-western direction. Based on structural geological observations the ruby deposits are bound to mica-rich boudins in fold hinges where fluids interacted with the marble-host rock in zones of higher permeability. Petrographic observations revealed that the Uluguru Mts deposits occur within calcite-dominated marbles whereas deposits in the Mahenge Mts are found in dolomite-dominated marbles. The mineral assemblage describing the marble-hosted ruby deposit in the Uluguru Mts is characterised by corundum-dolomite-phlogopite ± spinel, calcite, pargasite, scapolite, plagioclase, margarite, chlorite, tourmaline whereas the assemblage corundum-calcite-plagioclase-phlogopite ± dolomite, pargasite, sapphirine, titanite, tourmaline is present in samples from the Mahenge Mts. Although slightly different in mineral assemblage it was possible to draw a similar ruby formation history for both localities. Two ruby forming events were distinguished by textural differences, which could also be modeled by thermodynamic T-XCO2 calculations using non-ideal mixing models of essential minerals. A first formation of ruby appears to have taken place during the prograde path (M1) either by the breakdown of diaspore which was present in the original sedimentary precursor rock or by the breakdown of margarite to corundum and plagioclase. The conditions for M1 metamorphism was estimated at ∼750 °C at 10 kbar, which represents granulite facies conditions. A change in fluid composition towards a CO2 dominated fluid triggered a second ruby generation to form. Subsequently, the examined units underwent a late greenschist facies overprint. In the framework of the East African Orogen we

  8. Ion beam analysis of rubies and their simulants

    Energy Technology Data Exchange (ETDEWEB)

    Juncomma, U. [Plasma and Beam Physics Research Facility, Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50202 (Thailand); Intarasiri, S., E-mail: saweat@gmail.com [Science and Technology Research Institute, Chiang Mai University, Chiang Mai 50202 (Thailand); Thailand Center of Excellence in Physics, Commission on Higher Education, 328 Si Ayutthaya Road, Bangkok 10400 (Thailand); Bootkul, D. [Department of General Science (Gems and Jewelry), Faculty of Science, Srinakharinwirot University, Bangkok 10110 (Thailand); Thailand Center of Excellence in Physics, Commission on Higher Education, 328 Si Ayutthaya Road, Bangkok 10400 (Thailand); Tippawan, U., E-mail: beary1001@gmail.com [Plasma and Beam Physics Research Facility, Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai 50202 (Thailand); Thailand Center of Excellence in Physics, Commission on Higher Education, 328 Si Ayutthaya Road, Bangkok 10400 (Thailand)

    2014-07-15

    Ion beam analysis (IBA) is a set of well known powerful analytical techniques which use energetic particle beam as a probe. Among them, two techniques are suitable for gemological analysis, i.e., Particle Induced X-rays Emission (PIXE) and Ionoluminescence (IL). We combine these two techniques for the investigations of rubies and their simulants. The main objective is to find a reference fingerprint of these gemstones. The data are collected from several natural rubies, synthetic rubies, red spinels, almandine garnets and rubellite which very much resemble and are difficult to distinguish with the gemologist loupe. From our measurements, due to their different crystal structures and compositions, can be clearly distinguished by the IL and PIXE techniques. The results show that the PIXE spectra consist of a few dominant lines of the host matrix elements of each gemstone and some weaker lines due to trace elements of transition metals. PIXE can easily differentiate rubies from other stones by evaluating their chemical compositions. It is noticed that synthetic rubies generally contain fewer impurities, lower iron and higher chromium than the natural ones. Moreover, the IL spectrum of ruby is unique and different from those of others stones. The typical spectrum of ruby is centered at 694 nm, with small sidebands that can be ascribed to a Cr{sup 3+} emission spectrum which is dominated by an R-line at the extreme red end of the visible part of the electromagnetic spectrum. Although the spectrum of synthetic ruby is centered at the same wavelength, the peak is stronger due to higher concentration of Cr and lower concentration of Fe than for natural rubies. For spinel, the IL spectrum shows strong deformation where the R-line is split due to the presence of MgO. For rubellite, the peak center is shifted to 692 nm which might be caused by the replacement of Mn{sup 3+} at the Al{sup 3+} site of the host structure. It is noticed that almandine garnet is not luminescent due

  9. Metals and trace elements in pondweed and aquatic invertebrates at Ruby Lake National Wildlife Refuge

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — The Nevada Division of Wildlife operates the Gallagher Fish Hatchery in the Ruby Lake NWR in Ruby Valley, Nevada. The results of previous sampling of water, sediment...

  10. Nuclear microscopy of rubies: Trace elements and inclusions

    Science.gov (United States)

    Osipowicz, T.; Tay, T. S.; Orlic, I.; Tang, S. M.; Watt, F.

    1995-09-01

    The concentrations of trace elements (e.g. Ti, V, Cr, Fe and Cu) in ornamental rubies have been linked to the country of origin for natural stones [1,2]. These broad-beam PIXE results show relatively large variations between stones from one country, which might indicate that they stem from different geological environments in a country, or that there are inclusions or surface contaminations present in individual stones. PIXE elemental maps were used to find contamination and inclusion free regions on rubies from Mong Hsu, Burma, and from Thailand. Trace element concentrations were determined in these surface areas. The results indicate that the Fe-concentrations in Mong Hsu rubies have previously been overestimated due to the presence of surface contaminations. Cu is consistently present at a few hundred ppm level in these stones and not observed in any of the four Thai rubies, while it was observed sporadically in broad-beam measurements. The depth profiling capabilities of the proton microprobe were employed for the analysis of liquid and mineral inclusions in rubies, and some preliminary results are reported.

  11. Detection of water masers in a sample of 84 IRAS sources

    Institute of Scientific and Technical Information of China (English)

    WU YueFang; ESIMBEK Jarken; WANG JunZhi; LIU Xiang; QIN ShengLi; ZHANG Jin

    2007-01-01

    Using a newly installed system on the 25 m telescope of Urumqi Observatory, we searched for H2O maser emission towards 84 IRAS sources including young stellar objects (YSOs) and candidates for OH/IR stars. Water masers were detected in four star formation regions and one envelope of late type of stars for the first time. New water maser components were measured in two sources. In a maser source with no water maser emission detected six years ago, strong maser emission was found at different velocities, showing that there was a new explosion of water maser in this source.

  12. High-Velocity H2O Masers Associated Massive Star Formation Regions

    Institute of Scientific and Technical Information of China (English)

    徐烨; 蒋栋荣; 郑兴武; 顾敏峰; 俞志尧; 裴春传

    2001-01-01

    We report on the results of 12 CO (1-0) emission associated with H2O masers and massive star formation regions to identify high-velocity H2O masers. Several masers have a large blueshift, even up to 120 km.s-1, with respect to the CO peak, but no large redshifted maser appears. This result suggests that high-velocity H2O masers can most probably occur in high mass star-forming regions and quite a number of masers stem from the amplifications of a background source, which may enable those undetectable weak masers to come to an observable level.

  13. Water Masers in the Andromeda Galaxy: I. A Survey for Water Masers, Ammonia, and Hydrogen Recombination Lines

    CERN Document Server

    Darling, Jeremy; Amiri, Nikta; Lawrence, Kelsey

    2016-01-01

    We report the results of a Green Bank Telescope survey for water masers, ammonia (1,1) and (2,2), and the H66-alpha recombination line toward 506 luminous compact 24 micron-emitting regions in the Andromeda Galaxy (M31). We include the 206 sources observed in the Darling (2011) water maser survey for completeness. The survey was sensitive enough to detect any maser useful for ~10 microarcsecond/yr astrometry. No new water masers, ammonia lines, or H66-alpha recombination lines were detected individually or in spectral stacks reaching rms noise levels of ~3 mJy and ~0.2 mJy, respectively, in 3.1-3.3 km/s channels. The lack of detections in individual spectra and in the spectral stacks is consistent with Galactic extrapolations. Contrary to previous assertions, there do not seem to be additional bright water masers to be found in M31. The strong variability of water masers may enable new maser detections in the future, but variability may also limit the astrometric utility of known (or future) masers since flar...

  14. Microbunching of relativistic electrons using a two-frequency laser

    Science.gov (United States)

    Gordon, D.; Clayton, C. E.; Katsouleas, T.; Mori, W. B.; Joshi, C.

    1998-01-01

    A high power two-frequency laser can be used to modulate the axial momentum of a copropagating relativistic electron beam. The net work done on each electron is accounted for almost entirely by the axial electric field of the laser even when approaching the one-dimensional limit. After interacting with the laser, the electron beam can be bunched either by a long drift space or a dispersive optic. We give an example in which a 2.5-TW CO2 laser and a chicane compressor are used to transform a constant stream of 16-MeV electrons into a train of 60-fs microbunches, each containing 10 pC of charge.

  15. Extragalactic Water Maser Observations with VSOP-2

    Science.gov (United States)

    Hagiwara, Y.; VSOP-2 Science Working Group

    2009-08-01

    Space-VLBI is known to achieve greatly increased angular resolution compared with ground-based VLBI observations. VSOP-2 will offer 75 μarcsec angular resolution at 22 GHz. With this improved angular resolution, VSOP-2 observations of H_2O megamaser will refine the measurements of proper motions, accelerations, distances to galaxies, and other physical parameters of galactic nuclei. In this presentation, the prospects of VSOP-2 observations of extragalactic H_2O maser with strong emphasis on H_2O megamaser are presented.

  16. The layer by layer selective laser synthesis of ruby

    Directory of Open Access Journals (Sweden)

    Vlasova M.

    2010-01-01

    Full Text Available In the work, features of the layer-by-layer selective laser synthesis (SLS of ruby from an Al2O3-Cr2O3 mixture are considered depending on the irradiation power, the laser beam traverse speed, the height and amount of the backfill of powder layers. It has been established that, under irradiation, a track consisting of polycrystalline textured ruby forms. The morphology of the surface of the track and its crystalline structure are determined by the irradiation conditions.

  17. An introduction to scripting in Ruby for biologists

    Directory of Open Access Journals (Sweden)

    Law Andy

    2009-07-01

    Full Text Available Abstract The Ruby programming language has a lot to offer to any scientist with electronic data to process. Not only is the initial learning curve very shallow, but its reflection and meta-programming capabilities allow for the rapid creation of relatively complex applications while still keeping the code short and readable. This paper provides a gentle introduction to this scripting language for researchers without formal informatics training such as many wet-lab scientists. We hope this will provide such researchers an idea of how powerful a tool Ruby can be for their data management tasks and encourage them to learn more about it.

  18. Research on the Steering Strategy for Hydrogen Maser

    Science.gov (United States)

    Yin, D. S.; Zhao, S. H.; Gao, Y. P.

    2016-07-01

    In the master clock system, the local standard time UTC(k) with a better short-term stability will be generated, if the hydrogen maser is set as a frequency source of the master clock. But the hydrogen maser always exhibits an apparent frequency drift, thus its long-term stability gets poor with time, therefore the stability and accuracy of UTC(k) become worse. To solve this problem, we compare the performance of hydrogen maser with cesium clocks, and modify the time scale algorithm when the hydrogen maser is involved, we also propose a new steering strategy when hydrogen maser is used as the frequency source of master clock. We set up an experiment system and write programs, and finally the new steering strategy is testified with the laboratory data. Results show that when the hydrogen maser is involved in the atomic time scale calculation, the short-term frequency stability of reference time scale will be improved. Meanwhile, the local time UTC(k) has a better short-term frequency stability when the frequency source of the master clock uses hydrogen maser instead of cesium clock.

  19. The environment of the strongest galactic methanol maser

    CERN Document Server

    Sanna, A; Carrasco-Gonzalez, C; Reid, M J; Ellingsen, S P; Brunthaler, A; Moscadelli, L; Cesaroni, R; Krishnan, V

    2015-01-01

    The high-mass star-forming site G009.62-00.20E hosts the 6.7 GHz methanol maser source with the greatest flux density in the Galaxy which has been flaring periodically over the last ten years. We performed high-resolution astrometric measurements of the CH3OH, H2O, and OH maser emission and 7 mm continuum in the region. The radio continuum emission was resolved in two sources separated by 1300 AU. The CH3OH maser cloudlets are distributed along two north-south ridges of emission to the east and west of the strongest radio continuum component. This component likely pinpoints a massive young stellar object which heats up its dusty envelope, providing a constant IR pumping for the Class II CH3OH maser transitions. We suggest that the periodic maser activity may be accounted for by an independent, pulsating, IR radiation field provided by a bloated protostar in the vicinity of the brightest masers. We also report about the discovery of an elliptical distribution of CH3OH maser emission in the region of periodic v...

  20. THE ENVIRONMENT OF THE STRONGEST GALACTIC METHANOL MASER

    Energy Technology Data Exchange (ETDEWEB)

    Sanna, A.; Menten, K. M.; Carrasco-González, C.; Brunthaler, A. [Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn (Germany); Reid, M. J. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Ellingsen, S. P.; Krishnan, V. [School of Mathematics and Physics, University of Tasmania, Private Bag 37, Hobart, Tasmania 7001 (Australia); Moscadelli, L.; Cesaroni, R., E-mail: asanna@mpifr-bonn.mpg.de [INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze (Italy)

    2015-05-01

    The high-mass star-forming site G009.62+00.20 E hosts the 6.7 GHz methanol maser source with the greatest flux density in the Galaxy which has been flaring periodically over the last 10 yr. We performed high-resolution astrometric measurements of the CH{sub 3}OH, H{sub 2}O, and OH maser emission and 7 mm continuum in the region. The radio continuum emission was resolved in two sources separated by 1300 AU. The CH{sub 3}OH maser cloudlets are distributed along two north–south ridges of emission to the east and west of the strongest radio continuum component. This component likely pinpoints a massive young stellar object which heats up its dusty envelope, providing a constant IR pumping for the Class II CH{sub 3}OH maser transitions. We suggest that the periodic maser activity may be accounted for by an independent, pulsating, IR radiation field provided by a bloated protostar in the vicinity of the brightest masers. We also report the discovery of an elliptical distribution of CH{sub 3}OH maser emission in the region of periodic variability.

  1. Discovery of two new methanol masers in NGC 7538

    CERN Document Server

    Pestalozzi, M; Minier, V; Motte, F

    2006-01-01

    Context: NGC7538 is known to host a 6.7 and 12.2GHz methanol maser cospatial with a Ultra Compact (UC) HII region, IRS1. Aims: We report on the serendipitous discovery of two additional 6.7GHz methanol masers in the same region, not associated with IRS1. Methods: Interferometry maser positions are compared with recent single-dish and interferometry continuum observations. Results: The positions of the masers agree to high accuracy with the 1.2mm continuum peak emission in NGC7538 IRS9 and NGC7538 S. This clear association is also confirmed by the positional agreement of the masers with existing high resolution continuum observations at cm and/or mm wavelengths. Conclusions: Making use of the established strong relation between methanol masers and high-mass star formation, we claim that we have accurately positioned the high-mass protostars within the regions where they are detected. The variety of objects hosting a 6.7GHz methanol maser in NGC7538 shows that this emission probably traces different evolutionar...

  2. 19 CFR 12.151 - Prohibitions and conditions on importations of jadeite, rubies, and articles of jewelry...

    Science.gov (United States)

    2010-04-01

    ... are prohibited from importation into the United States (see 31 CFR part 537): (1) Jadeite mined or... jadeite, rubies, and articles of jewelry containing jadeite or rubies. 12.151 Section 12.151 Customs... conditions on importations of jadeite, rubies, and articles of jewelry containing jadeite or rubies....

  3. NG7538 IRS1 N: modeling a circumstellar maser disk

    CERN Document Server

    Pestalozzi, M R; Conway, J; Booth, R

    2004-01-01

    We present an edge-on Keplerian disk model to explain the main component of the 12.2 and 6.7 GHz methanol maser emission detected toward NGC7538-IRS1 N. The brightness distribution and spectrum of the line of bright masers are successfully modeled with high amplification of background radio continuum emission along velocity coherent paths through a maser disk. The bend seen in the position-velocity diagram is a characteristic signature of differentially rotating disks. For a central mass of 30 solar masses, suggested by other observations, our model fixes the masing disk to have inner and outer radii of about 270 AU and 750 AU.

  4. First SIMBA observations toward CH3OH masers

    CERN Document Server

    Pestalozzi, M R; Booth, R S

    2002-01-01

    We report SIMBA 1.2 mm dust continuum observations of the environments of eight methanol maser sources, all discovered during spatially fully-sampled, untargeted surveys of the galactic plane. We summarise our search for possible associations of the masers with IR sources (IRAS and MSX) and find that it is not always possible to make definite associations. A preliminary characterisation of the IR sources found in the maser neighbourhood is given according their position in the [60-25] -- [25-12] colour-colour diagram.

  5. Detection of water masers toward young stellar objects in the Large Magellanic Cloud

    Energy Technology Data Exchange (ETDEWEB)

    Johanson, A. K.; Migenes, V. [Department of Physics and Astronomy, Brigham Young University, N283 ESC, Provo, UT 84602 (United States); Breen, S. L., E-mail: ajohanson@byu.edu [CSIRO Astronomy and Space Science, Australia Telescope National Facility, P.O. Box 76, Epping NSW 1710 (Australia)

    2014-02-01

    We present results from a search for water maser emission toward N4A, N190, and N206, three regions of massive star formation in the Large Magellanic Cloud (LMC). Four water masers were detected; two toward N4A, and two toward N190. In the latter region, no previously known maser emission has been reported. Future studies of maser proper motion to determine the galactic dynamics of the LMC will benefit from the independent data points the new masers in N190 provide. Two of these masers are associated with previously identified massive young stellar objects (YSOs), which strongly supports the authenticity of the classification. We argue that the other two masers identify previously unknown YSOs. No masers were detected toward N206, but it does host a newly discovered 22 GHz continuum source, also associated with a massive YSO. We suggest that future surveys for water maser emission in the LMC be targeted toward the more luminous, massive YSOs.

  6. [Studies on the chemical constituents from Fructus Rubi].

    Science.gov (United States)

    Xie, Yihui; Miao, Juru; Liu, Wenqin

    2005-02-01

    Five compounds have been isolated from Fructus Rubi. On the basis of spectral analysis and physicochemical properties, their structures were establised as 4-hydroxy-3-methoxybenzoic acid (I), p-hydroxybenzoic acid (II), gallic acid (III), tiliroside (IV) and ellagic acid (V). I, II and III were found from the plant for the first time.

  7. Ruby On Rails和Struts+Hibernate的比较

    Institute of Scientific and Technical Information of China (English)

    Fikko

    2005-01-01

    Ruby On Rails是目前刚刚兴起的一个用于web程序快速开发的开源框架。Ruby On Rails建立在Ruby语言的基础上,提供了完整的web程序开发的组件。说它快速并不过分,它的开发速度可以比传统的比如基于Struts和Hibernate的框架快十倍以上,而且开发程序的代码要短小很多。目前Ruby On Rails已经得到了开发者群体包括J2EE在内的广泛关注.而且在其他语言的基础上也纷纷出现类似的框架。在此我们对Ruby On Rails和传统的Struts+Hibernate进行构架上的粗浅比较。

  8. Ruby coloured lead glasses by generation of silver nanoparticles

    Energy Technology Data Exchange (ETDEWEB)

    Gil, C. [Fundacion Centro Nacional del Vidrio, Pocillo, 1, 40100 La Granja de San Ildefonso (Segovia) (Spain); Villegas, M.A. [Centro Nacional de Investigaciones Metalurgicas (CENIM), Spanish Council for Scientific Research (CSIC), Avda. Gregorio del Amo, 8, 28040 Madrid (Spain)]. E-mail: mavillegas@cenim.csic.es

    2004-11-15

    Both yellow and red superficial ruby lead crystal glasses have been obtained by Ag{sup +} ion-exchange. For red ruby colouring lead glass substrates were previously doped with reducing oxides (arsenic, antimony, cerium and tin). The best experimental conditions for silver ion-exchange were determined. The optical absorption behaviour of the samples was studied to point out the influence of the parameters involved in the ion-exchange process. Moreover, other parameters affecting the final colouring of the glasses (kind of dopant, dopant concentration, etc.) were also analysed. The dopant percentage added to the lead crystal glass is the most important factor for developing superficial red ruby colouring. Antimony oxide doped lead glass ion-exchanged with silver showed the most intense red ruby colouring, even for a doping concentration lower than those of arsenic oxide doped samples able to enhance similar colour. Spectral saturation appeared for the highest doping concentration and for the most severe ion-exchange conditions. Chromatic coordinates were calculated from the corresponding transmission visible spectra. The colour purity showed by the samples obtained satisfies the ornamental requirements that motivated this research.

  9. Q-switched ruby laser in cosmetic dermatology

    Science.gov (United States)

    Kopera, Daisy

    1996-12-01

    The q-switched ruby laser has shown promising results in the treatment of blue and black tattoos. The red light of the ruby laser, 694 nm wavelength, selectively absorbed by dark pigments, is converted into heat and pigments are immediately vaporized. Energy levels range between 4, 5 and 12 J/cm2. Short exposure time does not exceed the thermal relaxation time of the target structures. Thus, thermal damage of the surrounding tissue is minimal. Not only exogenous pigment as tattoo ink but also physiological pigmented structures as melanocytes, melanosome loaden keratinocytes, and melanophages are affected by this type of laser application. Therefore the ruby laser represents a new option in the treatment of a variety of benign pigmented lesions in cosmetic dermatology. The benefit of this source can be seen in efficient clearing of the lesions without scarring. As a side effect transient hypopigmentation may occur. Ruby laser treatment of melanocytic lesions cannot be recommended because unpigmented nevus cells do not absorb red light and persist unaltered. They still bear the potency of further transformation, as into malignancy.

  10. ATCA survey of water masers in the Large Magellanic Cloud

    CERN Document Server

    Imai, H; Ellingsen, S P; Hagiwara, Y

    2013-01-01

    We have analysed archival data taken with the Australia Telescope Compact Array (ATCA) during 2001--2003 and detected nine new interstellar and circumstellar water masers in the LMC. This takes the total number of star formation water masers in the LMC to 23, spread over 14 different star forming regions and three evolved stars. Three water maser sources (N105a/MC23, N113/MC24, N157a/MC74) have been detected in all the previous observations that targeted these sites, although all show significant variability on timescales of decades. The total number of independent water maser sources now known in the LMC means that through very long baseline interferometry astrometric measurements it will be possible to construct a more precise model of the galactic rotation of the LMC and its orbital motion around the Milky Way Galaxy.

  11. Accurate OH maser positions from the SPLASH pilot region

    CERN Document Server

    Qiao, Hai-Hua; Green, James A; Breen, Shari L; Dawson, J R; Ellingsen, Simon P; Gómez, José F; Jordan, Christopher H; Shen, Zhi-Qiang; Lowe, Vicki; Jones, Paul A

    2016-01-01

    We report on high spatial resolution observations, using the Australia Telescope Compact Array (ATCA), of ground-state OH masers. These observations were carried out toward 196 pointing centres previously identified in the Southern Parkes Large-Area Survey in Hydroxyl (SPLASH) pilot region, between Galactic longitudes of $334^{\\circ}$ and $344^{\\circ}$ and Galactic latitudes of $-2^{\\circ}$ and $+2^{\\circ}$. Supplementing our data with data from the MAGMO (Mapping the Galactic Magnetic field through OH masers) survey, we find maser emission towards 175 of the 196 target fields. We conclude that about half of the 21 non-detections were due to intrinsic variability. Due to the superior sensitivity of the follow-up ATCA observations, and the ability to resolve nearby sources into separate sites, we have identified 215 OH maser sites towards the 175 fields with detections. Among these 215 OH maser sites, 111 are new detections. After comparing the positions of these 215 maser sites to the literature, we identify ...

  12. The Relationship between Class I and Class II Methanol Masers

    CERN Document Server

    Ellingsen, S P

    2005-01-01

    The Australia Telescope National Facility Mopra millimetre telescope has been used to search for 95.1-GHz class I methanol masers towards sixty-two 6.6-GHz class II methanol masers. A total of twenty-six 95.1-GHz masers were detected, eighteen of these being new discoveries. Combining the results of this search with observations reported in the literature, a near complete sample of sixty-six 6.6-GHz class II methanol masers has been searched in the 95.1-GHz transition, with detections towards 38 per cent (twenty-five detections ; not all of the sources studied in this paper qualify for the complete sample, and some of the sources in the sample were not observed in the present observations). There is no evidence of an anti-correlation between either the velocity range, or peak flux density of the class I and II transitions, contrary to suggestions from previous studies. The majority of class I methanol maser sources have a velocity range that partially overlaps with the class II maser transitions. The presence...

  13. Multibeam Maser Survey of methanol and excited OH in the Magellanic Clouds: new detections and maser abundance estimates

    CERN Document Server

    Green, J A; Fuller, G A; Breen, S L; Brooks, K; Burton, M G; Chrysostomou, A; Cox, J; Diamond, P J; Ellingsen, S P; Gray, M D; Hoare, M G; Masheder, M R W; McClure-Griffiths, N; Pestalozzi, M; Phillips, C; Quinn, L; Thompson, M A; Voronkov, M; Walsh, A; Ward-Thompson, D; Wong-McSweeney, D; Yates, J A; Cohen, R J

    2008-01-01

    We present the results of the first complete survey of the Large and Small Magellanic Clouds for 6668-MHz methanol and 6035-MHz excited-state hydroxyl masers. In addition to the survey, higher-sensitivity targeted searches towards known star-formation regions were conducted. The observations yielded the discovery of a fourth 6668-MHz methanol maser in the Large Magellanic Cloud (LMC), found towards the star-forming region N160a, and a second 6035-MHz excited-state hydroxyl maser, found towards N157a. We have also re-observed the three previously known 6668-MHz methanol masers and the single 6035-MHz hydroxyl maser. We failed to detect emission from either transition in the Small Magellanic Cloud. All observations were initially made using the Methanol Multibeam (MMB) survey receiver on the 64-m Parkes telescope as part of the MMB project and accurate positions have been measured with the Australia Telescope Compact Array (ATCA). We compare the maser populations in the Magellanic Clouds with those of our Galax...

  14. Identification of Phytophthora fragariae var. rubi by PCR.

    Science.gov (United States)

    Schlenzig, Alexandra

    2009-01-01

    The following chapter describes a PCR method for the identification of the raspberry root rot pathogen Phytophthora fragariae var. rubi. Furthermore, a nested PCR suitable for the detection of the pathogen in infected raspberry roots and validated against the "Duncan bait test" (EPPO Bull 35:87-91, 2005) is explained. Protocols for different DNA extraction methods are given which can be transferred to other fungal pathogens.

  15. Ruby on Rails测试框架研究

    Institute of Scientific and Technical Information of China (English)

    王刚

    2011-01-01

    Ruby on Rails是一个开源的web开发框架,其轻量级集成式MVC框架特别适合简单高效的开发web应用,此外Rails也提供了自动测试框架,本文将简要介绍此测试工具,并结合Rails项目的实际测试案例,讨论其优点及不足.

  16. [Agrobacterium rubi strains from blueberry plants are highly diverse].

    Science.gov (United States)

    Abrahamovich, Eliana; López, Ana C; Alippi, Adriana M

    2014-01-01

    The diversity of a collection of Agrobacterium rubi strains isolated from blueberries from different regions of Argentina was studied by conventional microbiological tests and molecular techniques. Results from biochemical and physiological reactions, as well as from rep-PCR and RFLP analysis of PCR-amplified 23S rDNA showed high phenotypic and genotypic intraspecific variation. Copyright © 2014 Asociación Argentina de Microbiología. Publicado por Elsevier España. All rights reserved.

  17. Dense Molecular Gas and H2O Maser Emission in Galaxies

    Indian Academy of Sciences (India)

    F. Huang; J. S. Zhang; R. M. Li; H. K. Li

    2014-09-01

    Extragalactic H2O masers have been found in dense gas circumstance in off-nuclear star formation regions or within parsecs of Active Galactic Nuclei (AGNs). HCN molecular (one of the best dense gas tracers) Emission has been detected in more than 60 galaxies. For HCN-detected galaxy sample, the relation of maser and gas emission was investigated here to identify physical observable properties that differentiate maser and non-maser galaxies. Our analysis results show that there is no significant difference on the infrared and gas emission between maser galaxies and galaxies without maser detection. For maser host HCN-galaxies, maser luminosity is found to be correlated to CO luminosity (a proxy of the total molecular gas) and HCN luminosity, i.e., kilomasers (H2O < 10⊙) with low maser luminosity having low gas emission luminosity, with respect to megamasers (H2O > 10⊙). For normalized maser and HCN luminosity (for removing distance effect), the correlation is still apparent. However, for normalized maser and CO luminosity, the correlation disappeared completely. Thus one proposition that the amount of dense molecular gas should be a good tracer of H2O maser emission can be made.

  18. How to Detect Inclined Water Maser Disks (and Possibly Measure Black Hole Masses)

    Science.gov (United States)

    Darling, Jeremy

    2017-03-01

    We describe a method for identifying inclined water maser disks orbiting massive black holes and for potentially using them to measure black hole masses. Owing to the geometry of maser amplification pathways, the minority of water maser disks are observable: only those viewed nearly edge-on have been identified, suggesting that an order of magnitude additional maser disks exist. We suggest that inward-propagating masers are gravitationally deflected by the central black hole, thereby scattering water maser emission out of the disk plane and enabling detection. The signature of an inclined water maser disk would be narrow masers near the systemic velocity that appear to emit from the black hole position, as identified by the radio continuum core. To explore this possibility, we present high-resolution (0.″07-0.″17) Very Large Array line and continuum observations of 13 galaxies with narrow water maser emission and show that three are good inclined-disk candidates (five remain ambiguous). For the best case, CGCG 120-039, we show that the maser and continuum emission are coincident to within 3.5 ± 1.4 pc (6.7 ± 2.7 mas). Subsequent very long baseline interferometric maps can confirm candidate inclined disks and have the potential to show maser rings or arcs that provide a direct measurement of black hole mass, although the mass precision will rely on knowledge of the size of the maser disk.

  19. Ruby on Rails构建Web敏捷开发%Agile Web Development with Ruby on Rails

    Institute of Scientific and Technical Information of China (English)

    龚贞; 李斌

    2010-01-01

    Ruby on Rails作为一种全新的WEB应用开发框架,提供了一套灵活、高效、简洁易用的解决方案,使得Web开发、部署和维护变得更简单和轻松.本文结合成都市铁路局客运卧具管理系统的实际案例,描述了Ruby on Rails便捷的遗代式增量开发和原型系统快速构建,充分展现了Rails框架的敏捷优势.

  20. INTERSTELLAR H{sub 2}O MASERS FROM J SHOCKS

    Energy Technology Data Exchange (ETDEWEB)

    Hollenbach, David [SETI Institute, Mountain View, CA 94043 (United States); Elitzur, Moshe [University of Kentucky, Lexington, KY 40506 (United States); McKee, Christopher F. [University of California, Berkeley, CA 94720 (United States)

    2013-08-10

    We present a model in which the 22 GHz H{sub 2}O masers observed in star-forming regions occur behind shocks propagating in dense regions (preshock density n{sub 0} {approx} 10{sup 6}-10{sup 8} cm{sup -3}). We focus on high-velocity (v{sub s} {approx}> 30 km s{sup -1}) dissociative J shocks in which the heat of H{sub 2} re-formation maintains a large column of {approx}300-400 K gas; at these temperatures the chemistry drives a considerable fraction of the oxygen not in CO to form H{sub 2}O. The H{sub 2}O column densities, the hydrogen densities, and the warm temperatures produced by these shocks are sufficiently high to enable powerful maser action. The observed brightness temperatures (generally {approx} 10{sup 11}-10{sup 14} K) are the result of coherent velocity regions that have dimensions in the shock plane that are 10-100 times the shock thickness of {approx}10{sup 13} cm. The masers are therefore beamed toward the observer, who typically views the shock ''edge-on'', or perpendicular to the shock velocity; the brightest masers are then observed with the lowest line-of-sight velocities with respect to the ambient gas. We present numerical and analytic studies of the dependence of the maser inversion, the resultant brightness temperature, the maser spot size and shape, the isotropic luminosity, and the maser region magnetic field on the shock parameters and the coherence path length; the overall result is that in galactic H{sub 2}O 22 GHz masers, these observed parameters can be produced in J shocks with n{sub 0} {approx} 10{sup 6}-10{sup 8} cm{sup -3} and v{sub s} {approx} 30-200 km s{sup -1}. A number of key observables such as maser shape, brightness temperature, and global isotropic luminosity depend only on the particle flux into the shock, j = n{sub 0} v{sub s} , rather than on n{sub 0} and v{sub s} separately.

  1. Observations of the Zeeman effect in Class I methanol masers

    Science.gov (United States)

    Pratim Sarma, Anuj; Momjian, Emmanuel

    2017-01-01

    We present observations of the Zeeman effect in Class I methanol maser sources toward high mass star forming regions. Toward DR21(OH), we have detected the Zeeman effect at 44 GHz in a 219 Jy/beam maser centered at an LSR velocity of 0.83 km/s, and we find $zB_\\text{los} = 53.5 \\pm 2.7$ Hz. If 44 GHz methanol masers are excited at $10^{7-8}$ cm$^{-3}$, then magnetic fields in DR21(OH) should be ~10 mG. Our detected $zB_\\text{los}$ would then imply that the Zeeman splitting factor for the 44 GHz methanol maser line should be ~5 Hz/mG. Such small values for z would not be surprising, since the methanol molecule is non-paramagnetic, like H2O. Since there are no direct measurements or calculations of the 44 GHz methanol maser Zeeman splitting factor to date, such empirical attempts could prove valuable in building a repository of measurements from which to gain an understanding of the magnitude of z.

  2. Non--local radiative transfer in strongly inverted masers

    CERN Document Server

    Daniel, F

    2013-01-01

    Maser transitions are commonly observed in media exhibiting a large range of densities and temperatures. They can be used to obtain information on the dynamics and physical conditions of the observed regions. In order to obtain reliable constraints on the physical conditions prevailing in the masing regions, it is necessary to model the excitation mechanisms of the energy levels of the observed molecules. We present a numerical method that enables us to obtain self-consistent solutions for both the statistical equilibrium and radiative transfer equations. Using the standard maser theory, the method of Short Characteristics is extended to obtain the solution of the integro-differential radiative transfer equation, appropriate to the case of intense masing lines. We have applied our method to the maser lines of the H2O molecule and we compare with the results obtained with a less accurate approach. In the regime of large maser opacities we find large differences in the intensity of the maser lines that could be...

  3. Gene flow analysis demonstrates that Phytophthora fragariae var. rubi constitutes a distinct species, Phytophthora rubi comb. nov.

    Science.gov (United States)

    Man in 't Veld, Willem A

    2007-01-01

    Isozyme analysis and cytochrome oxidase sequences were used to examine whether differentiation of P. fragariae var. fragariae and P. fragariae var. rubi at the variety level is justified. In isozyme studies six strains of both P. fragariae varieties were analyzed with malate dehydrogenase (MDH), glucose phosphate isomerase (GPI), aconitase (ACO), isocitrate dehydrogenase (IDH) and phosphogluconate dehydrogenase (PGD), comprising altogether seven putative loci. Five unique alleles (Mdh-1(A), Mdh-2(B), Gpi(A), Aco(B) and Idh-1(B)) were found in strains of P. fragariae var. fragariae, whereas five unique alleles (Mdh-1(B), Mdh-2(A), Gpi(B), Aco(A) and Idh-1(A)) were present in strains of P. fragariae var. rubi. It was inferred from these data that there is no gene flow between the two P. fragariae varieties. Cytochrome oxidase I (Cox I) sequences showed consistent differences at 15 positions between strains of Fragaria and Rubus respectively. Based on isozyme data, cytochrome oxidase I sequences, and previously published differences in restyriction enzyme patterns of mitochondrial DNA, sequences of nuclear and mitochondrial genes, AFLP patterns and pathogenicity, it was concluded that both specific pathogenic varieties of P. fragariae are reproductively isolated and constitute a distinct species. Consequently strains isolated from Rubus idaeus are assigned to Phytophthora rubi comb. nov.

  4. Water masers in the Kronian system

    Science.gov (United States)

    Pogrebenko, Sergei V.; Gurvits, Leonid I.; Elitzur, Moshe; Cosmovici, Cristiano B.; Avruch, Ian M.; Pluchino, Salvatore; Montebugnoli, Stelio; Salerno, Emma; Maccaferri, Giuseppe; Mujunen, Ari; Ritakari, Jouko; Molera, Guifre; Wagner, Jan; Uunila, Minttu; Cimo, Giuseppe; Schilliro, Francesco; Bartolini, Marco

    The presence of water has been considered for a long time as a key condition for life in planetary environments. The Cassini mission discovered water vapour in the Kronian system by detecting absorption of UV emission from a background star (Hansen et al. 2006). Prompted by this discovery, we started an observational campaign for search of another manifestation of the water vapour in the Kronian system, its maser emission at the frequency of 22 GHz (1.35 cm wavelength). Observations with the 32 m Medicina radio telescope (INAF-IRA, Italy) started in 2006 using Mk5A data recording and the JIVE-Huygens software correlator. Later on, an on-line spectrometer was used at Medicina. The 14 m Metsähovi radio telescope (TKK-MRO, Finland) joined the observational campaign in 2008 using a locally developed data capture unit and software spectrometer. More than 300 hours of observations were collected in 2006-2008 campaign with the two radio telescopes. The data were analysed at JIVE using the Doppler tracking technique to compensate the observed spectra for the radial Doppler shift for various bodies in the Kronian system (Pogrebenko et al. 2009). Here we report the observational results for Hyperion, Titan, Enceladus and Atlas, and their physical interpretation. Encouraged by these results we started a campaign of follow up observations including other radio telescopes.

  5. Amplification of OAM radiation by astrophysical masers

    Science.gov (United States)

    Gray, M. D.; Pisano, G.; Maccalli, S.; Schemmel, P.

    2014-12-01

    We extend the theory of astrophysical maser propagation through a medium with a Zeeman-split molecular response to the case of a non-uniform magnetic field, and allow a component of the electric field of the radiation in the direction of propagation: a characteristic of radiation with orbital angular momentum. A classical reduction of the governing equations leads to a set of nine differential equations for the evolution of intensity-like parameters for each Fourier component of the radiation. Four of these parameters correspond to the standard Stokes parameters, whilst the other five represent the z-component of the electric field, and its coupling to the conventional components in the x-y-plane. A restricted analytical solution of the governing equations demonstrates a non-trivial coupling of the Stokes parameters to those representing orbital angular momentum: the z-component of the electric field can grow from a background in which only Stokes-I is non-zero. A numerical solution of the governing equations reveals radiation patterns with a radial and angular structure for the case of an ideal quadrupole magnetic field perpendicular to the propagation direction. In this ideal case, generation of radiation orbital angular momentum, like polarization, can approach 100 per cent.

  6. Amplification of OAM Radiation by Astrophysical Masers

    CERN Document Server

    Gray, Malcolm; Maccalli, Stefania; Schemmel, Peter

    2014-01-01

    We extend the theory of astrophysical maser propagation through a medium with a Zeeman-split molecular response to the case of a non-uniform magnetic field, and allow a component of the electric field of the radiation in the direction of propagation: a characteristic of radiation with orbital angular momentum. A classical reduction of the governing equations leads to a set of nine differential equations for the evolution of intensity-like parameters for each Fourier component of the radiation. Four of these parameters correspond to the standard Stokes parameters, whilst the other five represent the $z$-component of the electric field, and its coupling to the conventional components in the $x-y$-plane. A restricted analytical solution of the governing equations demonstrates a non-trivial coupling of the Stokes parameters to those representing orbital angular momentum: the $z$-component of the electric field can grow from a background in which only Stokes-$I$ is non-zero. A numerical solution of the governing e...

  7. New Maser Emission from Nonmetastable Ammonia in NGC 7538. IV. Coincident Masers in Adjacent States of Para-ammonia

    CERN Document Server

    Hoffman, Ian M

    2014-01-01

    We present the first detection of para-ammonia masers in NGC 7538: multiple epochs of observation of the 14NH3 (J,K) = (10,8) and (9,8) lines. We detect both thermal absorption and nonthermal emission in the (10,8) and (9,8) transitions and the absence of a maser in the (11,8) transition. The (9,8) maser is observed to increase in intensity by 40% over six months. Using interferometric observations with a synthesized beam of 0.25", we find that the (10,8) and (9,8) masers originate at the same sky position near IRS1. With strong evidence that the (10,8) and (9,8) masers arise in the same volume, we discuss the application of pumping models for the simultaneous excitation of nonmetastable (J > K) para-ammonia states having the same value of K and consecutive values of J. We also present detections of thermal absorption in rotational states ranging in energy from E/k_B ~ 200 K to 2000 K, and several non-detections in higher-energy states. In particular, we describe the populations in eight adjacent rotational s...

  8. Proper Motions of Water Masers in Circumstellar Shells

    Science.gov (United States)

    Marvel, K. B.; Diamond, P. J.; Kemball, A. J.

    We present proper motion measurements of circumstellar water masers obtained with the VLBA. The objects observed include S Persei, VX Sagittarii, U Herculis, VY Canis Majoris, NML Cygni, IK Tauri and RX Bootis. Results of the observations and modeling indicate that the water masers exist in a kinematically complex region of the circumstellar envelope, which is not well fit by the standard model of a uniformly expanding spherical wind. Attempts at fitting an ellipsoidal geometric distribution with a variety of kinematic models are presented. Estimates for the distances of the stars are also discussed. A change in position of the maser spots as a function of velocity has been measured. This effect may be used to place limits on accelerations in the masing gas.

  9. The distribution of maser emission in OH/IR stars

    Science.gov (United States)

    Welty, Alan D.; Fix, John D.; Mutel, Robert L.

    1987-01-01

    The 1612 MHz OH emission from five OH/IR stars has been mapped at three epochs over a 2.5 yr period of time. Although the stars were observed at very different phases in the radio light curve of each, there were no remarkable changes in the appearance of the maps. This probably implies that the properties of the masers do not range widely throughout a maser shell. The maps have been used to produce star-centered surface maps of the distribution of maser emission from each star. The surface maps generally are sparsely filled with OH emission and are dominated by relatively few (about 10) major clumps of emission. The presence of large regions of low intensity in the surface maps suggests that the number of individual emitting elements is relatively small or that there are a larger number of elements which are distributed in the shell in a distinctly nonrandom manner.

  10. Multi-Wavelength Studies on H2O Maser Host Galaxies

    Indian Academy of Sciences (India)

    J. S. Zhang; J. Wang

    2011-03-01

    H2O maser emissions have been found in external galaxies for more than 30 years. Main sciences associated with extragalactic H2O masers can be summarized roughly into three parts: maser emission itself, AGN sciences and cosmology exploration. Our work in this field focusses on two projects: X-ray data analysis of individual maser source using X-ray penetrability to explore maser host obscured AGN; multi-wavelength statistical properties of the whole published H2O maser sample. Here their nuclear radio properties were investigated in detail, based on their 6-cm and 20-cm radio observation data. Comparing the radio properties between maser-detected sources and non-detected sources at similar distance scale, we find that: (1) maser host galaxies tend to have higher nuclear radio luminosity; (2) the spectral index of both samples is comparable (∼ 0.6), within the error ranges. In addition, for AGN-maser sources, the isotropic maser luminosity tends to increase with rising radio luminosity. Thus we propose the nuclear radio luminosity as one good indicator for searching AGN-masers in the future.

  11. Comparative study of the electronic structure of natural and synthetic rubies using XAFS and EDAX analyses

    Indian Academy of Sciences (India)

    P Parikh; D M Bhardwaj; R P Gupta; N L Saini; S Fernandes; R K Singhal; D C Jain; K B Garg

    2002-12-01

    We have studied the Cr–K-edge XANES and EXAFS in natural Indian rubies from two sources and a synthetic ruby at ESRF. Weight % of various constituents in them is determined using EDAX measurements. Taking the results from the three techniques together we are able to demonstrate their feasibility in quantitative study of precious stones.

  12. Ruby laser for treatment of tattoos: technical considerations affecting clinical use

    Science.gov (United States)

    Grove, Robert E.

    1990-06-01

    Recent clinical research on the use of ruby lasers for the treatment of tattoos and FIlk approval of a commercial system have renewed interest in this device. In this paper the principles of Q-switched ruby laser operation are reviewed, and potential sources of error in the estimation of delivered fluence are discussed.

  13. RubyMotion iOS develoment essentials

    CERN Document Server

    Nalwaya, Abhishek

    2013-01-01

    This is a step-by-step book that builds on your knowledge by adding to an example app over the course of each chapter. Each topic uses example code that can be compiled and tested to show how things work practically instead of just telling you the theory. Complicated tasks are broken down into easy to follow steps with clear explanations of what each line of code is doing.Whether you are a novice to iOS development or looking for a simpler alternative to Objective-C; with RubyMotion iOS Development Essentials, you will become a pro at writing great iOS apps

  14. Estimates of evapotranspiration from the Ruby Lake National Wildlife Refuge area, Ruby Valley, northeastern Nevada, May 1999-October 2000

    Science.gov (United States)

    Berger, David L.; Johnson, Michael J.; Tumbusch, Mary L.; Mackay, Jeffrey

    2001-01-01

    The Ruby Lake National Wildlife Refuge in Ruby Valley, Nevada, contains the largest area of perennial wetlands in northeastern Nevada and provides habitat to a large number of migratory and nesting waterfowl. The long-term preservation of the refuge depends on the availability of sufficient water to maintain optimal habitat conditions. In the Ruby Valley water budget, evapotranspiration (ET) from the refuge is one of the largest components of natural outflow. To help determine the amount of inflow needed to maintain wetland habitat, estimates of ET for May 1999 through October 2000 were made at major habitats throughout the refuge. The Bowen-ratio method was used to estimate daily ET at four sites: over open water, in a moderate-to-dense cover of bulrush marsh, in a moderate cover of mixed phreatophytic shrubs, and in a desert-shrub upland. The eddy-correlation method was used to estimate daily ET for periods of 2 to 12 weeks at a meadow site and at four sites in a sparse-to-moderate cover of phreatophytic shrubs. Daily ET rates ranged from less than 0.010 inch per day at all of the sites to a maximum of 0.464 inch per day at the open-water site. Average daily ET rates estimated for open water and a bulrush marsh were about four to five times greater than in areas of mixed phreatophytic shrubs, where the depth to ground water is less than 5 feet. Based on the seasonal distribution of major habitats in the refuge and on winter and summer ET rates, an estimated total of about 89,000 acre-feet of water was consumed by ET during October 1999-September 2000 (2000 water year). Of this total, about 49,800 acre-feet was consumed by ET in areas of open water and bulrush marsh.

  15. Methanol Maser Associated Outflows: Detection statistics and properties

    CERN Document Server

    de Villiers, H M; Thompson, M A; Ellingsen, S P; Urquhart, J S; Breen, S L; Burton, M G; Csengeri, T; Ward-Thompson, D

    2014-01-01

    We have selected the positions of 54 6.7GHz methanol masers from the Methanol Multibeam Survey catalogue, covering a range of longitudes between $20^{\\circ}$ and $34^{\\circ}$ of the Galactic Plane. These positions were mapped in the J=3-2 transition of both the $\\rm{^{13}CO}$ and $\\rm{C^{18}O}$ lines. A total of 58 $\\rm{^{13}CO}$ emission peaks are found in the vicinity of these maser positions. We search for outflows around all $\\rm{^{13}CO}$ peaks, and find evidence for high-velocity gas in all cases, spatially resolving the red and blue outflow lobes in 55 cases. Of these sources, 44 have resolved kinematic distances, and are closely associated with the 6.7GHz masers, a sub-set referred to as Methanol Maser Associated Outflows (MMAOs). We calculate the masses of the clumps associated with each peak using 870 $\\rm{\\mu m}$ continuum emission from the ATLASGAL survey. A strong correlation is seen between the clump mass and both outflow mass and mechanical force, lending support to models in which accretion is...

  16. Radio and IR interferometry of SiO maser stars

    CERN Document Server

    Wittkowski, M; Gray, M D; Humphreys, E M L; Karovicova, I; Scholz, M

    2012-01-01

    Radio and infrared interferometry of SiO maser stars provide complementary information on the atmosphere and circumstellar environment at comparable spatial resolution. Here, we present the latest results on the atmospheric structure and the dust condensation region of AGB stars based on our recent infrared spectro-interferometric observations, which represent the environment of SiO masers. We discuss, as an example, new results from simultaneous VLTI and VLBA observations of the Mira variable AGB star R Cnc, including VLTI near- and mid-infrared interferometry, as well as VLBA observations of the SiO maser emission toward this source. We present preliminary results from a monitoring campaign of high-frequency SiO maser emission toward evolved stars obtained with the APEX telescope, which also serves as a precursor of ALMA images of the SiO emitting region. We speculate that large-scale long-period chaotic motion in the extended molecular atmosphere may be the physical reason for observed deviations from poin...

  17. First microwave generation in the FOM free-electron maser

    NARCIS (Netherlands)

    Verhoeven, A. G. A.; Bongers, W. A.; Bratman, V. L.; Caplan, M.; Denisov, G. G.; van der Geer, C. A. J.; Manintveld, P.; Poelman, A. J.; Pluygers, J.; Shmelyov, M. Y.; Smeets, P. H. M.; Sterk, A. B.; Urbanus, W. H.

    1998-01-01

    A free-electron maser (FEM) has been built as a pilot experiment for a millimetre-wave source for applications on future fusion research devices such as ITER, the International Tokamak Experimental Reactor. A unique feature of the Dutch fusion FEM is the possibility to tune the frequency over the en

  18. First high power experiments with the Dutch free electron maser

    NARCIS (Netherlands)

    Verhoeven, A. G. A.; Bongers, W. A.; Bratman, V. L.; Caplan, M.; Denisov, G. G.; van Dijk, G.; van der Geer, C. A. J.; Manintveld, P.; Poelman, A. J.; Pluygers, J.; Shmelyov, M. Y.; Smeets, P. H. M.; Sterk, A. B.; Urbanus, W. H.

    1998-01-01

    A free electron maser (FEM) has been built as a mm-wave source for applications on future fusion research devices such as ITER, the international tokamak experimental reactor [M. A. Makowski, F. Elio, and D. Loeser, April 97, Proc. 10th Workshop on ECE and ECRH, EC10, 549-559. World Scientific (1998

  19. OH maser outburst in the W3 nebula

    Science.gov (United States)

    Gosachinskij, I. V.; Grenkov, S. A.; Ipatov, A. V.; Rakhimov, I. A.

    2016-07-01

    We report the results of three-year long observations of OH masers at 1665 MHz in the W3(OH) source carried out with the 32-m antenna of Svetloe Radio Astronomical Observatory.We found that the strongest activity during the period from December 2011 through March 2012 was exhibited by the region at radial velocity -46.2km s-1. The region showed no activity in the ensuing time. The most striking outburst was the event that occurred on January 23, 2013 at UT 03:27. At that time the flux of the region increased by a factor of seven in 90 s, and then decreased down to the initial level. Such a time scale yields the upper estimate of 0.18 AU (2.7 × 1012 cm) for the linear size of the maser dot. In 2013-2014 intensity variations were found the -47.6 and -45.1km s-1 components with time scales on the order of 10 hours and anticorrelated behavior of the left- and right-hand polarization fluxes. This is the first time that such phenomena have been found in the behavior of OH maser emission, and they cannot be explained by any existing models of maser variability.

  20. Single-dish monitoring of circumstellar water masers

    CERN Document Server

    Brand, J; Engels, D

    2002-01-01

    We present an overview of the long-term water maser monitoring program of a sample of late-type stars, carried out with the Medicina 32-m and Effelsberg 100-m telescopes, and describe the results in some detail. The role the SRT (Sardinia Radio Telescope) could play in this program is outlined.

  1. Star-forming protoclusters associated with methanol masers

    CERN Document Server

    Minier, V; Hill, T; Pestalozzi, M R; Purcell, C R; Garay, G; Walsh, A; Longmore, S N

    2004-01-01

    We present a multiwavelength study of five methanol maser sites which are not directly associated with a strong ($>100$ mJy) radio continuum source: G 31.28+0.06, G 59.78+0.06, G 173.49+2.42 (S231, S233IR), G 188.95+0.89 (S252, AFGL5180) and G 192.60-0.05 (S255IR). These radio-quiet methanol maser sites are often interpreted as precursors of ultra-compact \\ion{H}{ii} regions or massive protostar sites. In this work, the environment of methanol masers is probed from mid-IR to millimetre wavelengths at angular resolutions of $8''-34''$. Spectral energy distribution (SED) diagrams for each site are presented, together with mass and luminosity estimates. Each radio-quiet maser site is always associated with a massive ($>50$ M$_{\\odot}$), deeply embedded ($A_v>40$ mag) and very luminous ($>10^4$ S L$_{\\odot}$) molecular clump, with $L_{total}{\\propto}M_{gas}^{0.75}$. These physical properties characterise massive star-forming clumps in earlier evolutionary phases than \\ion{H}{ii} regions. In addition, colder gas c...

  2. RAPID FLUCTUATIONS OF WATER MASER EMISSION IN VY CMa

    Institute of Scientific and Technical Information of China (English)

    ZhengXingwu; EugenioScaliseJr; HanFu

    1999-01-01

    The monitoring observations of the short- time variation of the water maser to-ward the supergiant star of VY CMa were carried out from August 26 through September 24 1993, using the 13.7 m telescope at the Qinghai station of the Purple

  3. The diversity of methanol maser morphologies from VLBI observations

    CERN Document Server

    Bartkiewicz, A; Van Langevelde, H J; Richards, A M S; Pihlström, Y M

    2009-01-01

    We investigate which structures the 6.7 GHz methanol masers trace in the environment of high-mass protostar candidates by observing a homogenous sample of methanol masers selected from Torun surveys. We also probed their origins by looking for associated H II regions and IR emission. We selected 30 methanol sources with improved position accuracies achieved using MERLIN and another 3 from the literature. We imaged 31 of these using the European VLBI Network's expanded array of telescopes with 5-cm (6-GHz) receivers. We used the VLA to search for 8.4 GHz radio continuum counterparts and inspected Spitzer GLIMPSE data at 3.6-8 um from the archive. High angular resolution images allowed us to analyze the morphology and kinematics of the methanol masers in great detail and verify their association with radio continuum and mid-infrared emission. A new class of "ring-like" methanol masers in star--forming regions appeared to be suprisingly common, 29 % of the sample. The new morphology strongly suggests that methan...

  4. Interstellar H$_2$O Masers from J Shocks

    CERN Document Server

    Hollenbach, David; McKee, Christopher F

    2013-01-01

    We present a model in which the 22 GHz H$_2$O masers observed in star-forming regions occur behind shocks propagating in dense regions (preshock density $n_0 \\sim 10^6 - 10^8$ cm$^{-3}$). We focus on high-velocity ($v_s > 30$ km s$^{-1}$) dissociative J shocks in which the heat of H$_2$ re-formation maintains a large column of $\\sim 300-400$ K gas; at these temperatures the chemistry drives a considerable fraction of the oxygen not in CO to form H$_2$O. The H$_2$O column densities, the hydrogen densities, and the warm temperatures produced by these shocks are sufficiently high to enable powerful maser action. The observed brightness temperatures (generally $\\sim 10^{11} - 10^{14}$ K) are the result of coherent velocity regions that have dimensions in the shock plane that are 10 to 100 times the shock thickness of $\\sim 10^{13}$ cm. The masers are therefore beamed towards the observer, who typically views the shock "edge-on", or perpendicular to the shock velocity; the brightest masers are then observed with t...

  5. SiO and CH3OH mega-masers in NGC 1068

    Science.gov (United States)

    Wang, Junzhi; Zhang, Jiangshui; Gao, Yu; Zhang, Zhi-Yu; Li, Di; Fang, Min; Shi, Yong

    2014-11-01

    Maser is an acronym for microwave amplification by stimulated emission of radiation; in astronomy mega-masers are masers in galaxies that are ≥106 times more luminous than typical galactic maser sources. Observational studies of mega-masers can help us to understand their origins and characteristics. More importantly, mega-masers can be used as diagnostic tracers to probe the physical properties of their parent galaxies. Since the late 1970s, only three types of molecules have been found to form mega-masers: H2O, OH and H2CO. Here we report the detection of both SiO and CH3OH mega-masers near the centre of Seyfert 2 galaxy NGC 1068 at millimetre wavelengths, obtained using the IRAM 30-m telescope. We argue that the SiO mega-maser originated from the nuclear disk and the CH3OH mega-maser originated from shock fronts. High-resolution observations in the future will enable us to investigate AGN feedback and determine the masses of central supermassive black holes in such galaxies.

  6. Search for class II methanol masers at 23.1 GHz

    CERN Document Server

    Cragg, D M; Caswell, J L; Ellingsen, S P; Godfrey, P D

    2004-01-01

    In the early days of methanol maser discoveries the 9(2)-10(1) A+ transition at 23.1 GHz was found to exhibit maser characteristics in the northern star-forming region W3(OH), and probable maser emission in two other sources. Attention subsequently turned to the 6.6-GHz 5(1)-6(0) A+ methanol maser transition, which has proved a valuable tracer of early high-mass star formation. We have undertaken a new search for 23.1-GHz methanol masers in 50 southern star formation regions using the Parkes radiotelescope. The target sources all exhibit class II methanol maser emission at 6.6 GHz, with 20 sources also displaying maser features in the 107.0-GHz 3(1)-4(0) A+ methanol line. Strong emission at 23.1 GHz in NGC 6334F was confirmed, but no emission was detected in the remaining sources. Thus the 23.1-GHz methanol masers are rare. A maser model in which methanol molecules are pumped to the second torsionally excited state by radiation from warm dust can account for class II maser activity in all the transitions in w...

  7. UNUSUAL SHOCK-EXCITED OH MASER EMISSION IN A YOUNG PLANETARY NEBULA

    Energy Technology Data Exchange (ETDEWEB)

    Qiao, Hai-Hua; Shen, Zhi-Qiang [Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Rd, Shanghai, 200030 (China); Walsh, Andrew J. [International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845 (Australia); Gómez, José F. [Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía s/n, E-18008, Granada (Spain); Imai, Hiroshi [Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065 (Japan); Green, James A. [SKA Organisation, Jodrell Bank Observatory, Lower Withington, Macclesfield, Cheshire SK11 9DL (United Kingdom); Dawson, Joanne R. [Department of Physics and Astronomy and MQ Research Centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University, NSW 2109 (Australia); Ellingsen, Simon P. [School of Physical Sciences, Private Bag 37, University of Tasmania, Hobart 7001, TAS (Australia); Breen, Shari L. [Australia Telescope National Facility, CSIRO Astronomy and Space Science, P.O. Box 76, Epping, NSW 1710 (Australia); Jones, Paul A.; Cunningham, Maria R. [School of Physics, University of New South Wales, Sydney, NSW 2052 (Australia); Gibson, Steven J., E-mail: haihua.qiao@curtin.edu.au [Department of Physics and Astronomy, Western Kentucky University, 1906 College Heights Blvd, Bowling Green, KY 42101 (United States)

    2016-01-20

    We report on OH maser emission toward G336.644−0.695 (IRAS 16333−4807), which is a H{sub 2}O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3−35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H{sub 2}O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s{sup −1}). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of ∼2 to ∼10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN.

  8. Unusual shock-excited OH maser emission in a young Planetary Nebula

    CERN Document Server

    Qiao, Hai-Hua; Gomez, Jose F; Imai, Hiroshi; Green, James A; Dawson, Joanne R; Shen, Zhi-Qiang; Ellingsen, Simon P; Breen, Shari L; Jones, Paul A; Gibson, Steven J; Cunningham, Maria R

    2015-01-01

    We report on OH maser emission toward G336.644-0.695 (IRAS 16333-4807), which is a H2O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667 and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array (ATCA), hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3-35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H2O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km/s). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of ~2 to ~10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation ...

  9. Infrared characteristics of sources associated with OH, H2O, SiO and CH3OH masers

    CERN Document Server

    Esimbek, Jarken; Wu, Gang; Di Tang, Xin

    2013-01-01

    We collect all published OH, H2O, SiO and CH3OH masers in literature. The as-sociated infrared sources of these four masers were identi?ed with MSX PSC catalogues. We look for common infrared properties among the sources associated with four masers and make a statistical study. The MSX sources associated with stellar OH, stellar H2O and SiO masers concentrated in a small regions and the MSX sources associated with interstellar OH, interstellar H2O and CH3OH masers also concentrated in a small regions in an [A]-[D].vs.[A][-[E] diagram. These results give us new criterion to search for coexisting stellar maser samples for OH, H2O and SiO masers and interstellar maser samples for OH, H2O and CH3OH masers.

  10. Extended CH3OH maser flare excited by a bursting massive YSO

    Science.gov (United States)

    Moscadelli, L.; Sanna, A.; Goddi, C.; Walmsley, M. C.; Cesaroni, R.; Caratti o Garatti, A.; Stecklum, B.; Menten, K. M.; Kraus, A.

    2017-04-01

    Aims: Recently, substantial flaring in the 6.7 GHz methanol maser line has been observed toward the high-mass young stellar object (YSO) S255 NIRS 3, where an accretion burst was also detected in the IR. Our goal is to study the change in the properties of the 6.7 GHz masers between the pre- and outburst phases, and investigate the connection between the maser and the accretion burst. Methods: With the Karl G. Jansky Very Large Array (JVLA) and the European VLBI Network (EVN), we performed observations of the 6.7 GHz masers (covering a range in angular resolution from a few milliarcseconds to ≈1'') during the burst phase and compared these observations with pre-burst measurements at similar spatial scales. Results: The accretion burst and the subsequent increase in IR luminosity are very likely the origin of the 6.7 GHz maser flare. Since most maser centers operate in the unsaturated regime, a change by a relatively small factor (≈5) in the flux of pumping photons has produced an exponential growth in the maser intensity. The main pre-burst maser cluster is no longer detected during the burst. Compared to the pre-burst phase, flaring 6.7 GHz masers emit across a different VLSR range that is more strongly redshifted, and the emission extends over a larger area at larger separation from the high-mass YSO. In particular, the outburst peak emission originates from a remarkably extended (0.̋2-0.̋3) maser plateau at a radial distance of 500-1000 AU from the source. Conclusions: Both the maser flare and the extraordinarily large extent of the maser structure can be a natural consequence of the burst in the accretion luminosity of the high-mass YSO. Our results strongly support models that predict IR radiative pumping for the 6.7 GHz CH3OH masers.

  11. Suficiência amostral para mudas de cafeeiro cv. Rubi

    Directory of Open Access Journals (Sweden)

    Patriciani Estela Cipriano

    2012-04-01

    Full Text Available O número de plantas por parcela experimental é de extrema importância para a precisão dos resultados. O objetivou deste trabalho é encontrar o tamanho ótimo para experimentos de mudas de cafeeiro da cultivar Rubi MG 1192. O experimento foi instalado no Instituto Federal de Educação, Ciência e Tecnologia do Sul de Minas Gerais (IFSULDEMINAS, campus Machado. As plantas foram dispostas em 14 fileiras com 14 plantas em cada linha. Foram descartadas a primeira e última fileira e a primeira e última linha, as quais tiveram função de bordadura. Utilizaram-se, portanto, 144 mudas que individualmente caracterizavam as unidades básicas (UB. As avaliações ocorreram quando as plantas atingiram o sexto par de folhas definitivo e as variáveis respostas foram coletadas. Cada uma das 144 UB foi utilizada para simular 14 diferentes tamanhos de parcelas de 1UB até 72UB. Não foi considerada a forma das parcelas. Para cada um desses agrupamentos foi calculado o coeficiente de variação médio. Verificou-se que o tamanho ótimo de parcela útil para experimentos com mudas de café da cultivar Rubi MG 1192 varia de 2 a 8 mudas por parcela, de acordo com a variável em estudo.

  12. BioC implementations in Go, Perl, Python and Ruby.

    Science.gov (United States)

    Liu, Wanli; Islamaj Doğan, Rezarta; Kwon, Dongseop; Marques, Hernani; Rinaldi, Fabio; Wilbur, W John; Comeau, Donald C

    2014-01-01

    As part of a communitywide effort for evaluating text mining and information extraction systems applied to the biomedical domain, BioC is focused on the goal of interoperability, currently a major barrier to wide-scale adoption of text mining tools. BioC is a simple XML format, specified by DTD, for exchanging data for biomedical natural language processing. With initial implementations in C++ and Java, BioC provides libraries of code for reading and writing BioC text documents and annotations. We extend BioC to Perl, Python, Go and Ruby. We used SWIG to extend the C++ implementation for Perl and one Python implementation. A second Python implementation and the Ruby implementation use native data structures and libraries. BioC is also implemented in the Google language Go. BioC modules are functional in all of these languages, which can facilitate text mining tasks. BioC implementations are freely available through the BioC site: http://bioc.sourceforge.net. Database URL: http://bioc.sourceforge.net/

  13. Simulated Galactic methanol maser distribution to constrain Milky Way parameters

    Science.gov (United States)

    Quiroga-Nuñez, L. H.; van Langevelde, H. J.; Reid, M. J.; Green, J. A.

    2017-08-01

    Context. Using trigonometric parallaxes and proper motions of masers associated with massive young stars, the Bar and Spiral Structure Legacy (BeSSeL) survey has reported the most accurate values of the Galactic parameters so far. The determination of these parameters with high accuracy has a widespread impact on Galactic and extragalactic measurements. Aims: This research is aimed at establishing the confidence with which such parameters can be determined. This is relevant for the data published in the context of the BeSSeL survey collaboration, but also for future observations, in particular from the southern hemisphere. In addition, some astrophysical properties of the masers can be constrained, notably the luminosity function. Methods: We have simulated the population of maser-bearing young stars associated with Galactic spiral structure, generating several samples and comparing them with the observed samples used in the BeSSeL survey. Consequently, we checked the determination of Galactic parameters for observational biases introduced by the sample selection. Results: Galactic parameters obtained by the BeSSeL survey do not seem to be biased by the sample selection used. In fact, the published error estimates appear to be conservative for most of the parameters. We show that future BeSSeL data and future observations with southern arrays will improve the Galactic parameters estimates and smoothly reduce their mutual correlation. Moreover, by modeling future parallax data with larger distance values and, thus, greater relative uncertainties for a larger numbers of sources, we found that parallax-distance biasing is an important issue. Hence, using fractional parallax uncertainty in the weighting of the motion data is imperative. Finally, the luminosity function for 6.7 GHz methanol masers was determined, allowing us to estimate the number of Galactic methanol masers.

  14. Search for sub-millimeter H2O masers in active galaxies - the detection of a 321 GHz H2O maser in NGC4945

    CERN Document Server

    Hagiwara, Yoshiaki; Doi, Akihiro; Miyoshi, Makoto; Edwards, Philip G

    2016-01-01

    We present further results of a search for extragalactic submillimeter H2O masers using the Atacama Large Millimeter/Submillimeter Array (ALMA). The detection of a 321 GHz H2O maser in the nearby Type 2 Seyfert galaxy, the Circinus galaxy, has previously been reported, and here the spectral analysis of four other galaxies is described. A 321 GHz H2O maser is newly detected toward the center of NGC 4945, a nearby Type 2 Seyfert. The maser shows Doppler-shifted velocity features with velocity ranges similar to those of the 22 GHz H2O maser, however the non-contemporaneous observations also show differences in velocity offsets. The sub-parsec-scale distribution of the 22 GHz H2O masers revealed by earlier VLBI (Very Long Baseline Interferometry) observations suggests that the submillimeter masers could arise in an edge-on rotating disk. The maser features remain unresolved at the synthesized beam of ~0.54 (~30 pc) and are located toward the 321 GHz continuum peak within errors. There is some evidence for a high-...

  15. New Phase Fitted and Amplification Fitted Numerov-Type Methods for Periodic IVPs with Two Frequencies

    Directory of Open Access Journals (Sweden)

    Yonglei Fang

    2012-01-01

    Full Text Available Phase fitted and amplification fitted Numerov-type methods for periodic initial value problems with two frequencies are investigated. A one-frequency method and a two-frequency method are constructed. The two new methods both have algebraic order five and are dispersive of order six and dissipative of order five. The two-dimensional absolute stability region for the one-frequency method and the three-dimensional absolute stability region for the two-frequency method are plotted. Numerical experiments are reported to show the efficiency and competence of the two new methods.

  16. A Search for Submillimeter H2O Masers in Active Galaxies: The Detection of 321 GHZ H2O Maser Emission in NGC 4945

    Science.gov (United States)

    Hagiwara, Yoshiaki; Horiuchi, Shinji; Doi, Akihiro; Miyoshi, Makoto; Edwards, Philip G.

    2016-08-01

    We present further results of a search for extragalactic submillimeter H2O masers using the Atacama Large Millimeter/submillimeter Array (ALMA). The detection of a 321 GHz H2O maser in the nearby type 2 Seyfert galaxy, the Circinus galaxy, has previously been reported, and here the spectral analysis of four other galaxies is described. We have discovered H2O maser emission at 321 GHz toward the center of NGC 4945, a nearby type 2 Seyfert. The maser emission shows Doppler-shifted velocity features with velocity ranges similar to those of the previously reported 22 GHz H2O masers however, the non-contemporaneous observations also show differences in velocity offsets. The subparsec-scale distribution of the 22 GHz H2O masers revealed by earlier very long baseline interferometry observations suggests that the submillimeter masers could arise in an edge-on rotating disk. The maser features remain unresolved by the synthesized beam of ˜0.″54 (˜30 pc) and are located toward the 321 GHz continuum peak within errors. A marginally detected (3σ) high-velocity feature is redshifted by 579 km {{{s}}}-1 with respect to the systemic velocity of the galaxy. Assuming that this feature is real and arises from a Keplerian rotating disk in this galaxy, it is located at a radius of ˜0.020 pc (˜1.5 × 105 Schwarzschild radii), which would enable molecular material closer to the central engine to be probed than the 22 GHz H2O masers. This detection confirms that submillimeter H2O masers are a potential tracer of the circumnuclear regions of active galaxies, which will benefit from higher angular resolution studies with ALMA.

  17. CaRuby-Nano: a novel high affinity calcium probe for dual color imaging.

    Science.gov (United States)

    Collot, Mayeul; Wilms, Christian D; Bentkhayet, Asma; Marcaggi, Païkan; Couchman, Kiri; Charpak, Serge; Dieudonné, Stéphane; Häusser, Michael; Feltz, Anne; Mallet, Jean-Maurice

    2015-03-31

    The great demand for long-wavelength and high signal-to-noise Ca(2+) indicators has led us to develop CaRuby-Nano, a new functionalizable red calcium indicator with nanomolar affinity for use in cell biology and neuroscience research. In addition, we generated CaRuby-Nano dextran conjugates and an AM-ester variant for bulk loading of tissue. We tested the new indicator using in vitro and in vivo experiments demonstrating the high sensitivity of CaRuby-Nano as well as its power in dual color imaging experiments.

  18. The cyclotron maser theory of AKR and Z-mode radiation. [Auroral Kilometric Radiation

    Science.gov (United States)

    Wu, C. S.

    1985-01-01

    The cyclotron maser mechanism which may be responsible for the generation of auroral kilometric radiation and Z-mode radiation is discussed. Emphasis is placed on the basic concepts of the cyclotron maser theory, particularly the relativistic effect of the cyclotron resonance condition. Recent development of the theory is reviewed. Finally, the results of a computer simulation study which helps to understand the nonlinear saturation of the maser instability are reported.

  19. FORMALDEHYDE MASERS: EXCLUSIVE TRACERS OF HIGH-MASS STAR FORMATION

    Energy Technology Data Exchange (ETDEWEB)

    Araya, E. D.; Brown, J. E. [Western Illinois University, Physics Department, 1 University Circle, Macomb, IL 61455 (United States); Olmi, L. [INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze (Italy); Ortiz, J. Morales [University of Puerto Rico, Río Piedras Campus, Physical Sciences Department, P.O. Box 23323, San Juan, PR 00931 (United States); Hofner, P.; Creech-Eakman, M. J. [New Mexico Institute of Mining and Technology, Physics Department, 801 Leroy Place, Socorro, NM 87801 (United States); Kurtz, S. [Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apdo. Postal 3-72, 58089 Morelia, Michoacán (Mexico); Linz, H. [Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg (Germany)

    2015-11-15

    The detection of four formaldehyde (H{sub 2}CO) maser regions toward young high-mass stellar objects in the last decade, in addition to the three previously known regions, calls for an investigation of whether H{sub 2}CO masers are an exclusive tracer of young high-mass stellar objects. We report the first survey specifically focused on the search for 6 cm H{sub 2}CO masers toward non high-mass star-forming regions (non HMSFRs). The observations were conducted with the 305 m Arecibo Telescope toward 25 low-mass star-forming regions, 15 planetary nebulae and post-AGB stars, and 31 late-type stars. We detected no H{sub 2}CO emission in our sample of non HMSFRs. To check for the association between high-mass star formation and H{sub 2}CO masers, we also conducted a survey toward 22 high-mass star-forming regions from a Hi-GAL (Herschel infrared Galactic Plane Survey) sample known to harbor 6.7 GHz CH{sub 3}OH masers. We detected a new 6 cm H{sub 2}CO emission line in G32.74−0.07. This work provides further evidence that supports an exclusive association between H{sub 2}CO masers and young regions of high-mass star formation. Furthermore, we detected H{sub 2}CO absorption toward all Hi-GAL sources, and toward 24 low-mass star-forming regions. We also conducted a simultaneous survey for OH (4660, 4750, 4765 MHz), H110α (4874 MHz), HCOOH (4916 MHz), CH{sub 3}OH (5005 MHz), and CH{sub 2}NH (5289 MHz) toward 68 of the sources in our sample of non HMSFRs. With the exception of the detection of a 4765 MHz OH line toward a pre-planetary nebula (IRAS 04395+3601), we detected no other spectral line to an upper limit of 15 mJy for most sources.

  20. High Resolution Surveys of the Water and Methanol Star Formation Masers in the Central Molecular Zone

    Science.gov (United States)

    Rickert, Matthew; Yusef-Zadeh, Farhad; Ott, Juergen; Meier, David S.; Krieger, Nico; SWAG

    2017-01-01

    We present some of the first high resolution fully interferometric surveys of 6.7 GHz methanol and 22 GHz water masers towards the Central Molecular Zone (CMZ). These masers are good signposts for early (methanol masers with resolutions of 0.9” (0.04 pc) and 0.4 km/s (8 kHz) and an average channel sensitivity of ~0.01 Jy/beam. With this high resolution and sensitivity, we have detected ~100 methanol masers, which is over a factor of two more than has previously been detected. We have also conducted two surveys of water masers in this region. As part of the Survey of Water and Ammonia in the Galactic Center (SWAG), the Australia Telescope Compact Array (ATCA) was used to survey a variety of molecular lines, including the 22 GHz water line. With the ATCA, we have detected over 200 water masers using resolutions of 26” (1 pc) and 2 km/s (60 kHz) and an average channel sensitivity of ~0.01 Jy/beam. Afterward, we conducted the first on-the-fly (OTF) VLA survey of water masers with improved resolutions of 0.7” (0.03 pc) and 0.4 km/s (26 kHz) and an average channel sensitivity of ~0.05 Jy/beam. Although the analysis of this OTF survey is not yet complete, we have already identified water masers that were not visible in the SWAG data.The improvement in the number of detected masers allows us to better analyze the distribution of these masers. We show that the SWAG water masers appear uniformly distributed along the Galactic plane, despite the asymmetry of the molecular gas distribution, where ~2/3 of the gas mass is located at positive Galactic longitudes. The methanol masers follow the molecular gas distribution, with a majority of the masers being found at positive longitudes. This could indicate a difference in the star forming history of these two parts of the CMZ and/or that the 22 GHz water masers are contaminated by water masers produced from evolved stars as well as star forming regions, indicating that a larger percentage of 22 GHz water masers are produced

  1. Masers associated with high-mass star formation regions in the Large Magellanic Cloud

    CERN Document Server

    Ellingsen, S P; Caswell, J L; Quinn, L J; Fuller, G A

    2010-01-01

    We report the results of a sensitive search for 12.2 GHz methanol maser emission towards a sample of eight high-mass star formation regions in the Large Magellanic Clouds which have been detected in other maser transitions. We detected one source towards the star formation region N105a. This is the first detection of a 12.2 GHz methanol maser outside our Galaxy. We also made near-contemporaneous observations of the 6.7 GHz methanol and 22 GHz water masers towards these sources, resulting in the detection of water maser emission in six new sources, including one associated with the strongest 6.7 GHz maser in the Magellanic Clouds IRAS 05011-6815. The majority of the maser sources are closely associated with objects identified as likely Young Stellar Objects (YSO) on the basis of Spitzer Space Telescope observations. We find that the YSOs associated with masers tend to be more luminous and have redder infrared colours than the sample as a whole. SED modeling of the YSOs shows that the masers are associated with...

  2. Class II 6.7 GHz Methanol Maser Association with Young Massive Cores Revealed by ALMA

    Science.gov (United States)

    Chibueze, James O.; Csengeri, Timea; Tatematsu, Ken’ichi; Hasegawa, Tetsuo; Iguchi, Satoru; Alhassan, Jibrin A.; Higuchi, Aya E.; Bontemps, Sylvain; Menten, Karl M.

    2017-02-01

    We explored the implication of the association (or lack of it) of 6.7 GHz class II methanol (CH3OH) masers with massive dense cores (MDCs) detected (within a sample of ATLASGAL selected infrared quiet massive clumps) at 0.9 mm with Atacama Large Millimeter/submillimeter array. We found 42 out of the 112 cores (37.5%) detected with the Atacama Compact Array (ACA) to be associated with 6.7 GHz CH3OH masers. The lowest mass core with CH3OH maser association is ∼ 12 {M}ȯ . The angular offsets of the ACA cores from the 6.7 GHz CH3OH maser peak positions range from 0.″17 to 4.″79, with a median value of 2.″19. We found a weak correlation between the 0.9 mm continuum (MDCs) peak fluxes and the peak fluxes of their associated methanol multibeam (MMB) 6.7 GHz CH3OH masers. About 90% of the cores associated with 6.7 GHz CH3OH masers have masses of >40 M ⊙. The CH3OH maser containing cores are candidates for embedded high-mass protostellar objects in their earliest evolutionary stages. With our ACA 0.9 continuum data compared with the MMB 6.7 GHz CH3OH maser survey, we have constrained the cores already housing massive protostars based on their association with the radiatively pumped 6.7 GHz CH3OH masers.

  3. Distribution of SiO and OH Maser Stars inthe Galactic Plane

    Institute of Scientific and Technical Information of China (English)

    2001-01-01

    The observational results of the Nobeyama 45-m SiO maser survey and the Arecibo 305-m OH maser survey are assembled for an analysis of the distribution and kinematics of late-type stars in the Galactic plane.It is found that neither SiO maser stars nor OH maser stars show any concentration to the spiral arms,which imply that they do not belong to the arm population and quite possibly they are low-mass stars in late stage of evolution.A rotational curve is also derived for these objects and a few features which may be real are discussed and compared with those

  4. Supernova Remnant Shock - Molecular Cloud Interactions: Masers as tracers of hadronic particle acceleration

    CERN Document Server

    Frail, Dale A

    2011-01-01

    We review the class of galactic supernova remnants which show strong interactions with molecular clouds, revealed through shock-excited hydroxyl masers. These remnants are preferentially found among the known GeV and TeV detections of supernova remnants. It has been argued that the masers trace out the sites of hadronic particle acceleration. We discuss what is known about the physical conditions of these shocked regions and we introduce a potential new maser tracer for identifying the sites of cosmic ray acceleration. This review includes a reasonably complete bibliography for researchers new to the topic of shock-excited masers and supernova remnants.

  5. Stress determination in thermally grown alumina scales using ruby luminescence

    Energy Technology Data Exchange (ETDEWEB)

    Renusch, D.; Veal, B.W.; Koshelev, I.; Natesan, K.; Grimsditch [Argonne National Lab., IL (United States); Hou, P.Y. [Lawrence Berkeley Lab., CA (United States)

    1996-06-01

    By exploiting the strain dependence of the ruby luminescence line, we have measured the strain in alumina scales thermally grown on Fe-Cr- Al alloys. Results are compared and found to be reasonably consistent with strains determined using x rays. Oxidation studies were carried out on alloys Fe - 5Cr - 28Al and Fe - 18Cr - 10Al (at.%). Significantly different levels of strain buildup were observed in scales on these alloys. Results on similar alloys containing a ``reactive element`` (Zr or Hf) in dilute quantity are also presented. Scales on alloys containing a reactive element (RE) can support significantly higher strains than scales on RE-free alloys. With the luminescence technique, strain relief associated with spallation thresholds is readily observed.

  6. Passive Seismic Imaging of the Ruby Mountains Core Complex, Nevada

    Science.gov (United States)

    Litherland, M.; Klemperer, S. L.

    2015-12-01

    We investigate the deep crustal structure of the Ruby Mountains Core Complex (RMCC) using data collected from the Ruby Mountains Seismic Experiment. This project, part of the Earthscope Flexible Array program, deployed 50 passive broadband stations across the RMCC from 2010 to 2012. Previous investigations of the area have included extensive surface mapping and active seismic profiles across the surrounding basins, but better imaging beneath the mountain range is needed to understand the tectonic processes that formed the RMCC. The RMCC exhibits typical core-complex structure of deep crustal rocks exhumed to the surface beneath a gently dipping detachment, with a thick mylonitic shear zone directly underlying the detachment. In the RMCC, the westward dip of the detachment, the ~1km-thick mylonite zone formed in the Paleogene, and a south-to-north increase in metamorphic grade provide targets for imaging. We used common conversion point stacking of receiver functions to produce 3 profiles of structural discontinuities beneath the RMCC: one along the axis of the RMCC, and two crossing lines, one in the northern RMCC, and one in the southern part of the range. Due to the deep sedimentary basins surrounding the RMCC, various de-multiple processes were required to reduce the effects of basin reverberations. To better constrain the velocity structure of the area, we used ambient-noise tomography, and finally, we produced a joint inversion of our receiver functions and ambient-noise data. We observe a mostly flat Moho at about 30 km depth beneath the RMCC that dips slightly to the south, with faint mid-crustal converters that also dip south at ~30°. In the southern RMCC, the Moho dips ~20° westward, but this is not observed in the northern RMCC. This suggests that much of the exhumation involved in the RMCC formation likely involved ductile flow that left a mostly flat Moho, but more recent processes also may have left observable changes in lower-crustal structure.

  7. Comparison of three Statistical Classification Techniques for Maser Identification

    CERN Document Server

    Manning, Ellen M; Ellingsen, Simon P; Breen, Shari L; Chen, Xi; Humphries, Melissa

    2016-01-01

    We applied three statistical classification techniques - linear discriminant analysis (LDA), logistic regression and random forests - to three astronomical datasets associated with searches for interstellar masers. We compared the performance of these methods in identifying whether specific mid-infrared or millimetre continuum sources are likely to have associated interstellar masers. We also discuss the ease, or otherwise, with which the results of each classification technique can be interpreted. Non-parametric methods have the potential to make accurate predictions when there are complex relationships between critical parameters. We found that for the small datasets the parametric methods logistic regression and LDA performed best, for the largest dataset the non-parametric method of random forests performed with comparable accuracy to parametric techniques, rather than any significant improvement. This suggests that at least for the specific examples investigated here accuracy of the predictions obtained ...

  8. Positron-Cyclotron Maser for the Core Emissions from Pulsars

    CERN Document Server

    Ma, C; Wang, D; Wu, X; Ma, Chun-yu; Mao, Ding-yi; Wang, De-yu; Wu, Xin-ji

    1997-01-01

    We use the cyclotron-maser theory to explain the core emission from the magnetosphere of pulsars. As a kind of direct and efficient maser type of emission, it can give rise to escaping radiation with extremely high brightness temperature and narrow angle with respect to the magnetic axis. We find that the growth rates and real frequencies of the O-mode electromagnetic wave propagating parallel to the magnetic fields depend on the ratio of the plasma frequency $\\omega_p$ and the gyrofrequency $\\omega_b$ rather than the plasma frequency alone, as described by other models. The emission takes place in the region where the magnitude of $\\omega_p/\\omega_b$ is $10^{-2}$. The corresponding altitude is about a few decades of neutron star radius, where the magnetic field strength is about $10^6-10^8 G$. The qualitative spectrum and the lower frequency cut-off of the radio emission is obtained by this model.

  9. Asymptotic inference in system identification for the atom maser.

    Science.gov (United States)

    Catana, Catalin; van Horssen, Merlijn; Guta, Madalin

    2012-11-28

    System identification is closely related to control theory and plays an increasing role in quantum engineering. In the quantum set-up, system identification is usually equated to process tomography, i.e. estimating a channel by probing it repeatedly with different input states. However, for quantum dynamical systems such as quantum Markov processes, it is more natural to consider the estimation based on continuous measurements of the output, with a given input that may be stationary. We address this problem using asymptotic statistics tools, for the specific example of estimating the Rabi frequency of an atom maser. We compute the Fisher information of different measurement processes as well as the quantum Fisher information of the atom maser, and establish the local asymptotic normality of these statistical models. The statistical notions can be expressed in terms of spectral properties of certain deformed Markov generators, and the connection to large deviations is briefly discussed.

  10. Asymptotic inference in system identification for the atom maser

    CERN Document Server

    Catana, Catalin; Guta, Madalin

    2011-01-01

    System identification is an integrant part of control theory and plays an increasing role in quantum engineering. In the quantum set-up, system identification is usually equated to process tomography, i.e. estimating a channel by probing it repeatedly with different input states. However for quantum dynamical systems like quantum Markov processes, it is more natural to consider the estimation based on continuous measurements of the output, with a given input which may be stationary. We address this problem using asymptotic statistics tools, for the specific example of estimating the Rabi frequency of an atom maser. We compute the Fisher information of different measurement processes as well as the quantum Fisher information of the atom maser, and establish the local asymptotic normality of these statistical models. The statistical notions can be expressed in terms of spectral properties of certain deformed Markov generators and the connection to large deviations is briefly discussed.

  11. WARPING AND PRECESSION IN EXTRAGALACTIC MASER ACCRETION DISCS

    Directory of Open Access Journals (Sweden)

    A. Caproni

    2009-01-01

    Full Text Available Interferometric maser observations have been used to probe the physical conditions of extragalactic accretion discs at sub-parsec scales. The inferred kinematic of the water maser spots presents small deviations from Keplerian motions, which have been attributed to the warping and twisting of the parsec-scale disc. However, their physical origin is still a matter of debate in the literature. Motivated by this, we analyzed the general relativistic Bardeen-Petterson e ect, driven by a Kerr black hole, as the potential physical mechanism responsible for the disc warping and precession in the nearby Seyfert 2 galaxies NGC 1068 and NGC 4258. Assuming a power-law accretion disc, whose parameters were constrained by the observational data, we derived the basic quantities concerning the Bardeen-Petterson e ect for both sources. Some consequences from this peculiar relativistic mechanism are also presented in this work.

  12. CEPHEID VARIABLES IN THE MASER-HOST GALAXY NGC 4258

    Energy Technology Data Exchange (ETDEWEB)

    Hoffmann, Samantha L.; Macri, Lucas M., E-mail: lmacri@tamu.edu [George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A and M University, College Station, TX 77843 (United States)

    2015-06-15

    We present results of a ground-based survey for Cepheid variables in NGC 4258. This galaxy plays a key role in the Extragalactic Distance Scale due to its very precise and accurate distance determination via very long baseline interferometry observations of water masers. We imaged two fields within this galaxy using the Gemini North telescope and the Gemini Multi-Object Spectrograph, obtaining 16 epochs of data in the Sloan Digital Sky Survey gri bands over 4 yr. We carried out point-spread function photometry and detected 94 Cepheids with periods between 7 and 127 days, as well as an additional 215 variables which may be Cepheids or Population II pulsators. We used the Cepheid sample to test the absolute calibration of theoretical gri Period–Luminosity relations and found good agreement with the maser distance to this galaxy. The expected data products from the Large Synoptic Survey Telescope should enable Cepheid searches out to at least 10 Mpc.

  13. Cepheid Variables in the Maser-Host Galaxy NGC 4258

    CERN Document Server

    Hoffmann, Samantha L

    2015-01-01

    We present results of a ground-based survey for Cepheid variables in NGC 4258. This galaxy plays a key role in the Extragalactic Distance Scale due to its very precise and accurate distance determination via VLBI observations of water masers. We imaged two fields within this galaxy using the Gemini North telescope and GMOS, obtaining 16 epochs of data in the SDSS gri bands over 4 years. We carried out PSF photometry and detected 94 Cepheids with periods between 7 and 127 days, as well as an additional 215 variables which may be Cepheids or Population II pulsators. We used the Cepheid sample to test the absolute calibration of theoretical gri Period-Luminosity relations and found good agreement with the maser distance to this galaxy. The expected data products from the Large Synoptic Survey Telescope (LSST) should enable Cepheid searches out to at least 10 Mpc.

  14. Quarterly report Ruby Lake Migratory Waterfowl Refuge: August, September, October, 1939

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from August through October of 1939. The report begins by summarizing...

  15. Quarterly report: Ruby Lake Migratory Waterfowl Refuge: November, December, 1939, January, 1940

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from November of 1939 through January of 1940. The report begins by...

  16. Ruby Lake National Wildlife Refuge Quarterly narrative report: November, December, 1941, January, 1942

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from November of 1941 through January of 1942. The report begins by...

  17. [Ruby Lake National Wildlife Refuge Quarterly narrative report: February - April, 1941

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments from February through April of 1941. The report begins by summarizing...

  18. Ruby Lake National Wildlife Refuge: Annual narrative report: Calendar year 1983

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake NWR outlines Refuge accomplishments during the 1983 calendar year. The report begins with a summary of the year's...

  19. Quarterly Report Ruby Lake Migratory Waterfowl Refuge February, March, April, 1940

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1940 quarterly year. The report begins by summarizing...

  20. Quarterly Report Ruby Lake Migratory Waterfowl Refuge August, September, October, 1940

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1940 quarterly year. The report begins by summarizing...

  1. Ruby Lake National Wildlife Refuge update and preliminary water report: January 1 through December 1, 1996

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report includes current elevations, water flow measurements, precipitation and evaporation, water flow highlights, and plans for 1997 for Ruby Lake NWR.

  2. The Trail Inventory of Ruby Lake National Wildlife Refuge [Cycle 1

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — The purpose of this report is to create a baseline inventory of all non-motorized trails on Ruby Lake National Wildlife Refuge. Trails in this inventory are eligible...

  3. In situ pressure calibration for piston cylinder cells via ruby fluorescence with fiber optics.

    Science.gov (United States)

    Koyama-Nakazawa, Kazuko; Koeda, Masahito; Hedo, Masato; Uwatoko, Yoshiya

    2007-06-01

    A fiber-optic measurement technique is developed for estimating the pressure inside a piston cylinder cell up to approximately 4 GPa, based on the pressure-induced R1 fluorescence line shift of ruby (ruby scale). Ruby scale and a conventional technique (calibration on phase transitions of bismuth) were simultaneously applied to the cell filled with a pressure transmitting medium of isopropyl alcohol. The pressure readings of the two methods were consistent with each other, and no pressure gradient was observed. The ruby scale has the advantages of real time estimation and easy installation in a small space. Because of these advantages, three fibers were simultaneously introduced in the sample space at the same time, and pressure distribution was measured for Fluorinert (FC70:FC77=1:1), Daphne oil 7373, and Fomblin oil (YHVAC 13014).

  4. Visuaalantropoloogia - inimlik mõõde asjade maailmas / Jay Ruby ; interv. Peeter Linnap

    Index Scriptorium Estoniae

    Ruby, Jay

    2006-01-01

    Ameerika visuaalkultuuri teoreetik Jay Ruby on paari viimase aastakümne jooksul keskendunud pildilise kommunikatsiooni etnograafilisele käsitlemisele Ameerika maaühiskonnas. Peeter Linnapi intervjuu Jay Rubyga Tartu Kõrgemas Kunstikoolis 23. V

  5. Visuaalantropoloogia - inimlik mõõde asjade maailmas / Jay Ruby ; interv. Peeter Linnap

    Index Scriptorium Estoniae

    Ruby, Jay

    2006-01-01

    Ameerika visuaalkultuuri teoreetik Jay Ruby on paari viimase aastakümne jooksul keskendunud pildilise kommunikatsiooni etnograafilisele käsitlemisele Ameerika maaühiskonnas. Peeter Linnapi intervjuu Jay Rubyga Tartu Kõrgemas Kunstikoolis 23. V

  6. Ruby Lake National Wildlife Refuge Narrative Report January-April, 1945

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake outlines Refuge accomplishments during the 1945 quarterly year. The report begins with a summary of the weather and water...

  7. Quarterly Report Ruby Lake Migratory Waterfowl Refuge August, September, October, 1939

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1939 quarterlyl year. The report begins by summarizing...

  8. Ruby Lake National Wildlife Refuge Annual Narrative Report Calender Year 1977

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1977 calendar year. The report begins with an introduction to...

  9. Ruby Lake National Wildlife Refuge Annual Narrative Report Calender Year 1979

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1979 calendar year. The report begins with an introduction to...

  10. Ruby Lake National Wildlife Refuge Annual Narrative Report Calender Year 1978

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1978 calendar year. The report begins with an introduction to...

  11. Greater Sandhill Crane colt survival on the Ruby Lake National Wildlife Refuge

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This report details Greater Sandhill Crane colt survival at Ruby lake NWR during the time period from 1984 to 2006. Management recommendations are suggested to...

  12. Annual Narrative Report : Calendar Year 1981 : Ruby Lake National Wildlife Refuge

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1981 calendar year. The report begins with a summary...

  13. Annual Narrative Report : Calendar Year 1982 : Ruby Lake National Wildlife Refuge

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1982 calendar year. The report begins with a summary...

  14. Advances in Trace Element "Fingerprinting" of Gem Corundum, Ruby and Sapphire, Mogok Area, Myanmar

    National Research Council Canada - National Science Library

    F Lin Sutherland; Khin Zaw; Sebastien Meffre; Tzen-Fui Yui; Kyaw Thu

    2015-01-01

    ... corundum area and also identified rare alluvial ruby and sapphire grains characterised by unusually high silicon, calcium and gallium, presence of noticeable boron, tin and niobium and very low iron, titanium and magnesium contents...

  15. Ruby Lake National Wildlife Refuge Annual Narrative Report Calender Year 1983

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1983 calendar year. The report begins with a summary...

  16. Ruby Lake National Wildlife Refuge Annual Narrative Report Calender Year 1982

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — This annual narrative report for Ruby Lake National Wildlife Refuge outlines Refuge accomplishments during the 1982 calendar year. The report begins with a summary...

  17. The Water Maser in II Zw 96: Scientific Justification

    Energy Technology Data Exchange (ETDEWEB)

    Wiggins, Brandon Kerry [Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

    2015-08-06

    We propose a VLBI search to image and locate the water emission in II Zw 96. We propose 3 sites within II Zw 96 for VLBI followup (see the proposed target listing below). We request 2.5 hours of on-source integration time with the VLBA per source. The array will achieve ~ 65µJy sensitivity in K band in this time which will be sufficient to detect luminous water maser features.

  18. A CO observation of the galactic methanol masers

    CERN Document Server

    Ren, Zhiyuan; Liu, Tie; Li, Lixin; Li, Di; Ju, Binggang

    2014-01-01

    Context: We investigated the molecular gas associated with 6.7 GHz methanol masers throughout the Galaxy using a J=1-0 transition of the CO isotopologues. Methods:Using the 13.7-meter telescope at the Purple Mountain Observatory (PMO), we have obtained ^{12}CO and ^{13}CO (1-0) lines for 160 methanol masers sources from the first to the third Galactic quadrants. We made efforts to resolve the distance ambiguity by careful comparison with the radio continuum and HI 21 cm observations. Results: First, the maser sources show increased ^{13}CO line widths toward the Galactic center, suggesting that the molecular gas are more turbulent toward the Galactic center. This trend can be noticeably traced by the ^{13}CO line width. Second, the ^{12}CO excitation temperature shows a noticeable correlation with the H_2 column density. A possible explanation consistent with the collapse model is that the higher surface-density gas is more efficient to the stellar heating and/or has a higher formation rate of high-mass stars...

  19. Evolved star water maser cloud size determined by star size

    CERN Document Server

    Richards, A M S; Gray, M D; Lekht, E E; Mendoza-Torres, J E; Murakawa, K; Rudnitskij, G; Yates, J A

    2012-01-01

    Cool, evolved stars undergo copious mass loss but the details of how the matter is returned to the ISM are still under debate. We investigated the structure and evolution of the wind at 5 to 50 stellar radii from Asymptotic Giant Branch and Red Supergiant stars. 22-GHz water masers around seven evolved stars were imaged using MERLIN, at sub-AU resolution. Each source was observed at between 2 and 7 epochs (several stellar periods). We compared our results with long-term Pushchino single dish monitoring. The 22-GHz emission is located in ~spherical, thick, unevenly filled shells. The outflow velocity doubles between the inner and outer shell limits. Water maser clumps could be matched at successive epochs separated by <2 years for AGB stars, or at least 5 years for RSG. This is much shorter than the decades taken for the wind to cross the maser shell, and comparison with spectral monitoring shows that some features fade and reappear. In 5 sources, most of the matched features brighten or dim in concert from...

  20. The 6-GHz Multibeam Maser Survey I. Techniques

    CERN Document Server

    Green, J A; Fuller, G A; Avison, A; Breen, S L; Brooks, K; Burton, M G; Chrysostomou, A; Cox, J; Diamond, P J; Ellingsen, S P; Gray, M D; Hoare, M G; Masheder, M R W; McClure-Griffiths, N M; Pestalozzi, M; Phillips, C; Quinn, L; Thompson, M A; Voronkov, M; Walsh, A; Ward-Thompson, D; Wong-McSweeney, D; Yates, J A; Cohen, R J

    2008-01-01

    A new 7-beam 6-7 GHz receiver has been built to survey the Galaxy and the Magellanic Clouds for newly forming high-mass stars that are pinpointed by strong methanol maser emission at 6668 MHz. The receiver was jointly constructed by Jodrell Bank Observatory (JBO) and the Australia Telescope National Facility (ATNF) and allows simultaneous coverage at 6668 and 6035 MHz. It was successfully commissioned at Parkes in January 2006 and is now being used to conduct the Parkes-Jodrell multibeam maser survey of the Milky Way. This will be the first systematic survey of the entire Galactic plane for masers of not only 6668-MHz methanol, but also 6035-MHz excited-state hydroxyl. The survey is two orders of magnitude faster than most previous systematic surveys and has an rms noise level of ~0.17 Jy.This paper describes the observational strategy, techniques and reduction procedures of the Galactic and Magellanic Cloud surveys, together with deeper, pointed, follow-up observations and complementary observations with oth...

  1. ALMA reveals VYCMa's sub-mm maser and dust distribution

    CERN Document Server

    Richards, A M S; Humphreys, E M; Vlahakis, C; Vlemmings, W; Baudry, A; De Beck, E; Decin, L; Etoka, S; Gray, M D; Harper, G M; Hunter, T R; Kervella, P; Kerschbaum, F; McDonald, I; Melnick, G; Muller, S; Neufeld, D; O'Gorman, E; Parfenov, S Yu; Peck, A B; Shinnaga, H; Sobolev, A M; Testi, L; Uscanga, L; Wootten, A; Yates, J A; Zijlstra, A

    2014-01-01

    Cool, evolved stars have copious, enriched winds. The structure of these winds and the way they are accelerated is not well known. We need to improve our understanding by studying the dynamics from the pulsating stellar surface to about 10 stellar radii, where radiation pressure on dust is fully effective. Some red supergiants have highly asymmetric nebulae, implicating additional forces. We retrieved ALMA Science Verification data providing images of sub-mm line and continuum emission from VY CMa. This enables us to locate water masers with milli-arcsec precision and resolve the dusty continuum. The 658-, 321- and 325-GHz masers lie in irregular, thick shells at increasing distances from the centre of expansion. For the first time this is confirmed as the stellar position, coinciding with a compact peak offset to the NW of the brightest continuum emission. The maser shells (and dust formation zone) overlap but avoid each other on tens-au scales. Their distribution is broadly consistent with excitation models...

  2. Identification of Bursting Water Maser Features in Orion KL

    CERN Document Server

    Hirota, Tomoya; Fujisawa, Kenta; Honma, Mareki; Kawaguchi, Noriyuki; Kim, Mi Kyoung; Kobayashi, Hideyuki; Imai, Hiroshi; Omodaka, Toshihiro; Katsunori,; Shibata, M; Shimoikura, Tomomi; Yonekura, Yoshinori

    2011-01-01

    In February 2011, a burst event of the H$_{2}$O maser in Orion KL (Kleinmann-Low object) has started after 13-year silence. This is the third time to detect such phenomena in Orion KL, followed by those in 1979-1985 and 1998. We have carried out astrometric observations of the bursting H$_{2}$O maser features in Orion KL with VERA (VLBI Exploration of Radio Astrometry), a Japanese VLBI network dedicated for astrometry. The total flux of the bursting feature at the LSR velocity of 7.58 km s$^{-1}$ reaches 4.4$\\times10^{4}$ Jy in March 2011. The intensity of the bursting feature is three orders of magnitudes larger than that of the same velocity feature in the quiescent phase in 2006. Two months later, another new feature appears at the LSR velocity of 6.95 km s$^{-1}$ in May 2011, separated by 12 mas north of the 7.58 km s$^{-1}$ feature. Thus, the current burst occurs at two spatially different features. The bursting masers are elongated along the northwest-southeast direction as reported in the previous burs...

  3. Ruby (Al2O3: Cr3+) Fluorescence Thermometer Using PLD-PMSR Technique

    Institute of Scientific and Technical Information of China (English)

    WU Jin-ling; WANG Yu-tian

    2005-01-01

    A kind of fluorescence fiber-optic thermometer is devised based on the solid-state ruby fluorescence material. The characteristics of fluorescence material absorption and emission are analyzed, and the fiber-optic temperature measurement probe in ruby is developed. This system is particularly adaptable to the temperature measurement in the range of 20 ℃ to 600 ℃. During the experiment, this method is proved to be useful to temperature measurement with high resolution and precision.

  4. Very Large Array Monitoring of 1720 MHz OH Masers toward the Galactic Center

    Science.gov (United States)

    Pihlström, Y. M.; Sjouwerman, L. O.; Mesler, R. A.

    2011-10-01

    We present the first variability study of the 1720 MHz OH masers located in the Galactic center. Most of these masers are associated with the interaction between the supernova remnant Sgr A East and the interstellar medium, but a few masers are associated with the circumnuclear disk (CND). The monitoring program covered five epochs and a timescale of 20-195 days, during which no masers disappeared and no new masers appeared. All masers have previously been detected in a single-epoch observation about one year prior to the start of the monitoring experiment, implying relatively stable conditions for the 1720 MHz OH masers. No extreme variability was detected. The masers associated with the northeastern interaction region between the supernova remnant and the +50 km s-1 molecular cloud show the highest level of variability. This can be explained with the +50 km s-1 molecular cloud being located behind the supernova remnant and with a region of high OH absorbing column density along the line of sight. Possibly, the supernova remnant provides additional turbulence to the gas in this region, through which the maser emission must travel. The masers in the southern interaction region are located on the outermost edge of Sgr A East, the line of sight of which is not covered by either absorbing OH gas or a supernova remnant, in agreement with the much lower variability level observed. Similarly, the masers associated with the CND show little variability, consistent with those arising through collisions between relatively large clumps of gas in the CND and no significant amount of turbulent gas along the line of sight.

  5. Mini-ruby is rapidly taken up by neurons and astrocytes in organotypic brain slices.

    Science.gov (United States)

    Ullrich, Celine; Humpel, Christian

    2011-10-01

    Cholinergic neurons are intensively studied, because they degenerate in Alzheimer's disease. Although neurotracer techniques are widely used to study axonal transport, guidance, regeneration or sprouting it is not clear if cholinergic neurons can be stained by tracer techniques and studied in brain slices. The aim of the present study was to evaluate the characteristics of the neurotracer Mini-ruby in organotypic brain slices of the basal nucleus of Meynert (nBM), focusing on cholinergic neurons. Mini-ruby is a biotinylated dextran amine and is taken up very fast by a variety of cells. When 2-week old nerve growth factor-incubated brain slices of the nBM were treated with Mini-ruby crystals for 1 h, only a few (2-3%) cholinergic neurons were clearly labeled as shown by co-localization with choline acetyltransferase. The staining was found in neuN-positive neurons and microtubule associated protein-2 (MAP-2)-positive nerve fibers. A very rapid dynamic change was observed in these labeled varicosities within seconds. However, Mini-ruby was taken up also by many glutamine synthethase-positive astrocytes. At the site of Mini-ruby application an intense CD11b-positive microglial staining was evident. In conclusion, neurons and astrocytes in organotypic brain slices can be labeled very fast with the fluorescent dye Mini-ruby which undergoes dynamic processes.

  6. Simply rails 2 the ultimate beginner's guide to Ruby on rails

    CERN Document Server

    Lenz, Patrick

    2008-01-01

    Want to learn all about Ruby on Rails 2.0, the web application framework that is inspiring developers around the world? The second edition of this practical, hands on book will: show you how to install Ruby on Rails on Windows, Mac, or Linux walk you, step by step, through the development of a Web 2.0 social news application, just like digg.com show you how to test, debug, benchmark, and deploy your Rails application Unlike other Rails books, this book doesn't assume that you are an experienced web developer, or that you've used Ruby before. An entire chapter is devoted to learning Ruby in a fun way, using the interactive Ruby console, so you can follow along at home. You'll be an accomplished Ruby programmer in no time! The example application that the book builds - a user-generated news web site - is built upon with each following chapter, and concepts such as sessions, cookies and basic AJAX usage are gradually introduced. Different aspects of Rails, such as user authentication, session cookies, and automa...

  7. A Design of Sports Portal Based on Ruby on Rails%基于Ruby on Rails框架的体育门户网站的研究

    Institute of Scientific and Technical Information of China (English)

    周洁

    2008-01-01

    基于Ruby语言构建的全新的Web开发框架Ruby Oil Rails,为Web应用程序开发提供了极其便捷的途径,近年来的迅速兴起成为了Web开发社区的焦点.采用支持敏捷开发的Ruby on Rails框架,研究并设计了一个新型体育门户网站,并重点介绍了网站各模块的主要功能以及实现的关键技术.

  8. Ruby on Rails与Struts+Hibernate架构之比较分析%Compare and Analysis between Ruby on Rails and Struts+Hibernate Frame

    Institute of Scientific and Technical Information of China (English)

    吴吉义

    2007-01-01

    Ruby on Rails是一个基于Ruby语言构建的全新Web应用程序架构,为Web应用程序开发提供了一种极其快捷的途径,正在和已经引起业界相当的兴趣.在给出了Ruby on Rails与轻量级J2EE架构Struts+Hibernate关键特性的基础上,从前端控制器、动作和模型,持久性框架三个方面对两种架构进行了比较.

  9. Physico-Chemical Research on the Sounding Rocket Maser 13

    Science.gov (United States)

    Lockowandt, Christian; Kemi, Stig; Abrahamsson, Mattias; Florin, Gunnar

    MASER is a sounding rocket platform for short-duration microgravity experiments, providing the scientific community with an excellent microgravity tool. The MASER programme has been running by SSC from 1987 and has up to 2012 provided twelve successful flights for microgravity missions with 6-7 minutes of microgravity, the g-level is normally below 1x10-5 g. The MASER 13 is planned to be launched in spring 2015 from Esrange Space Center in Northern Sweden. The rocket will carry four ESA financed experiment modules. The MASER 13 vehicle will be propelled by the 2-stage solid fuel VSB-30 rocket motor, which provided the 390 kg payload with an apogee of 260 km and 6 and a half minutes of microgravity. Swedish Space Corporation carries out the MASER missions for ESA and the program is also available for other customers. The payload comprise four different experiment modules of which three could be defined as physic-chemical research; XRMON-SOL, CDIC-3, MEDI. It also comprises the Maser Service Module and the recovery system. The Service Module provided real-time 5 Mbps down-link of compressed experiment digital video data from the on-board cameras, as well as high-speed housekeeping telemetry data. XRMON-SOL In this experiment the influence of gravity on the formation of an equiaxed microstructure will be investigated. Special attention will be put on the aspect of nucleation, segregation and impingement. The experiment scope is to melt and solidify an AlCu-alloy sample in microgravity. The solidification will be performed in an isothermal environment. The solidification process will be monitored and recorded with X-ray image during the whole flight, images will also be down-linked to ground for real-time monitoring and possible interaction. CDIC-3 The goal is to study in migrogravity the spatio-temporal dynamics of a chemical front travelling in a thin solution layer open to the air and specifically the respective role of Marangoni and density-related hydrodynamic

  10. SiO Maser Survey toward the Inner Galactic Disk 40 < l < 70 and |b| < 10

    CERN Document Server

    Nakashima, J; Nakashima, Jun-ichi; Deguchi, Shuji

    2003-01-01

    We present the results of an SiO maser survey for color-selected IRAS sources in the area 40 < l < 70 and |b| < 10 in the SiO J=1-0, v=1 and 2 transitions. We detected 134 out of 272 observed sources in SiO masers; 127 were new detections. A systematic difference in the detection rates between SiO and OH maser searches was found. Especially, in the color ranges with log(F_{25}/F_{12}) smaller than -0.1, the detection rate of the SiO masers is significantly higher than that of OH masers. We found a possible kinematic influence of the galactic arm on the distribution of SiO maser sources. It was found that the velocity dispersion of SiO maser sources tends to decrease with the galactocentric distance. Using the present and previous data of SiO maser surveys, we found that the local velocity gradient of the rotational velocity of the Galaxy is consistent with the values obtained from other kinds of disk population stars within a statistical uncertainty. The Oort's constants, "A" and "B", were computed f...

  11. Detectability of Circumstellar SiO Maser Emission on VSOP-2 Baselines

    Science.gov (United States)

    Colomer, F.; Bujarrabal, V.; Ruiz, R. S.; Dodson, R.; Alcolea, J.; Desmurs, J.-F.

    2009-08-01

    We have studied compact circumstellar SiO maser emission at 86 GHz with the Global Millimeter VLBI Array (GMVA), which provides the same spatial resolution as the VSOP-2 to ground baselines at 43 GHz. We present preliminary maps of the emission, estimate the flux and size of the maser spots, and discuss their detectability on baselines from VSOP-2 to ground telescopes.

  12. Methanol masers and millimetre lines : a common origin in protostellar envelopes

    NARCIS (Netherlands)

    Torstensson, Karl Johan Erik

    2011-01-01

    In this thesis we study the earliest stages of high-mass star formation. Class II methanol masers are only associated with massive star formation and are a unique probe of these environments. Through observations we have studied where and when the methanol maser emission occur in relation to the pro

  13. Discovery of Two New Class II Methanol Maser Transitions in G345.01+1.79

    CERN Document Server

    Ellingsen, S P; Cragg, D M; Godfrey, P D

    2012-01-01

    We have used the Swedish ESO Submillimetre Telescope (SEST) to search for new class II methanol maser transitions towards the southern source G345.01+1.79. Over a period of 5 days we observed 11 known or predicted class II methanol maser transitions. Emission with the narrow line width and characteristic velocity of class II methanol masers (in this source) was detected in 8 of these transitions, two of which have not previously been reported as masers. The new class II methanol maser transitions are the 13(-3)-12(-4)E transition at 104.1 GHz and the 5(1)-4(2)E transition at 216.9 GHz. Both of these are from transition series for which there are no previous known class II methanol maser transitions. This takes the total number of known class II methanol maser series to 10, and the total number of transitions (or transition groups) to 18. The observed 104.1 GHz maser suggests the presence of two or more regions of masing gas with similar line of sight velocities, but quite different physical conditions. Althou...

  14. Recent results on the peformance of EFOS, NP and NX hydrogen masers

    Science.gov (United States)

    Reinhardt, V.; Ingold, J. S.; Stalder, T.; Saifi, M.; Dachel, P.; Wardrip, S. C.

    1984-01-01

    In response to a NASA Goddard Space Flight Center Work Assignment, Bendix Field Engineering Corporation evaluated the performance of the Oscilloquartz EPOS-2 hydrogen maser along with that of NASA NX-3 and NP-2 hydrogen masers in early 1983. This paper presents the results of that evaluation.

  15. Very Large Array monitoring of 1720 MHz OH masers toward the Galactic Center

    CERN Document Server

    Pihlström, Y M; Mesler, R A

    2011-01-01

    We present the first variability study of the 1720 MHz OH masers located in the Galactic Center. Most of these masers are associated with the interaction between the supernova remnant SgrAEast and the interstellar medium, but a few masers are associated with the Circumnuclear Disk. The monitoring program covered five epochs and a timescale of 20-195 days, during which no masers disappeared and no new masers appeared. All masers have previously been detected in a single epoch observation about one year prior to the start of the monitoring experiment, implying relatively stable conditions for the 1720 MHz OH masers. No extreme variability was detected. The masers associated with the northeastern interaction region between the supernova remnant and the +50km/s molecular cloud show the highest level of variability. This can be explained with the +50km/s molecular cloud being located behind the supernova remnant and with a region of high OH absorbing column density along the line of sight. Possibly the supernova r...

  16. Magnetic fields around evolved stars: further observations of H$_2$O maser polarization

    CERN Document Server

    Leal-Ferreira, M L; Kemball, A; Amiri, N

    2013-01-01

    We aim to detect the magnetic field and infer its properties around four AGB stars using H$_2$O maser observations. The sample we observed consists of the following sources: the semi-regular variable RT Vir and the Mira variables AP Lyn, IK Tau, and IRC+60370. We observed the 6$_{1,6}-5_{2,3}$ H$_2$O maser rotational transition, in full-polarization mode, to determine its linear and circular polarization. Based on the Zeeman effect, one can infer the properties of the magnetic field from the maser polarization analysis. We detected a total of 238 maser features, in three of the four observed sources. No masers were found toward AP Lyn. The observed masers are all located between 2.4 and 53.0 AU from the stars. Linear and circular polarization was found in 18 and 11 maser features, respectively. We more than doubled the number of AGB stars in which magnetic field has been detected from H$_2$O maser polarization, as our results confirm the presence of fields around IK Tau, RT Vir and IRC+60370. The strength of ...

  17. Excited-state hydroxyl maser catalogue from the methanol multibeam survey -- I. Positions and Variability

    CERN Document Server

    Avison, A; Fuller, G A; Caswell, J L; Green, J A; Breen, S L; Ellingsen, S P; Gray, M D; Pestalozzi, M; Thompson, M A; Voronkov, M A

    2016-01-01

    We present the results of the first complete unbaised survey of the Galactic Plane for 6035-MHz excited-state hydroxyl masers undertaken as part of the Methanol Multibeam Survey. These observations cover the Galactic longitude ranges $186^{\\circ}< l < 60^{\\circ}$ including the Galactic Centre. We report the detection of 127 excited-state hydroxyl masers within the survey region, 47 being new sources. The positions of new detections were determined from interferometric observations with the Australia Telescope Compact Array. We discuss the association of 6035-MHz masers in our survey with the 6668-MHz masers from the MMB Survey, finding 37 likely methanol-excited-state hydroxyl masers maser pairs with physical separations of <=0.03pc and 55 pairings separated by <=0.1pc. Using these we calculate for the first time an excited-state hydroxyl maser life time of between 3.3x10^3 and 8.3x10^3 years. We also discuss the variability of the 6035-MHz masers and detection rates of counterpart 6030-MHz excite...

  18. A general catalogue of 6.7GHz methanol masers II: statistical analysis

    CERN Document Server

    Pestalozzi, M R; Collett, J; Minier, V; Conway, J; Booth, R; Pestalozzi, Michele R.

    2006-01-01

    Context: Methanol masers at 6.7GHz are recognised markers of high-mass star formation regions. The study of their distribution in the Galaxy gives important insights into the star formation activity of the Milky Way. We present a statistical analysis on the General Catalogue of 6.7GHz methanol masers in the Galaxy with the aim of extracting global properties of the masers. Aims: We provide constraints on the luminosity function of 6.7GHz methanol masers and on their total number in the Galaxy. Methods: We model the spatial distribution of the masers in the Milky Way by using their distribution in galactocentric distance which is unambiguous once a rotation curve for the Galaxy is assumed. This is the starting point for determining the luminosity function of the masers. Results: The luminosity function of 6.7GHz methanol masers is modelled as a power-law with sharp cutoffs and having an index lying between -1.5 and -2. We also predict the number of detections of methanol masers assuming different sensitivity l...

  19. Spectral Dynamics of a Free-Electron Maser with a Step-Tapered Undulator

    NARCIS (Netherlands)

    Eecen, P. J.; Schep, T. J.; Tulupov, A. V.

    1995-01-01

    The spectral behavior of a high-power, high-gain free-electron maser (FEM) is investigated. The maser has a step-tapered undulator consisting of two sections with different strengths and lengths and equal periodicities. The sections are separated by a field-free gap. The configuration is enclosed

  20. Inward Motions of the Compact SiO Masers Around VX Sagittarii

    CERN Document Server

    Chen, X; Imai, H; Kamohara, R; Chen, Xi; Shen, Zhi-Qiang; Imai, Hiroshi; Kamohara, Ryuichi

    2006-01-01

    We report Very Long Baseline Array (VLBA) observations of 43 GHz v=1, J=1-0 SiO masers in the circumstellar envelope of the M-type semi-regular variable star VX Sgr at 3 epochs during 1999 April-May. These high-resolution VLBA images reveal a persistent ringlike distribution of SiO masers with a projected radius of ~3 stellar radii. The typical angular size of 0.5 mas for individual maser feature was estimated from two-point correlation function analysis for maser spots. We found that the apparent size scale of maser features was distinctly smaller than that observed in the previous observations by comparing their fractions of total power imaged. This change in the size scale of maser emission may be related to stellar activity that caused a large SiO flare during our observations. Our observations confirmed the asymmetric distribution of maser emission, but the overall morphology has changed significantly with the majority of masers clustering to the north-east of the star compared to that lying to the south...

  1. Two-frequency picosecond laser based on composite vanadate crystals with {sigma}-polarised radiation

    Energy Technology Data Exchange (ETDEWEB)

    Sirotkin, A A; Sadovskiy, S P; Garnov, Sergei V [A M Prokhorov General Physics Institute, Russian Academy of Sciences, Moscow (Russian Federation)

    2013-07-31

    A two-frequency picosecond laser based on {alpha}-cut Nd:YVO{sub 4}-YVO{sub 4} composite vanadate crystals is experimentally studied for the s-polarised radiation at the {sup 4}F{sub 3/2} - {sup 4}I{sub 11/2} transition with frequency tuning using Fabry-Perot etalons of different thickness. The difference between the radiation wavelengths was tuned within the range of 1.2-4.4 nm. In the mode-locking regime, the two-frequency radiation power was 280 mW at an absorbed pump power of 12 W. (lasers)

  2. Characterizing supernova remnant and molecular cloud interaction environments using Class I methanol (CH3OH) masers

    Science.gov (United States)

    McEwen, Bridget C.

    Astronomical masers are useful probes of the physical conditions of the gas in which they are formed. Masers form under specific physical conditions and therefore, can be used to trace distinct environments, for example, star forming regions (SFRs), supernova remnants (SNRs), evolved stars, and outflows. In particular, collisionally excited 36 and 44 GHz methanol (CH3OH) and 1720 MHz hydroxl (OH) masers are found associated with gas shocked by the interaction between SNRs and neighboring molecular clouds (MCs). The overall goal of my thesis research is to combine modeling and observations to characterize the properties and formation of Class I CH3OH masers in these SNR/MC interaction regions. Developing a general model of the distribution of maser emission in these regions in all SNRs interacting with MCs will aid in the understanding of different processes that may be triggered through these interactions, namely induced star formation (SF) and cosmic ray (CR) acceleration. More accurate information on the density (and density gradients) in these turbulent regions could, for example, be used as inputs or constraints for models of galactic SNR CR acceleration and help explain if conditions are conducive for SF. In this thesis, I present results from calculations of the physical conditions necessary for the occurrence of collisionally pumped Class I 36, 44, 84, and 95 GHz CH3OH maser lines near SNRs, using an escape probability and level population code. The modeling shows that given a sufficient CH3OH abundance, CH3OH maser emission arises over a wide range of densities and temperatures, with optimal conditions at 10 4 sample of SNRs with previous and recent CH 3OH maser detections (G1.4-0.1, W28, Sgr A East, G5.7-0.0, W44, and W51C). I also discuss how detections of CH3OH masers can be used along with other maser tracers, i.e. H2O masers, to pinpoint sights of SF near SNRs. Furthermore, I will discuss the close spatial and kinematic correlation of CH3OH masers in

  3. Time Variation of SiO Masers in VX Sagittarii over an Optically Quiescent Phase

    Science.gov (United States)

    Kamohara, Ryuichi; Deguchi, Shuji; Miyoshi, Makoto; Shen, Zhi-Qiang

    2005-04-01

    The time variation of SiO masers in a semi-regular variable, VX Sgr, was investigated in the period between 1994 and 2004 when the optical light curve exhibited an ˜6-yr quiescent phase intercepting a regularly pulsating era. The quiescent period occurred with a delay of several years after a decrease in the SiO maser flux. VLBA observations of SiO masers made during this period showed no drastic spatial variation except for emission features being shifted from south-west to north-east. The SiO maser flux decrease, and a succeeding optical quiescent phase, may indicate that the stellar mass-loss rate diminished over a few years around 1994. A SiO maser flare occurring in 1999 may be a reminiscence of a final gas blow, which resulted in the optically quiescent period.

  4. A Survey and Statistics of Interstellar OH and H2O Masers

    Institute of Scientific and Technical Information of China (English)

    Han-Ping Liu; J. R. Forster; Jin Sun

    2005-01-01

    We present a statistical analysis of a sky survey of interstellar H2O and OH masers. These masers can be classified into three categories: isolated H2O masers, isolated OH masers, and simple OH/H2O maser associations. The total number of sources in each category is of the same order of magnitude, and as an evolutionary phase they can maintain ~ 105 yr. An improved radiative pumping mechanism is proposed. This model avoids some of the deficiencies of previous radiative models, such as shortage of exciting photons. The statistical results obtained from the survey can be interpreted by the new mechanism together with the evolutionary model in which the gravitational force of the central stellar objects is responsible for the HII region.

  5. Excited-state hydroxyl maser polarimetry: Who ate all the {\\pi}s?

    CERN Document Server

    Green, James A; McClure-Griffiths, Naomi M

    2015-01-01

    We present polarimetric maser observations with the Australia Telescope Compact Array (ATCA) of excited-state hydroxyl (OH) masers. We observed 30 fields of OH masers in full Stokes polarization with the Compact Array Broadband Backend (CABB) at both the 6030 and 6035 MHz excited-state OH transitions, and the 6668-MHz methanol maser transition, detecting 70 sites of maser emission. Amongst the OH we found 112 Zeeman pairs, of which 18 exhibited candidate {\\pi} components. This is the largest single full polarimetric study of multiple sites of star formation for these frequencies, and the rate of 16% {\\pi} components clearly indicates the {\\pi} component exists, and is comparable to the percentage recently found for ground-state transitions. This significant percentage of {\\pi} components, with consistent proportions at both ground- and excited-state transitions, argues against Faraday rotation suppressing the {\\pi} component emission. Our simultaneous observations of methanol found the expected low level of p...

  6. A note on the periodic methanol masers in G9.62+0.20E

    CERN Document Server

    van der Walt, DJ; Etoka, S; Goedhart, S; Heever, SP van den

    2016-01-01

    A number of mechanisms to understand the periodic class II methanol masers associated with some high-mass star forming regions have been proposed in the past. Two recent proposals, ie. by Parfenov &Sobolev (2014) and Sanna et al. (2015) were presented to explicitly explain the periodic masers in sources with light curves similar to the methanol masers in G9.62+0.20E. We evaluate to what extent the proposals and models presented by these authors can explain the light curve of the methanol masers in G9.62+0.20E. It is argued that neither of the proposed mechanisms can reproduce the light curves of the methanol masers in G9.62+0.20E.

  7. Zeeman Effect observations toward 36 GHz methanol masers in the Galactic Center

    Science.gov (United States)

    Potvin, Justin A.; Momjian, Emmanuel; Pratim Sarma, Anuj

    2017-01-01

    We present observations of 36 GHz Class I methanol masers taken with the Karl G. Jansky Very Large Array (VLA) in the B configuration with the aim of detecting the Zeeman Effect. We targeted several 36 GHz Class I methanol masers associated with supernova remnants (SNRs) toward the Galactic Center. Each source was observed in dual circular polarizations for three hours. The observed spectral profiles of the masers are complex, with several components blended in velocity. In only one case was the Stokes V maser profile prominent enough to reveal a 2-sigma hint of a magnetic field of zBlos = 14.56 +/- 5.60 Hz; we have chosen to express our results in terms of zBlos since the Zeeman splitting factor (z) for 36 GHz methanol masers has not been measured. There are several hints that these spectra would reveal significant magnetic fields if they could be spatially and spectrally resolved.

  8. The 6-GHz methanol multibeam maser catalogue II: Galactic longitudes 6 to 20

    CERN Document Server

    Green, J A; Fuller, G A; Avison, A; Breen, S L; Ellingsen, S P; Gray, M D; Pestalozzi, M R; Quinn, L; Thompson, M A; Voronkov, M A

    2010-01-01

    We present the second portion of an unbiased survey of the Galactic plane for 6668-MHz methanol masers. This section of the survey spans the longitude range 6 degrees to 20 degrees. We report the detection of 119 maser sources, of which 42 are new discoveries. The masers are tightly constrained to the Galactic plane, with only four outside a latitude range of +/- 1 degree. This longitude region includes the brightest known 6668-MHz methanol maser, 9.621+0.196, as well as the two brightest newly discovered sources in the southern survey as a whole. We list all the sources associated with the 3-kpc arms within +/- 15 degrees longitude and consider further candidates beyond 15 degrees longitude. We identify three new sources associated with the Galactic bar and comment on the density of masers in relation to the bar orientation.

  9. Methanol masers as tools to study high-mass star formation

    CERN Document Server

    Pestalozzi, Michele

    2007-01-01

    In this contribution I will attempt to show that the study of galactic 6.7 and 12.2GHz methanol masers themselves, as opposed to the use of methanol masers as signposts, can yield important conclusions contributing to the understanding of high-mass star formation. Due to their exclusive association with star formation, methanol masers are the best tools to do this, and their large number allows to probe the entire Galaxy. In particular I will focus on the determination of the luminosity function of methanol masers and on the determination of an unambiguous signature for a circumstellar masing disc seen edge-on. Finally I will try to point out some future fields of research in the study of methanol masers.

  10. New SIO Masers in Star Forming Regions W:51 IRS:2 and SAGITTARIUS-B2 MD:5

    Science.gov (United States)

    Hasegawa, T.; Morita, K.; Okumura, S.; Kaifu, N.; Suzuki, H.; Ohishi, M.; Hayashi, M.; Ukita, N.

    The maser emission of the 43 GHz SiO J = 1-0 transitions in two regions of active star formation, W51 IRS2 and Sgr B2 MD5, have been detected using the 45 m telescope at Nobeyama. The SiO masers coincide in position with strong H2O masers in each region within a positional uncertainty of 5arcsec. If the masers radiate isotropically, the power radiated from W51 IRS2 and Sgr B2 MD5 in the masing 43 GHz SiO lines are comparable to that from the maser in Orion-KL.

  11. Investigation of two-frequency Nd{sup 3+} : YAG laser

    Energy Technology Data Exchange (ETDEWEB)

    Arapov, Yu D; Ivanov, A F; Kas' yanov, I V; Magda, L E [E.I. Zababakhin All-Russian Scientific-Research Institute of Technical Physics, Russian Federal Nuclear Centre, Snezhinsk, Chelyabinsk region (Russian Federation)

    2013-02-28

    A repetitively pulsed two-frequency laser is developed. Pulsed operation of a laser based on a Nd{sup 3+} : YAG crystal with simultaneous amplification of radiation at two wavelengths in a single-pass amplifier is studied. (laser optics 2012)

  12. G10.472+0.027: An Extreme water maser outflow associated with a Massive Protostellar Cluster

    CERN Document Server

    Titmarsh, A M; Breen, S L; Caswell, J L; Voronkov, M A

    2013-01-01

    An Australia Telescope Compact Array search for 22 GHz water masers towards 6.7 GHz class II methanol masers detected in the Methanol Multibeam (MMB) survey has resulted in the detection of extremely high velocity emission from one of the sources. The water maser emission associated with this young stellar object covers a velocity span of nearly 300 km/s. The highest velocity water maser emission is red-shifted from the systemic velocity by 250 km/s, which is a new record for high-mass star formation regions. The maser is associated with a very young late O, or early B star, which may still be actively accreting matter (and driving the extreme outflow). If that is the case future observations of the kinematics of this water maser will provide a unique probe of accretion processes in the highest mass young stellar objects and test models of water maser formation.

  13. G 10.472+0.027: AN EXTREME WATER MASER OUTFLOW ASSOCIATED WITH A MASSIVE PROTOSTELLAR CLUSTER

    Energy Technology Data Exchange (ETDEWEB)

    Titmarsh, A. M.; Ellingsen, S. P. [School of Mathematics and Physics, University of Tasmania, Hobart, Tasmania (Australia); Breen, S. L.; Caswell, J. L.; Voronkov, M. A. [CSIRO Astronomy and Space Science, Australia Telescope National Facility, P.O. Box 76 Epping, NSW 1710 (Australia)

    2013-09-20

    An Australia Telescope Compact Array search for 22 GHz water masers toward 6.7 GHz class II methanol masers detected in the Methanol Multibeam survey has resulted in the detection of extremely high-velocity emission from one of the sources. The water maser emission associated with this young stellar object covers a velocity span of nearly 300 km s{sup –1}. The highest velocity water maser emission is redshifted from the systemic velocity by 250 km s{sup –1}, which is a new record for high-mass star formation regions. The maser is associated with a very young late O, or early B star, which may still be actively accreting matter (and driving the extreme outflow). If that is the case, future observations of the kinematics of this water maser will provide a unique probe of accretion processes in the highest mass young stellar objects and test models of water maser formation.

  14. A WATER MASER AND NH{sub 3} SURVEY OF GLIMPSE EXTENDED GREEN OBJECTS

    Energy Technology Data Exchange (ETDEWEB)

    Cyganowski, C. J. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Koda, J.; Towers, S.; Meyer, J. Donovan [Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794 (United States); Rosolowsky, E. [Department of Physics and Astronomy, University of British Columbia, Okanagan, Kelowna BC V1V 1V7 (Canada); Egusa, F. [Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Chuo-ku, Sagamihara, Kanagawa 252-5210 (Japan); Momose, R. [Department of Astronomy, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan); Robitaille, T. P., E-mail: ccyganowski@cfa.harvard.edu [Max Planck Institute for Astronomy, Heidelberg (Germany)

    2013-02-10

    We present the results of a Nobeyama 45 m H{sub 2}O maser and NH{sub 3} survey of all 94 northern GLIMPSE extended green objects (EGOs), a sample of massive young stellar objects (MYSOs) identified based on their extended 4.5 {mu}m emission. We observed the NH{sub 3}(1,1), (2,2), and (3,3) inversion lines, and detected emission toward 97%, 63%, and 46% of our sample, respectively (median rms {approx} 50 mK). The H{sub 2}O maser detection rate is 68% (median rms {approx} 0.11 Jy). The derived H{sub 2}O maser and clump-scale gas properties are consistent with the identification of EGOs as young MYSOs. To explore the degree of variation among EGOs, we analyze subsamples defined based on mid-infrared (MIR) properties or maser associations. H{sub 2}O masers and warm dense gas, as indicated by emission in the higher-excitation NH{sub 3} transitions, are most frequently detected toward EGOs also associated with both Class I and II CH{sub 3}OH masers. Ninety-five percent (81%) of such EGOs are detected in H{sub 2}O (NH{sub 3}(3,3)), compared to only 33% (7%) of EGOs without either CH{sub 3}OH maser type. As populations, EGOs associated with Class I and/or II CH{sub 3}OH masers have significantly higher NH{sub 3} line widths, column densities, and kinetic temperatures than EGOs undetected in CH{sub 3}OH maser surveys. However, we find no evidence for statistically significant differences in H{sub 2}O maser properties (such as maser luminosity) among any EGO subsamples. Combining our data with the 1.1 mm continuum Bolocam Galactic Plane Survey, we find no correlation between isotropic H{sub 2}O maser luminosity and clump number density. H{sub 2}O maser luminosity is weakly correlated with clump (gas) temperature and clump mass.

  15. Kinetic analysis of two dimensional metallic grating Cerenkov maser

    Energy Technology Data Exchange (ETDEWEB)

    Zhao Ding [Key Laboratory of High Power Microwave Sources and Technologies, Institute of Electronics, Chinese Academy of Sciences, Beijing 100190 (China)

    2011-08-15

    The dispersion relation of two dimensional metallic grating Cerenkov maser has been given by using kinetic analysis, in which the influence of electron movement is directly considered without using an equivalent dielectric medium assumption. The effects of structural parameters and beam state on the interaction gain and synchronous frequency have also been investigated in detail by numerical calculations. To an illustrative case, the quantitative relations produced from varying the gap distance between electron beam and metallic grating, beam current, electron transverse to axial velocity ratio, and electron axial velocity spread have been obtained. The developed method can be used to predict the real interaction system performances.

  16. Water Masers in W49 North and Sagittarius B2

    OpenAIRE

    McGrath, E. J.; Goss, W. M.; De Pree, C. G.

    2004-01-01

    Using the Very Large Array (VLA) of the National Radio Astronomy Observatory in the A and B configurations, we have obtained simultaneous high resolution observations of both the 22 GHz water maser lines as well as the 22 GHz continuum for the H II regions W49N and Sagittarius B2. The angular resolution of both observations is ~0.1", which at the distance of W49N (11.4 kpc; Gwinn, Moran, & Reid 1992) and Sgr B2 (8.5 kpc) corresponds to a physical size of

  17. Rapid middle Miocene extension and unroofing of the southern Ruby Mountains, Nevada

    Science.gov (United States)

    Colgan, Joseph P.; Howard, Keith A.; Fleck, Robert J.; Wooden, Joseph L.

    2010-01-01

    Paleozoic rocks in the northern Ruby Mountains were metamorphosed during Mesozoic crustal shortening and Cenozoic magmatism, but equivalent strata in the southern Ruby Mountains were never buried deeper than stratigraphic depths prior to exhumation in the footwall of a west dipping brittle normal fault. In the southern Ruby Mountains, Miocene sedimentary rocks in the hanging wall of this fault date from 15.2 to 11.6 Ma and contain abundant detritus from the Paleozoic section. Apatite fission track and (U-Th)/He samples of the Eocene Harrison Pass pluton record rapid cooling that peaked ca. 17–15 Ma, while apatite fission track data from Jurassic plutons east and west of the southern Ruby Mountains indicate near-surface temperatures (pluton to be partially reset rather than to directly record fault slip. Our new data, together with published data on the distribution and composition of Miocene basin fill, suggest that rapid middle Miocene slip took place on the west dipping brittle detachment that bounds the Ruby Mountains and East Humboldt Range for 150 km along strike. This fault was thus active during a period of rapid extension (ca. 17–15 to 12–10 Ma) documented widely across the northern Basin and Range Province.

  18. Water and Methanol Maser Survey of Protostars in the Orion Molecular Cloud Complex

    CERN Document Server

    Kang, Miju; Choi, Minho; Choi, Yunhee; Kim, Kee-Tae; Di Francesco, James; Park, Yong-Sun

    2013-01-01

    The results of a maser survey toward ninety-nine protostars in the Orion molecular cloud complex are presented. The target sources are low-mass protostars identified from infrared observations. Single-dish observations were carried out in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz. Most of the detected sources were mapped to determine the source positions. Five water maser sources were detected, and they are excited by HH 1-2 VLA 3, HH 1-2 VLA 1, L1641N MM1/3, NGC 2071 IRS 1/3, and an object in the OMC 3 region. The water masers showed significant variability in intensity and velocity with time scales of a month or shorter. Four methanol emission sources were detected, and those in the OMC 2 FIR 3/4 and L1641N MM1/3 regions are probably masers. The methanol emission from the other two sources in the NGC 2071 IRS 1-3 and V380 Ori NE regions are probably thermal. For the water masers, the number of detections per protostar in the survey region is about 2%, which s...

  19. Formation and evolution of the water maser outflow event in AFGL 2591 VLA 3-N

    CERN Document Server

    Trinidad, M A; Estalella, R; Cantó, J; Raga, A; Torrelles, J M; Patel, N A; Gómez, J F; Anglada, G; Carrasco-González, C; Rodríguez, L F

    2012-01-01

    In this paper we analyze multi-epoch Very Long Baseline Interferometry (VLBI) water maser observations carried out with the Very Long Baseline Array (VLBA) toward the high-mass star-forming region AFGL 2591. We detected maser emission associated with the radio continuum sources VLA 2 and VLA 3. In addition, a water maser cluster, VLA 3-N, was detected ~ 0.5" north of VLA 3. We concentrate the discussion of this paper on the spatio-kinematical distribution of the water masers towards VLA 3-N. The water maser emission toward the region VLA 3-N shows two bow shock-like structures, Northern and Southern, separated from each other by ~ 100 mas (~ 330 AU). The spatial distribution and kinematics of the water masers in this cluster have persisted over a time span of seven years. The Northern bow shock has a somewhat irregular morphology, while the Southern one has a remarkably smooth morphology. We measured the proper motions of 33 water maser features, which have an average proper motion velocity of ~ 1.3 mas/yr (~...

  20. A CATALOG OF METHANOL MASERS IN MASSIVE STAR-FORMING REGIONS. III. THE MOLECULAR OUTFLOW SAMPLE

    Energy Technology Data Exchange (ETDEWEB)

    Gómez-Ruiz, A. I. [Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis E. Erro 1, Tonantzintla, Puebla, C.P. 72840, México (Mexico); Kurtz, S. E.; Loinard, L. [Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apartado Postal 3-72, Morelia 58089, México (Mexico); Araya, E. D. [Physics Department, Western Illinois University, 1 University Circle, Macomb, IL 61455 (United States); Hofner, P. [New Mexico Institute of Mining and Technology, Socorro, NM 87801 (United States)

    2016-02-15

    We present an interferometric survey of the 44 GHz class I methanol maser transition toward a sample of 69 sources consisting of high-mass protostellar object (HMPO) candidates and ultracompact (UC) H ii regions. We found a 38% detection rate (16 of 42) in the HMPO candidates and a 54% detection rate (13 of 24) for the regions with ionized gas. This result indicates that class I methanol maser emission is more common toward the more evolved young stellar objects of our sample. Comparing with similar interferometric data sets, our observations show narrower linewidths, likely due to our higher spatial resolution. Based on a comparison between molecular outflow tracers and the maser positions, we find several cases where the masers appear to be located at the outflow interface with the surrounding core. Unlike previous surveys, we also find several cases where the masers appear to be located close to the base of the molecular outflow, although we cannot discard projection effects. This and other surveys of class I methanol masers not only suggest that these masers may trace shocks at different stages, but also that they may even trace shocks arising from a number of different phenomena occurring in star-forming regions: young/old outflows, cloud–cloud collisions, expanding H ii regions, among others.

  1. First detection of 22 GHz H2O masers in TX Camelopardalis

    CERN Document Server

    Cho, Se-Hyung; Yun, Youngjoo

    2014-01-01

    Simultaneous time monitoring observations of H$_{2}$O $6_{16}-5_{23}$, SiO $J$ = 1--0, 2--1, 3--2, and $^{29}$SiO $v$ = 0, $J$ = 1--0 lines were carried out in the direction of the Mira variable star TX Cam with the Korean VLBI Network single dish radio telescopes. For the first time, the H$_{2}$O maser emission from TX Cam was detected near the stellar velocity at five epochs from April 10, 2013 ($\\phi$ = 3.13) to June 4, 2014 ($\\phi$ = 3.89) including minimum optical phases. The intensities of H$_{2}$O masers are very weak compared to SiO masers. The variation of peak antenna temperature ratios among SiO $v$ = 1, $J$ = 1--0, $J$ = 2--1, and $J$ = 3--2 masers is investigated according to their phases. The shift of peak velocities of H$_{2}$O and SiO masers with respect to the stellar velocity is also investigated according to observed optical phases. The H$_{2}$O maser emission occurs around the stellar velocity during our monitoring interval. On the other hand, the peak velocities of SiO masers show a sprea...

  2. 44 GHz Class I Methanol (CH$_{3}$OH) Maser Survey in the Galactic Center

    CERN Document Server

    McEwen, Bridget; Sjouwerman, Loránt

    2016-01-01

    We report on a large 44 GHz ($7_0-6_1$ A$^+$) methanol (CH$_3$OH) maser survey of the Galactic Center (GC). The Karl G. Jansky Very Large Array was used to search for CH$_3$OH maser emission covering a large fraction of the region around Sgr A. In 25 pointings, over 300 CH$_3$OH maser sources ($>10\\sigma$) were detected. The majority of the maser sources have a single peak emission spectrum with line of sight velocities that range from about $-$13 km\\,s$^{-1}$ to 72 km\\,s$^{-1}$. Most maser sources were found to have velocities around 35$-$55 km\\,s$^{-1}$, closely following velocities of neighboring interacting molecular clouds. The full width half maximum of each individual spectral feature is very narrow ($\\sim$0.85 km\\,s$^{-1}$ on average). In the north, where Sgr A East is known to be interacting with the 50 km\\,s$^{-1}$ molecular cloud, more than 100 44 GHz CH$_3$OH masers were detected. In addition, three other distinct concentrations of masers were found, which appear to be located closer to the interi...

  3. On the Relationship of UC H II Regions and Class II Methanol Masers: I. Source Catalogs

    CERN Document Server

    Hu, Bo; Wu, Yuanwei; Bartkiewicz, Anna; Rygl, Kazi; Reid, Mark J; Urquhart, James S; Zheng, Xingwu

    2016-01-01

    We conducted VLA C-configuration observations to measure positions and luminosities of Galactic Class II 6.7 GHz methanol masers and their associated ultra-compact H II regions. The spectral resolution was 3.90625 kHz and the continuum sensitivity reached 45 \\uJypb. We mapped 372 methanol masers with peak flux densities of more than 2 Jy selected from the literature, 367 of them were detected. Absolute positions have nominal uncertainties of 0.3 arcsec. In this first paper on the data analysis, we present three catalogs, the first gives information on the strongest feature of 367 methanol maser sources, and the second on all detected maser spots. The third catalog present derived data of the 279 radio continuum sources found in the vicinity of maser sources. Among them, 140 show evidence of physical association with maser sources. Our catalogs list properties including distance, flux density, radial velocity and the distribution of masers on the Galactic plane is then provided as well. We found no significant...

  4. Methanol masers Reliable tracers of the early stages of high-mass star formation

    CERN Document Server

    Ellingsen, S P

    2006-01-01

    The GLIMPSE and MSX surveys have been used to examine the mid-infrared properties of a statistically complete sample of 6.7 GHz methanol masers. The GLIMPSE point sources associated with methanol masers are clearly distinguished from the majority, typically having extremely red mid-infrared colors, similar to those expected of low-mass class 0 young stellar objects. The intensity of the GLIMPSE sources associated with methanol masers is typically 4 magnitudes brighter at 8.0 micron than at 3.6 micron. Targeted searches towards GLIMPSE point sources with [3.6]-[4.5] > 1.3 and an 8.0 micron magnitude less than 10 will detect more than 80% of class II methanol masers. Many of the methanol masers are associated with sources within infrared dark clouds (IRDC) which are believed to mark regions where high-mass star formation is in its very early stages. The presence of class II methanol masers in a significant fraction of IRDC suggests that high-mass star formation is common in these regions. Different maser specie...

  5. Accelerating a water maser face-on jet from a high mass young stellar object

    Science.gov (United States)

    Motogi, Kazuhito; Sorai, Kazuo; Honma, Mareki; Hirota, Tomoya; Hachisuka, Kazuya; Niinuma, Kotaro; Sugiyama, Koichiro; Yonekura, Yoshinori; Fujisawa, Kenta

    2016-10-01

    We report on long-term single-dish and VLBI monitoring for intermittent flare activities of a dominant blue-shifted H2O maser associated with a southern high mass young stellar object, G353.273+0.641. Bi-weekly single-dish monitoring using the Hokkaido University Tomakomai 11 m radio telescope has shown that a systematic acceleration continues over four years beyond the lifetime of individual maser features. This fact suggests that the H2O maser traces a region where molecular gas is steadily accelerated. There were five maser flares during the five years of monitoring, and maser distributions in four of them were densely monitored by VLBI Exploration of Radio Astrometry (VERA). The overall distribution of the maser features suggests the presence of a bipolar jet, with the 3D kinematics indicating that it is almost face-on (inclination angle of ˜ 8°-17° from the line of sight). Most maser features were recurrently excited within a region of 100×100 au2 around the radio continuum peak, while their spatial distributions significantly varied between each flare. This confirms that episodic propagations of outflow shocks recurrently invoke intermittent flare activities. We also measured annual parallax, deriving a source distance of 1.70^{+0.19}_{-0.16} kpc that is consistent with the commonly used photometric distance.

  6. Accelerating an Water Maser Face-on Jet from a High Mass Young Stellar Object

    CERN Document Server

    Motogi, Kazuhito; Honma, Mareki; Hirota, Tomoya; Hachisuka, Kazuya; Niinuma, Kotaro; Sugiyama, Koichiro; Yonekura, Yosinori; Fujisawa, Kenta

    2015-01-01

    We report on a long-term single-dish and VLBI monitoring for intermittent flare activities of a Dominant Blue-Shifted H$_{2}$O Maser (DBSM) associated with a southern high mass young stellar object, G353.273+0.641. Bi-weekly single-dish monitoring using Hokkaido University Tomakomai 11-m radio telescope has shown that a systematic acceleration continues over four years beyond a lifetime of individual maser features. This fact suggests that the H$_{2}$O maser traces a region where molecular gas is steadily accelerated. There were five maser flares during five-years monitoring, and maser distributions in four of them were densely monitored by the VLBI Exploration of Radio Astrometry (VERA). The overall distribution of the maser features suggests the presence of a bipolar jet, with the 3D kinematics indicating that it is almost face-on (inclination angle of $\\sim$ 8$^{\\fdg}$--17$^{\\fdg}$ from the line-of-sight). Most of maser features were recurrently excited within a region of 100$\\times$100 AU$^{2}$ around the...

  7. First description of the male and additional data on the female morphology of Aprostocetus rubi Graham (Hymenoptera: Chalcidoidea: Eulophidae).

    Science.gov (United States)

    Jałoszyński, Paweł

    2016-07-01

    The previously unknown male of Aprostocetus rubi Graham (Eulophidae: Tetrastichinae) was reared, together with females, from galls of the raspberry gall midge Lasioptera rubi (Schrank) (Diptera: Cecidomyiidae) collected in Central Poland. The male is described and illustrated for the first time, and additional information provided on the morphology of the female.

  8. Cathodoluminescence Phenomena of Treated Rubies%优化处理红宝石的阴极发光特征

    Institute of Scientific and Technical Information of China (English)

    李敬敬

    2012-01-01

    使用阴极发光仪对热处理红宝石、染色处理红宝石、充填处理红宝石样品进行发光现象观察,并与天然红宝石、合成红宝石的阴极发光现象对比,得知优化红宝石的阴极发光现象与天然红宝石相近,而处理红宝石的发光强度比天然红宝石及合成红宝石要弱,但处理特征在阴极发光仪下清晰可见.%In this paper,experiments were made on series of rubies with the help of cathodoluminescence instrument;and luminous phenomena of heat-treated ruby,dyed ruby ,and filling processing ruby samples were discussed. Conclusions are drawn that luminous phenomenon of enhancing rubies is similar to that of natural rubies, yet luminous intensity of treated rubies is poorer than that of natural and synthetic rubies.

  9. Hemangioma rubi: doença ou simples achado?

    Directory of Open Access Journals (Sweden)

    Silva, Marcelo Campos Appel

    2006-01-01

    Full Text Available Objetivos: Realizar revisão da literatura sobre os hemangiomas rubi (HR e verificar qual seu significado clínico. Fonte de dados: Revisão da literatura nacional e internacional, através de pesquisa de livros de referência e artigos indexados no Medline, Scielo e LILACS. Síntese dos dados: Os HR têm elevada prevalência na população adulta, sendo a principal dermatose em idosos. Apresentam-se como pápulas esféricas, de cor vermelho brilhante ou violáceas, não-compressíveis à vitropressão, medindo cerca de 1-5 mm, assintomáticas, de distribuição variada no corpo, sendo encontradas mais freqüentemente no tronco. Ao exame histopatológico apresentam-se como proliferações vasculares, na derme, sob epiderme normal. A etiologia ainda não está completamente esclarecida. Embora usualmente benignos, seu achado pode sugerir associação com doenças sistêmicas. Conclusões: Os HR são dermatoses bastante freqüentes na população adulta, sendo queixa comum em consultas em ambulatório de dermatologia. Seu surgimento costuma ser imperceptível, pois se localiza em locais de difícil visualização, como dorso ou couro cabeludo. A observação das lesões é importante e, em caso de aumento do número, tamanho ou distribuição, é aconselhável procurar um dermatologista para revisão.

  10. Two frequency ICRF heating of D-T plasmas on TFTR

    Energy Technology Data Exchange (ETDEWEB)

    Rogers, J.H.; Majeski, R.; Wilson, J.R.; Hosea, J.C.; Schilling, G.; Stevens, J. [Princeton Univ., NJ (United States). Plasma Physics Lab.; Ho, Y.L. [Science Applications International Corp., San Diego, CA (United States); Raman, S. [Michigan Univ., Ann Arbor, MI (United States); Rasmussen, D.A. [Oak Ridge National Lab., TN (United States)

    1993-11-01

    Modifications have been made to allow two of the ICRF antennas (bays L and M) on TFTR to operate at either of two frequencies, 43 MHz or 64 MHz. This was accomplished by lengthening the resonant loops feeding the antennas (2{lambda} at 43 MHz, 3{lambda} at 64 MHz) and replacing the conventional quarter wave impedance transformers with a tapered impedance design. The other two antennas (bays K and N) will operate at a fixed frequency, 43 MHz. The two frequency operation allows a combination of {sup 3}He-minority (or T second harmonic) and H-minority heating at full toroidal field on TFIR. Multiple frequency operation may also be useful in direct electron heating and current drive experiments. Other modifications have been made which are expected to permit arbitrary phasing between the current straps on bays M and L. The system design of the antenna, resonant loops and impedance matching system as well as preliminary TFTR results are discussed.

  11. The effect of ruby laser light on cellular proliferation of epidermal cells.

    Science.gov (United States)

    Liew, S H; Grobbelaar, A O; Gault, D T; Green, C J; Linge, C

    1999-11-01

    In ruby laser-assisted hair removal, microscopic damage is often seen in the basal epidermal cells, where melanosomes are concentrated. It is not known whether this treatment leads to cellular hyperproliferation. It was the aim of this study to investigate this. Ten white patients were treated with the Chromos 694-nm Depilation Ruby Laser, and biopsies taken before and after treatments to assess the presence of cell hyperproliferation, which normally accompanies epidermal damage, with immunohistochemical staining of keratin 16 and Ki67. No evidence of cell hyperproliferation was seen in all specimens examined after ruby laser irradiation. The authors conclude that despite the possible microscopic damages seen in the basal epidermis after laser hair removal, there is no evidence of cellular hyperproliferation. This is in contrast to ultraviolet-irradiated cell damage, in which increased basal cell turnover is seen.

  12. Simplified nonlinear theory of the dielectric loaded rectangular Cerenkov maser

    Institute of Scientific and Technical Information of China (English)

    Zhao Ding; Ding Yao-Gen

    2012-01-01

    To rapidly and accurately investigate the performance of the dielectric loaded rectangular Cerenkov maser,a simplified nonlinear theory is proposed,in which the variations of wave amplitude and wave phase are determined by two coupled first-order differential equations.Through combining with the relativistic equation of motion and adopting the forward wave assumption,the evolutions of the forward wave power,the power growth rate,the axial wave number,the accumulated phase offset,and the information of the particle movement can be obtained in a single-pass calculation.For an illustrative example,this method is used to study the influences of the beam current,the gap distance between the beam and the dielectric surface,and the momentum spread on the forward wave.The variations of the saturated power and the saturation length with the working frequency for the beams with different momentum spreads have also been studied.The result shows that the beam-wave interaction is very sensitive to the electron beam state.To further verify this simplified theory,a comparison with the result produced from a rigorous method is also provided,we find that the evolution curves of the forward wave power predicted by the two methods exhibit excellent agreement.In practical applications,the developed theory can be used for the design and analysis of the rectangular Cerenkov maser.

  13. H2CO Observations Towards CH3OH Maser Sources

    Science.gov (United States)

    Okoh, Daniel; Esimbek, Jarken; Zhou, JianJun; Tang, Xindi; Chukwude, Augustine; Urama, Johnson; Okeke, Pius

    2013-03-01

    Formaldehyde (H2CO) is an accurate probe of physical conditions in dense and low-temperature molecular clouds towards massive star formation regions, while 6.7 GHz methanol (CH3OH) masers provide ideal sites to probe the earliest stages of massive stellar formation. We present preliminary results of our investigation into the possible relationship between formaldehyde and methanol astrophysical masers with the view to expanding knowledge on massive star formation processes. Observations are done using the Nanshan 25m radio telescope of the Xinjiang Astronomical Observatories, Urumqi, China. 127 Methanol sources (from the work of Green et al. 2010, Xu et al. 2003, Pestalozzi et al. 2005, and Xu et al. 2009) have been observed so far for 4.8 GHz formaldehyde absorption lines, and H2CO signals have been detected in 86 of them, 31 of which are newly discovered. We obtained good correlation (0.85 correlation coefficient) between the velocities of the sources, and a poor correlation (-0.03 correlation coefficient) between their intensities, an indication that signals from the two lines originate from about the same region, but that the excitation mechanisms that drive them are likely different.

  14. Comparison of Three Statistical Classification Techniques for Maser Identification

    Science.gov (United States)

    Manning, Ellen M.; Holland, Barbara R.; Ellingsen, Simon P.; Breen, Shari L.; Chen, Xi; Humphries, Melissa

    2016-04-01

    We applied three statistical classification techniques-linear discriminant analysis (LDA), logistic regression, and random forests-to three astronomical datasets associated with searches for interstellar masers. We compared the performance of these methods in identifying whether specific mid-infrared or millimetre continuum sources are likely to have associated interstellar masers. We also discuss the interpretability of the results of each classification technique. Non-parametric methods have the potential to make accurate predictions when there are complex relationships between critical parameters. We found that for the small datasets the parametric methods logistic regression and LDA performed best, for the largest dataset the non-parametric method of random forests performed with comparable accuracy to parametric techniques, rather than any significant improvement. This suggests that at least for the specific examples investigated here accuracy of the predictions obtained is not being limited by the use of parametric models. We also found that for LDA, transformation of the data to match a normal distribution led to a significant improvement in accuracy. The different classification techniques had significant overlap in their predictions; further astronomical observations will enable the accuracy of these predictions to be tested.

  15. The brightest OH maser in the sky: a flare of emission in W75 N

    OpenAIRE

    Alakoz, A. V.; Slysh, V. I.; Popov, M. V.; Val'tts, I. E.

    2005-01-01

    A flare of maser radio emission in the OH-line 1665 MHz has been discovered in the star forming region W75 N in 2003, with the flux density of about 1000 Jy. At the time it was the strongest OH maser detected during the whole history of observations since the discovery of cosmic masers in 1965. The flare emission is linearly polarized with a degree of polarization near 100%. A weaker flare with a flux of 145 Jy was observed in this source in 2000 - 2001, which was probably a precursor of the ...

  16. Search for electric dipole moment in 129Xe atom using active nuclear spin maser

    Directory of Open Access Journals (Sweden)

    Ichikawa Y.

    2014-03-01

    Full Text Available An experimental search for an electric dipole moment in the diamagnetic atom 129Xe is in progress through the precision measurement of spin precession frequency using an active nuclear spin maser. A 3He comagnetometer has been incorporated into the active spin maser system in order to cancel out the long-term drifts in the external magnetic field. Also, a double-cell geometry has been adopted in order to suppress the frequency shifts due to interaction with polarized Rb atoms. The first EDM measurement with the 129Xe active spin maser and the 3He comagnetometer has been conducted.

  17. Historical Cost Curves for Hydrogen Masers and Cesium Beam Frequency and Timing Standards

    Science.gov (United States)

    Remer, D. S.; Moore, R. C.

    1985-01-01

    Historical cost curves were developed for hydrogen masers and cesium beam standards used for frequency and timing calibration in the Deep Space Network. These curves may be used to calculate the cost of future hydrogen masers or cesium beam standards in either future or current dollars. The cesium beam standards are decreasing in cost by about 2.3% per year since 1966, and hydrogen masers are decreasing by about 0.8% per year since 1978 relative to the National Aeronautics and Space Administration inflation index.

  18. Modelling CH$_3$OH masers: Sobolev approximation and accelerated lambda iteration method

    CERN Document Server

    Nesterenok, Aleksandr

    2015-01-01

    A simple one-dimensional model of CH$_3$OH maser is considered. Two techniques are used for the calculation of molecule level populations: the accelerated lambda iteration (ALI) method and the large velocity gradient (LVG), or Sobolev, approximation. The LVG approximation gives accurate results provided that the characteristic dimensions of the medium are larger than 5-10 lengths of the resonance region. We presume that this condition can be satisfied only for the largest observed maser spot distributions. Factors controlling the pumping of class I and class II methanol masers are considered.

  19. Optical-coupling nuclear spin maser under highly stabilized low static field

    Energy Technology Data Exchange (ETDEWEB)

    Yoshimi, A., E-mail: yoshimi@ribf.riken.jp [RIKEN Nishina Center (Japan); Inoue, T.; Uchida, M.; Hatakeyama, N.; Asahi, K. [Tokyo Institute of Technology, Department of Physics (Japan)

    2008-01-15

    A nuclear spin maser of a new type, that employs a feedback scheme based on optical nuclear spin detection, has been fabricated. The spin maser is operated at a low static field of 30 mG by using the optical detection method. The frequency stability and precision of the spin maser have been improved by a highly stabilized current source for the static magnetic field. An experimental setup to search for an electric dipole moment (EDM) in {sup 129}Xe atom is being developed.

  20. MAGNETIC FIELDS AND THE POLARIZATION OF ASTROPHYSICAL MASER RADIATION: A REVIEW

    Directory of Open Access Journals (Sweden)

    W. D. Watson

    2009-01-01

    Full Text Available Basic aspects of the relationship between the magnetic eld and polarized maser radiation are described with the emphasis on interpreting the observed spectra. Special attention is given to three issues { the limitations on the applicability of the classic solutions of Goldreich, Keeley, & Kwan (1973, inferring the strength of the magnetic eld from the circular polarization when the Zeeman splitting is much less than the spectral linebreadth (especially for SiO masers, and the signi cance of the absence of components of the Zeeman triplet in the spectra of OH masers in regions of star formation.

  1. RUBI: rapid proteomic-scale prediction of lysine ubiquitination and factors influencing predictor performance.

    Science.gov (United States)

    Walsh, Ian; Di Domenico, Tomás; Tosatto, Silvio C E

    2014-04-01

    Post-translational modification of protein lysines was recently shown to be a common feature of eukaryotic organisms. The ubiquitin modification is regarded as a versatile regulatory mechanism with many important cellular roles. Large-scale datasets are becoming available for H. sapiens ubiquitination. However, using current experimental techniques the vast majority of their sites remain unidentified and in silico tools may offer an alternative. Here, we introduce Rapid UBIquitination (RUBI) a sequence-based ubiquitination predictor designed for rapid application on a genome scale. RUBI was constructed using an iterative approach. At each iteration, important factors which influenced performance and its usability were investigated. The final RUBI model has an AUC of 0.868 on a large cross-validation set and is shown to outperform other available methods on independent sets. Predicted intrinsic disorder is shown to be weakly anti-correlated to ubiquitination for the H. sapiens dataset and improves performance slightly. RUBI predicts the number of ubiquitination sites correctly within three sites for ca. 80% of the tested proteins. The average potentially ubiquitinated proteome fraction is predicted to be at least 25% across a variety of model organisms, including several thousand possible H. sapiens proteins awaiting experimental characterization. RUBI can accurately predict ubiquitination on unseen examples and has a signal across different eukaryotic organisms. The factors which influenced the construction of RUBI could also be tested in other post-translational modification predictors. One of the more interesting factors is the influence of intrinsic protein disorder on ubiquitinated lysines where residues with low disorder probability are preferred.

  2. Disk-outflow models as applied to high mass star forming regions through methanol and water maser observations

    CERN Document Server

    Farmer, Hontas

    2013-01-01

    As the recent publication by Breen et al (2013) found Class II methanol masers are exclusively associated with high mass star forming regions. Based on the positions of the Class I and II methanol and H$_{2}$O masers, UC H II regions and 4.5 $\\mu$m infrared sources, and the center velocities ($v_{\\text{LSR}}$) of the Class I methanol and H$_{2}$O masers, compared to the $v_{\\text{LSR}}$ of the Class II methanol masers, we propose three disk-outflow models that may be traced by methanol masers. In all three models, we have located the Class II methanol maser near the protostar, and the Class I methanol maser in the outflow, as is known from observations during the last twenty years. In our first model, the H$_{2}$O masers trace the linear extent of the outflow. In our second model, the H$_{2}$O masers are located in a circumstellar disk. In our third model, the H$_{2}$O masers are located in one or more outflows near the terminating shock where the outflow impacts the ambient interstellar medium. Together, the...

  3. Ruby and Sm:YAG fluorescence pressure gauges up to 120 GPa and 700 K

    Science.gov (United States)

    Wei, Qingguo; Dubrovinskaia, Natalia; Dubrovinsky, Leonid

    2011-08-01

    Diamond anvil cell (DAC) technique relies on pressure determination based on use of pressure gauges. Fluorescence-based gauges, such as ruby and Sm doped yttrium aluminum garnet (Sm:YAG), are frequently used in the high pressure research. Here we present the results of DAC experiments which allowed extending calibration curves of the fluorescence frequency versus pressure up to 120 GPa at high temperatures up to 700 K for both for ruby and Sm:YAG. Cubic boron nitride was used as the reference gauge.

  4. Observation of ultraslow light propagation in a ruby crystal at room temperature.

    Science.gov (United States)

    Bigelow, Matthew S; Lepeshkin, Nick N; Boyd, Robert W

    2003-03-21

    We have observed slow light propagation with a group velocity as low as 57.5+/-0.5 m/s at room temperature in a ruby crystal. A quantum coherence effect, coherent population oscillations, produces a very narrow spectral "hole" in the homogeneously broadened absorption profile of ruby. The resulting rapid spectral variation of the refractive index leads to a large value of the group index. We observe slow light propagation both for Gaussian-shaped light pulses and for amplitude modulated optical beams in a system that is much simpler than those previously used for generating slow light.

  5. Ruby on Rails与Struts+Hibernate架构之比较分析

    Institute of Scientific and Technical Information of China (English)

    吴吉义

    2007-01-01

    Ruby on Rails是一个基于Ruby语言构建的全新Web应用程序架构,为Web应用程序开发提供了一种极其快捷的途径,正在和已经引起业界相当的兴趣.在给出了Ruby on Rails与轻量级J2EE架构Struts+Hibernate关键特性的基础上,从前端控制器、动作和模型,持久性框架三个方面对两种架构进行了比较.

  6. Growth of ruby and sapphire crystals by the flux method; Crescimento de cristais de rubi e safira pelo metodo do fluxo

    Energy Technology Data Exchange (ETDEWEB)

    Ribeiro, Gislene da Silva [Universidade Federal de Mato Grosso (DRM/UFMT), Cuiaba, MT (Brazil). Dept. de Recuros Minerais; Prado, Rogerio Junqueira, E-mail: rjprado@ufmt.b [Universidade Federal de Mato Grosso (IF/UFMT), Cuiaba, MT (Brazil). Inst. de Fisica

    2010-07-01

    This work reports the growth of corundum crystals by the flux method. The main objective was the evaluation of versatility, effectiveness and real possibilities of the flux method to the synthesis and doping of monocrystals with impurities of particular interest. In this work the chosen impurities were 1) Cr and 2) Fe and Ti, aiming the synthesis of rubies and sapphires, respectively. The crystals were grown by heating a mixture of Al{sub 2}O{sub 3}:Cr or Al{sub 2}O{sub 3}:Fe:Ti and flux (MoO{sub 3}). The maximum crystal size obtained was 1.0 mm, all transparent, presenting well developed faces, bipyramidal hexagonal shape, and showing a typical red (ruby) and/or light blue (sapphire) color. EDX and XPD experiments were performed in order to characterize some of the synthesized crystals. All crystallized specimens presented the a-alumina atomic structure. (author)

  7. Crescimento de cristais de rubi e safira pelo método do fluxo Growth of ruby and sapphire crystals by the flux method

    Directory of Open Access Journals (Sweden)

    Gislene da Silva Ribeiro

    2010-01-01

    Full Text Available This work reports the growth of corundum crystals by the flux method. The main objective was the evaluation of versatility, effectiveness and real possibilities of the flux method to the synthesis and doping of monocrystals with impurities of particular interest. In this work the chosen impurities were i Cr and ii Fe and Ti, aiming the synthesis of rubies and sapphires, respectively. The crystals were grown by heating a mixture of Al2O3:Cr or Al2O3:Fe:Ti and flux (MoO3. The maximum crystal size obtained was 1.0 mm, all transparent, presenting well developed faces, bipiramidal hexagonal shape, and showing a typical red (ruby and/or light blue (sapphire color. EDX and XPD experiments were performed in order to characterize some of the synthesized crystals. All crystallized specimens presented the α-alumina atomic structure.

  8. Extremely Rapid Variations of Water Maser Emission from the Circinus Galaxy

    CERN Document Server

    Greenhill, L J; Norris, R P; Gough, R G; Sinclair, M W; Moran, J M; Mushotzky, R F

    1996-01-01

    The water maser lines in the nucleus of the Circinus galaxy vary on time scales as short as a few minutes, at least two orders of magnitude less than for other Galactic or extragalactic water masers. The amplitude of one line more than doubled in about 10 minutes. The intensity changes cannot be attributed easily to a mechanism of intrinsic fluctuations. The variability may be the result of strong interstellar diffractive scintillation along the line of sight within our Galaxy, which would be the first example of diffractive scintillation for any source at 22 GHz and for any source other than a pulsar. However, only the very shortest timescales for interstellar scintillation, obtained from pulsar observations and scaled to 22 GHz, correspond to the observed maser variability. Alternatively, the intensity changes may be a reaction to fluctuations in compact background or radiative pump sources and thereby may be related to variability of the central engine. The maser spectral features symmetrically bracket the...

  9. Water maser emission from X-ray-heated circumnuclear gas in active galaxies

    Science.gov (United States)

    Neufeld, David A.; Maloney, Philip R.; Conger, Sarah

    1994-01-01

    We have modeled the physical and chemical conditions present within dense circumnuclear gas that is irradiated by X-rays from an active galactic nucleus. Over a wide range of X-ray fluxes and gas pressures, the effects of X-ray heating give rise to a molecular layer at temperatures of 400-1000 K within which the water abundance is large. The physical conditions within this molecular layer naturally give rise to collisionally pumped maser emission in the 6(sub 16) - 5(sub 23) 22 GHz transition of ortho-water, with predicted maser luminosities of 10(exp 2 +/- 0.5) solar luminosity per sq. pc of illuminated area. Given plausible assumptions about the geometry of the source and about the degree to which the maser emission is anisotropic, such surface luminosities are sufficient to explain the large apparent luminosities observed in water maser sources that are associated with active galactic nuclei.

  10. Water maser emission from X-ray-heated circumnuclear gas in active galaxies

    Science.gov (United States)

    Neufeld, David A.; Maloney, Philip R.; Conger, Sarah

    1994-12-01

    We have modeled the physical and chemical conditions present within dense circumnuclear gas that is irradiated by X-rays from an active galactic nucleus. Over a wide range of X-ray fluxes and gas pressures, the effects of X-ray heating give rise to a molecular layer at temperatures of 400-1000 K within which the water abundance is large. The physical conditions within this molecular layer naturally give rise to collisionally pumped maser emission in the 616 - 523 22 GHz transition of ortho-water, with predicted maser luminosities of 102 +/- 0.5 solar luminosity per sq. pc of illuminated area. Given plausible assumptions about the geometry of the source and about the degree to which the maser emission is anisotropic, such surface luminosities are sufficient to explain the large apparent luminosities observed in water maser sources that are associated with active galactic nuclei.

  11. An Infrared Photometric Study of Galaxies with Extragalactic H2O Maser Sources

    Institute of Scientific and Technical Information of China (English)

    2007-01-01

    All galaxies with extragalactic H2O maser sources observed so far are collected. With the 2MASS and the IRAS photometric data an infrared study is performed on those galaxies. By a comparison between the H2O maser detected sources and non-detected sources in the infrared it is indicated that infrared properties in the IRAS 12-25/μm and 60-100/μm are important for producing H2O masers in galaxies. It is also found that the H2O maser galaxies with different nuclear activity types have rather different infrared properties mainly in the IRAS 12-60/μm region.

  12. Distances to Dark Clouds: Comparing Extinction Distances to Maser Parallax Distances

    CERN Document Server

    Foster, Jonathan B; Benjamin, Robert A; Hoare, Melvin G; Jackson, James M

    2012-01-01

    We test two different methods of using near-infrared extinction to estimate distances to dark clouds in the first quadrant of the Galaxy using large near infrared (2MASS and UKIDSS) surveys. VLBI parallax measurements of masers around massive young stars provide the most direct and bias-free measurement of the distance to these dark clouds. We compare the extinction distance estimates to these maser parallax distances. We also compare these distances to kinematic distances, including recent re-calibrations of the Galactic rotation curve. The extinction distance methods agree with the maser parallax distances (within the errors) between 66% and 100% of the time (depending on method and input survey) and between 85% and 100% of the time outside of the crowded Galactic center. Although the sample size is small, extinction distance methods reproduce maser parallax distances better than kinematic distances; furthermore, extinction distance methods do not suffer from the kinematic distance ambiguity. This validatio...

  13. Hemangioma rubi no couro cabeludo Cherry hemangioma in the scalp

    Directory of Open Access Journals (Sweden)

    José Marcos Pereira

    2004-02-01

    Full Text Available O hemangioma rubi (HR é dermatose de origem vascular extremamente freqüente, acometendo mais de 75% da população acima de 70 anos de idade. Em geral compõe-se de lesões múltiplas,localizadas predominantemente no alto do tronco e braços. Clinicamente é caracterizado por lesões que variam desde máculas puntiformes até lesões papulosas com cinco milímetros de diâmetro. As mais novas são vermelhas, em tons vivos, e as mais antigas podem ser azuladas. O HR é de etiologia desconhecida. Histologicamente chama atenção uma neoformação de vasos capilares, que se tornam dilatados e com fenestrações em suas paredes. A membrana basal está muito espessada e existe abundante estroma de colágeno entre os vasos. O presente trabalho demonstra a alta incidência do HR no couro cabeludo Em amostra de 171 pacientes, sendo 85 homens e 86 mulheres, o autor observou que 123 deles (72% tinham HR no couro cabeludo, localização em que o HR nunca foi descrito na literatura.Cherry hemangioma (CH is an extremely frequent dermatosis with vascular origin involving more than 75% of the population over 70 years of age. Normally they are multiplex spots and focus predominantly on the upper trunk and arms. Clinically they are characterized by pinpoint maculae and papules with up to 5 millimeters in diameter. The most recent lesions can be a strong red color while the older ones are bluish. The etiology of CH is still unknown. From the histologic standpoint, the neoformation of the capillary tube draws attention: they are very dilated and with fenestration along the wall. The basement membranes are thickened and there is abundant collagen stroma between the veins. This work demonstrates the high frequency of CH in the scalp. In a sample of 171 patients (85 men and 86 women the author noted that 123 (72% had CH in the scalp. However, according to the literature, CH in the scalp has never been described.

  14. ITEL Experiment Module and its Flight on MASER9

    Science.gov (United States)

    Löth, K.; Schneider, H.; Larsson, B.; Jansson, O.; Houltz, Y.

    2002-01-01

    The ITEL (Interfacial Turbulence in Evaporating Liquid) module is built under contract from the European Space Agency (ESA) and is scheduled to fly onboard a Sounding Rocket (MASER 9) in March 2002. The project is conducted by Swedish Space Corporation (SSC) with Lambda-X as a subcontractor responsible for the optical system. The Principle Investigator is Pierre Colinet from Université Libre de Bruxelles (ULB). The experiment in ITEL on Maser 9 is part of a research program, which will make use of the International Space Station. The purpose of the flight on Maser 9 is to observe the cellular convection (Marangoni-Bénard instability) which arise when the surface tension varies with temperature yielding thermocapillary instabilities. During the 6 minutes of microgravity of the ITEL experiment, a highly volatile liquid layer (ethyl alcohol) will be evaporated, and the convection phenomena generated by the evaporation process will be visualized. Due to the cooling by latent heat consumption at the level of the evaporating free surface, a temperature gradient is induced perpendicularly to it. The flight experiment module contains one experiment cell, including a gas system for regulation of nitrogen flow over the evaporating surface and an injection unit that is used for injection of liquid into the cell both initially and during surface regulation. The experiment cell is equipped with pressure and flow sensors as well as thermocouples both inside the liquid and at different positions in the cell. Two optical diagnostic systems have been developed around the experiment cell. An interferometric optical tomograph measures the 3-dimensional distribution of temperature in the evaporating liquid and a Schlieren system visualizes the temperature gradients inside the liquid together with the liquid surface deformation. A PC/104 based electronic system is used for management and control of the experiment. The electronic system handles measurements, housekeeping, image

  15. A Search for Water Maser Emission from Brown Dwarfs and Low-luminosity Young Stellar Objects

    Science.gov (United States)

    Gómez, José F.; Palau, Aina; Uscanga, Lucero; Manjarrez, Guillermo; Barrado, David

    2017-05-01

    We present a survey for water maser emission toward a sample of 44 low-luminosity young objects, comprising (proto-)brown dwarfs, first hydrostatic cores (FHCs), and other young stellar objects (YSOs) with bolometric luminosities lower than 0.4 L ⊙. Water maser emission is a good tracer of energetic processes, such as mass-loss and/or accretion, and is a useful tool to study these processes with very high angular resolution. This type of emission has been confirmed in objects with L bol ≳ 1 L ⊙. Objects with lower luminosities also undergo mass-loss and accretion, and thus, are prospective sites of maser emission. Our sensitive single-dish observations provided a single detection when pointing toward the FHC L1448 IRS 2E. However, follow-up interferometric observations showed water maser emission associated with the nearby YSO L1448 IRS 2 (a Class 0 protostar of L bol ≃ 3.6-5.3 L ⊙) and did not find any emission toward L1448 IRS 2E. The upper limits for water maser emission determined by our observations are one order of magnitude lower than expected from the correlation between water maser luminosities and bolometric luminosities found for YSOs. This suggests that this correlation does not hold at the lower end of the (sub)stellar mass spectrum. Possible reasons are that the slope of this correlation is steeper at L bol ≤ 1 L ⊙ or that there is an absolute luminosity threshold below which water maser emission cannot be produced. Alternatively, if the correlation still stands at low luminosity, the detection rates of masers would be significantly lower than the values obtained in higher-luminosity Class 0 protostars.

  16. St\\"ackel-type dynamic model of the Galaxy based on maser kinematic data

    CERN Document Server

    Gromov, A O; Ossipkov, L P

    2016-01-01

    A dynamic model of the Galaxy is constructed based on kinematic data for masers with trigonometric parallaxes. Maser data is used to compute the model potential in the Galactic plane. The potential is then generalized to three dimensions assuming the existence of a third quadratic integral of motion. The resulting Galactic model potential is of St\\"ackel's type. The corresponding space density function is determined from Poisson's equation.

  17. Distribution of H/sub 2/O masers in the sagittarius B2 core

    Energy Technology Data Exchange (ETDEWEB)

    Kobayashi, Hideyuki; Ishiguro, Masato; Chikada, Yoshihiro; Ukita, Nobuharu; Morita, Koh-ichiro; Okumura, S.K.; Kasuga, Takashi; Kawabe, Ryohei

    1989-01-01

    The first results of H/sub 2/O maser observations with the Nobeyama Millimeter array are presented. The distribution of H/sub 2/O masers in the Sgr B2 core was observed with a 2'.5 x 2'.5 wide field and with 540 kms/sup -1/ total velocity coverage. Thirty-nine resolved maser spots were detected with a relative positional accuracy of 0''.3, which are clustered into four separate regions. Three of them are previously known and lie close to compact H2 regions. The fourth, newly discovered, is not associated with a continuum source, but is close to the site of H/sub 2/CO and OH masers in the middle of Sgr B2(N) and Sgr B2(M). In Sgr B2 North, the cluster lies at the edge of the continuum ridge. One of the maser spots shows strong and wide velocity-spread emission, suggesting it may correspond to a center of star-forming activity. In Sgr B2 Middle, the strong maser spots are projected just on the face of a compact H2 region, and are redshifted relative to the central velocity of the H2 region. There are two possibilities to interpret our results in Sgr B2(M). One is the H/sub 2/O maser spots distribute around the H2 region and are infalling to the H2 region. The other is the H/sub 2/O maser sources are associated with the cloud in the foreground of the H2 region. (author).

  18. Suppression of cyclotron instability in Electron Cyclotron Resonance ion sources by two-frequency heating

    Energy Technology Data Exchange (ETDEWEB)

    Skalyga, V. [Institute of Applied Physics of Russian Academy of Sciences, 46 Ulyanova st., Nizhny Novgorod (Russian Federation); Lobachevsky State University of Nizhny Novgorod (UNN), 23 Gagarina st., Nizhny Novgorod (Russian Federation); Izotov, I.; Mansfeld, D. [Institute of Applied Physics of Russian Academy of Sciences, 46 Ulyanova st., Nizhny Novgorod (Russian Federation); Kalvas, T.; Koivisto, H.; Komppula, J.; Kronholm, R.; Laulainen, J.; Tarvainen, O. [Department of Physics, University of Jyväskylä, Jyväskylä (Finland)

    2015-08-15

    Multiple frequency heating is one of the most effective techniques to improve the performance of Electron Cyclotron Resonance (ECR) ion sources. The method increases the beam current and average charge state of the extracted ions and enhances the temporal stability of the ion beams. It is demonstrated in this paper that the stabilizing effect of two-frequency heating is connected with the suppression of electron cyclotron instability. Experimental data show that the interaction between the secondary microwave radiation and the hot electron component of ECR ion source plasmas plays a crucial role in mitigation of the instabilities.

  19. Nanosecond time-resolved characterization of a pentacene-based room-temperature MASER

    Science.gov (United States)

    Salvadori, Enrico; Breeze, Jonathan D.; Tan, Ke-Jie; Sathian, Juna; Richards, Benjamin; Fung, Mei Wai; Wolfowicz, Gary; Oxborrow, Mark; Alford, Neil Mcn.; Kay, Christopher W. M.

    2017-02-01

    The performance of a room temperature, zero-field MASER operating at 1.45 GHz has been examined. Nanosecond laser pulses, which are essentially instantaneous on the timescale of the spin dynamics, allow the visible-to-microwave conversion efficiency and temporal response of the MASER to be measured as a function of excitation energy. It is observed that the timing and amplitude of the MASER output pulse are correlated with the laser excitation energy: at higher laser energy, the microwave pulses have larger amplitude and appear after shorter delay than those recorded at lower laser energy. Seeding experiments demonstrate that the output variation may be stabilized by an external source and establish the minimum seeding power required. The dynamics of the MASER emission may be modeled by a pair of first order, non-linear differential equations, derived from the Lotka-Volterra model (Predator-Prey), where by the microwave mode of the resonator is the predator and the spin polarization in the triplet state of pentacene is the prey. Simulations allowed the Einstein coefficient of stimulated emission, the spin-lattice relaxation and the number of triplets contributing to the MASER emission to be estimated. These are essential parameters for the rational improvement of a MASER based on a spin-polarized triplet molecule.

  20. Proper Motions of H2O Masers in the Water Fountain Source IRAS 19190+1102

    CERN Document Server

    Day, F M; Claussen, M J; Sahai, R

    2010-01-01

    We report on the results of two epochs of Very Long Baseline Array (VLBA) observations of the 22 GHz water masers toward IRAS 19190+1102. The water maser emission from this object shows two main arc-shaped formations perpendicular to their NE-SW separation axis. The arcs are separated by ~280 mas in position, and are expanding outwards at an angular rate of 2.35 mas/yr. We detect maser emission at velocities between -53.3 km/s to +78.0 km/s and there is a distinct velocity pattern where the NE masers are blueshifted and the SW masers are redshifted. The outflow has a three-dimensional outflow velocity of 99.8 km/s and a dynamical age of about 59 yr. A group of blueshifted masers not located along the arcs shows a change in velocity of more than 35 km/s between epochs, and may be indicative of the formation of a new lobe. These observations show that IRAS 19190+1102 is a member of the class of "water fountain"' pre-planetary nebulae displaying bipolar structure

  1. Methanol and excited OH masers towards W51: I - Main and South

    CERN Document Server

    Etoka, Sandra; Fuller, Gary A

    2012-01-01

    MERLIN phase-referenced polarimetric observations towards the W51 complex were carried out in March 2006 in the Class II methanol maser transition at 6.668 GHz and three of the four excited OH maser hyperfine transitions at 6 GHz. Methanol maser emission is found towards both W51 Main and South. We did not detect any emission in the excited OH maser lines at 6.030 and 6.049 GHz down to a 3 sigma limit of ~20 mJy per beam. Excited OH maser emission at 6.035 GHz is only found towards W51 Main. This emission is highly circularly polarised (typically 45% and up to 87%). Seven Zeeman pairs were identified in this transition, one of which contains detectable linear polarisation. The magnetic field strength derived from these Zeeman pairs ranges from +1.6 to +6.8 mG, consistent with the previously published magnetic field strengths inferred from the OH ground-state lines. The bulk of the methanol maser emission is associated with W51 Main, sampling a total area of ~3"x2.2" (i.e., ~16200x11900 AU), while only two mas...

  2. H$_2$O maser emission from bright rimmed clouds in the northern hemisphere

    CERN Document Server

    Valdettaro, R; Brand, J; Cesaroni, R

    2005-01-01

    We report the results of a multi-epoch survey of water maser observations at 22.2 GHz with the Medicina radiotelescope from 44 bright rimmed clouds (BRCs) of the northern hemisphere identified by Sugitani et al. (1989) as potential sites of star formation. The data span 16 years of observations and allow to draw conclusions about the maser detection rate in this class of objects. In spite of the relatively high far-infrared luminosities of the embedded sources ($L_{\\rm FIR}\\ga 10^2$ L$_\\odot$), H$_2$O maser emission was detected towards three globules only. Since the occurrence of water masers is higher towards bright IRAS sources, the lack of frequent H$_2$O maser emission is somewhat surprising if the suggestion of induced intermediate- and high-mass star formation within these globules is correct. The maser properties of two BRCs are characteristic of exciting sources of low-mass, while the last one (BRC~38) is consistent with an intermediate-mass object. We argue that most BRCs host young stellar objects ...

  3. A search for 85.5- and 86.6-GHz methanol maser emission

    CERN Document Server

    Ellingsen, S P; Minier, V; Müller, E; Godfrey, P D

    2003-01-01

    We have used the Australia Telescope National Facility Mopra 22m millimetre telescope to search for emission from the 85.5-GHz and 86.6-GHz transitions of methanol. The search was targeted towards 22 star formation regions which exhibit maser emission in the 107.0-GHz methanol transition, as well as in the 6.6-GHz transition characteristic of class II methanol maser sources. A total of 22 regions were searched at 85.5 GHz resulting in 5 detections, of which 1 appears to be a newly discovered maser. For the 86.6-GHz transition observations were made of 18 regions which yielded 2 detections, but no new maser sources. This search demonstrates that emission from the 85.5- and 86.6-GHz transitions is rare. Detection of maser emission from either of these transitions therefore indicates the presence of special conditions, different from those in the majority of methanol maser sources. We have observed temporal variability in the 86.6-GHz emission towards 345.010+1.792, which along with the very narrow line width, c...

  4. A `Water Spout' Maser Jet in S235AB-MIR

    CERN Document Server

    Burns, Ross A; Handa, Toshihiro; Omodaka, Toshihiro; Nakagawa, Akiharu; Nagayama, Takumi; Ueno, Yuji

    2015-01-01

    We report on annual parallax and proper motion observations of H2O masers in S235AB-MIR, which is a massive young stellar object in the Perseus Arm. Using multi-epoch VLBI astrometry we measured a parallax of pi = 0.63 +- 0.03 mas, corresponding to a trigonometric distance of D = 1.56+-0.09 kpc, and source proper motion of ( u alpha cos d , u d) = (0.79 +- 0.12, -2.41 +- 0.14) mas/yr. Water masers trace a jet of diameter 15 au which exhibits a definite radial velocity gradient perpendicular to its axis. 3D maser kinematics were well modelled by a rotating cylinder with physical parameters: v_out = 45+-2 km/s, v_rot = 22+-3 km/s, i = 12+-2 degrees, which are the outflow velocity, tangential rotation velocity and line-of-sight inclination, respectively. One maser feature exhibited steady acceleration which may be related to the jet rotation. During our 15 month VLBI programme there were three `maser burst' events caught `in the act' which were caused by the overlapping of masers along the line of sight.

  5. A Water Maser and Ammonia Survey of GLIMPSE Extended Green Objects (EGOs)

    CERN Document Server

    Cyganowski, C J; Rosolowsky, E; Towers, S; Meyer, J Donovan; Egusa, F; Momose, R; Robitaille, T P

    2012-01-01

    We present the results of a Nobeyama 45-m water maser and ammonia survey of all 94 northern GLIMPSE Extended Green Objects (EGOs), a sample of massive young stellar objects (MYSOs) identified based on their extended 4.5 micron emission. We observed the ammonia (1,1), (2,2), and (3,3) inversion lines, and detect emission towards 97%, 63%, and 46% of our sample, respectively (median rms ~50 mK). The water maser detection rate is 68% (median rms ~0.11 Jy). The derived water maser and clump-scale gas properties are consistent with the identification of EGOs as young MYSOs. To explore the degree of variation among EGOs, we analyze subsamples defined based on MIR properties or maser associations. Water masers and warm dense gas, as indicated by emission in the higher-excitation ammonia transitions, are most frequently detected towards EGOs also associated with both Class I and II methanol masers. 95% (81%) of such EGOs are detected in water (ammonia(3,3)), compared to only 33% (7%) of EGOs without either methanol m...

  6. EVN observations of 6.7 GHz methanol masers in clusters of massive young stellar objects

    CERN Document Server

    Bartkiewicz, Anna; van Langevelde, Huib

    2014-01-01

    Methanol masers at 6.7 GHz are associated with high-mass star-forming regions (HMSFRs) and often have mid-infrared (MIR) counterparts characterized by extended emission at 4.5 $\\mu$m, which likely traces outflows from massive young stellar objects (MYSOs). Our objectives are to determine the milliarcsecond (mas) morphology of the maser emission and to examine if it comes from one or several candidate MIR counterparts in the clusters of MYSOs. The European VLBI Network (EVN) was used to image the 6.7 GHz maser line with ~2.'1 field of view toward 14 maser sites from the Torun catalog. Quasi-simultaneous observations were carried out with the Torun 32 m telescope. We obtained maps with mas angular resolution that showed diversity of methanol emission morphology: a linear distribution (e.g., G37.753-00.189), a ring-like (G40.425+00.700), and a complex one (e.g., G45.467+00.053). The maser emission is usually associated with the strongest MIR counterpart in the clusters; no maser emission was detected from other ...

  7. The 6-GHz methanol multibeam maser catalogue I: Galactic Centre region, longitudes 345 to 6

    CERN Document Server

    Caswell, J L; Green, J A; Avison, A; Breen, S L; Brooks, K J; Burton, M G; Chrysostomou, A; Cox, J; Diamond, P J; Ellingsen, S P; Gray, M D; Hoare, M G; Masheder, M R W; McClure-Griffiths, N M; Pestalozzi, M R; Phillips, C J; Quinn, L; Thompson, M A; Voronkov, M A; Walsh, A J; Ward-Thompson, D; Wong-McSweeney, D; Yates, J A; Cohen, R J

    2010-01-01

    We have conducted a Galactic plane survey of methanol masers at 6668 MHz using a 7-beam receiver on the Parkes telescope. Here we present results from the first part, which provides sensitive unbiased coverage of a large region around the Galactic Centre. Details are given for 183 methanol maser sites in the longitude range 345$^{\\circ}$ through the Galactic Centre to 6$^{\\circ}$. Within 6$^{\\circ}$ of the Centre, we found 88 maser sites, of which more than half (48) are new discoveries. The masers are confined to a narrow Galactic latitude range, indicative of many sources at the Galactic Centre distance and beyond, and confined to a thin disk population; there is no high latitude population that might be ascribed to the Galactic Bulge. Within 2$^{\\circ}$ of the Galactic Centre the maser velocities all lie between -60 and +77 \\kms, a range much smaller than the 540 \\kms range observed in CO. Elsewhere, the maser with highest positive velocity (+107 \\kms) occurs, surprisingly, near longitude 355$^{\\circ}$ and...

  8. A 95 GHz Class I Methanol Maser Survey Toward GLIMPSE Extended Green Objects (EGOs)

    CERN Document Server

    Chen, Xi; Shen, Zhi-Qiang; Titmarsh, Anita; Gan, Cong-Gui

    2011-01-01

    We report the results of a systematic survey for 95 GHz class I methanol masers towards a new sample of 192 massive young stellar object (MYSO) candidates associated with ongoing outflows (known as extended green objects or EGOs) identified from the Spitzer GLIMPSE survey. The observations were made with the Australia Telescope National Facility (ATNF) Mopra 22-m radio telescope and resulted in the detection of 105 new 95 GHz class I methanol masers. For 92 of the sources our observations provide the first identification of a class I maser transition associated with these objects (i.e. they are new class I methanol maser sources). Our survey proves that there is indeed a high detection rate (55%) of class I methanol masers towards EGOs. Comparison of the GLIMPSE point sources associated with EGOs with and without class I methanol maser detections shows they have similar mid-IR colors, with the majority meeting the color selection criteria -0.6<[5.8]-[8.0]<1.4 and 0.5<[3.6]-[4.5]<4.0. Investigation...

  9. Whole Genome Sequences of the Raspberry and Strawberry Pathogens Phytophthora rubi and P. fragariae.

    Science.gov (United States)

    Tabima, Javier F; Kronmiller, Brent A; Press, Caroline M; Tyler, Brett M; Zasada, Inga A; Grünwald, Niklaus J

    2017-10-01

    Phytophthora rubi and P. fragariae are two closely related oomycete plant pathogens that exhibit strong morphological and physiological similarities but are specialized to infect different hosts of economic importance, namely, raspberry and strawberry. Here, we report the draft genome sequences of these two Phytophthora species as a first step toward understanding the genomic processes underlying plant host adaptation in these pathogens.

  10. Peddling Poverty for Profit: Elements of Oppression in Ruby Payne's Framework

    Science.gov (United States)

    Gorski, Paul C.

    2008-01-01

    Ruby Payne, CEO of aha! Process, Inc., and author of "A Framework for Understanding Poverty" (2005), has become one of the most influential figures in the U.S. public education milieu. Payne's framework, built largely upon understanding the "culture" of poverty, instructs educators on the values and mindsets poor students carry into the classroom…

  11. Performance evaluation of Abbott CELL-DYN Ruby for routine use.

    Science.gov (United States)

    Lehto, T; Hedberg, P

    2008-10-01

    CELL-DYN Ruby is a new automated hematology analyzer suitable for routine use in small laboratories and as a back-up or emergency analyzer in medium- to high-volume laboratories. The analyzer was evaluated by comparing the results from the CELL-DYN((R)) Ruby with the results obtained from CELL-DYN Sapphire . Precision, linearity, and carryover between patient samples were also assessed. Precision was good at all levels for the routine cell blood count (CBC) parameters, CV% being CELL-DYN Ruby results showed a good correlation (R(2) >or= 0.98) with CELL-DYN Sapphire for the CBC parameters. For the absolute reticulocyte count, R(2) was 0.82. In the white blood cell (WBC) differentials, the between-days precision was good for all parameters (CV%: cell types that occur in low numbers showed higher CVs, as expected. The methodological comparison of the WBC differential parameters of neutrophils, lymphocytes, and eosinophils showed excellent correlations (R(2) >or= 0.97), and the correlation coefficient for absolute monocyte count and monocyte percentage were 0.91 and 0.87, respectively. For absolute basophil count and basophil percentage the correlations were weaker (R(2) = 0.46 and 0.34, respectively). Carryover was minimal for all the parameters studied. The linearities of WBC, red blood cell, PLTs, and hemoglobin were acceptable within the tested ranges. In conclusion, the results of the evaluation showed the performance of CELL-DYN Ruby to be good.

  12. What We All (Supposedly) Know about the Poor: A Critical Discourse Analysis of Ruby Payne's "Framework"

    Science.gov (United States)

    Dworin, Joel E.; Bomer, Randy

    2008-01-01

    This article discusses a professional development text by Ruby Payne that claims to inform teachers about the lives and minds of children from poor households. We use Critical Discourse Analysis (Fairclough, 1995; Gee, 2005; Rogers, Malancharuvil-Berkes, & Mosley, 2005) to examine how the author enlists readers' participation in deficit…

  13. 75 FR 66779 - Ruby Lake National Wildlife Refuge, Elko and White Pine Counties, NV; Comprehensive Conservation...

    Science.gov (United States)

    2010-10-29

    ... observation and photography, and environmental education and interpretation. We will review and update the CCP... than 200 springs emanating from the base of the Ruby Mountains provide life-sustaining water to the 39..., photography, interpretation, environmental education, waterfowl hunting, and recreational fishing....

  14. The Push and the Pull: Deficit Models, Ruby Payne, and Becoming a "Warm Demander"

    Science.gov (United States)

    Boucher, Michael L.; Helfenbein, Robert J.

    2015-01-01

    Despite a caveat at the end of "A Framework for Understanding Poverty"(1996/2005), Ruby Payne's deficit model has led researchers to criticize her effect on White pre-service teaching students (Smiley and Helfenbein in "Multicult Perspect" 13(1):5-15, 2011; Gorski in "Educ Leadersh" 65:32-36, 2008a, "Equity…

  15. New sapphire and ruby components and their manufacture using diamond abrasives

    Science.gov (United States)

    Sauser, D.

    The properties of synthetic aluminum oxides (sapphire and ruby) and their applications in watchmaking (watch bearings and watchglasses) and as hard-wearing components such as centering devices for optical fibres and water jet nozzles for material cutting are discussed. Examples are given of the use of diamonds tools for machining such components, including sawing, drilling, grinding and polishing operations.

  16. Skin pigmentation and texture changes after hair removal with the normal-mode ruby laser.

    Science.gov (United States)

    Haedersdal, M; Egekvist, H; Efsen, J; Bjerring, P

    1999-11-01

    Promising clinical results have been obtained with the normal mode ruby laser for removal of unwanted hair. Melanin within the hair follicles is thought to act as target for the ruby laser pulses, whereas epidermal melanin is thought to be a competitive chromophore, responsible for potential side effects. This study aimed (i) to objectify postoperative changes in skin pigmentation and texture and (ii) to evaluate the importance of variations in preoperative skin pigmentation for the development of side effects 12 weeks after 1 treatment with the normal-mode ruby laser. A total of 17 volunteers (skin types I-IV) were laser-treated in the hairy pubic region (n = 51 test areas). A shaved test area served as control. Skin reflectance spectroscopical measurements, 3-dimensional surface contour analysis and ultrasonography objectified postoperative changes in skin pigmentation and texture. Blinded clinical assessments revealed postoperative hyperpigmentation (2% of test areas) and hypopigmentation (10%), whereas no textural changes were seen. Reflectance spectroscopically-determined pigmentary changes depended on the degree of preoperative skin pigmentation, fairly pigmented skin types experiencing subclinical hyperpigmentation and darkly pigmented skin types experiencing subclinical hypopigmentation. Three-dimensional surface profilometry documented similar pre- and postoperative surface contour parameters, indicating that the skin surface texture is preserved after laser exposure. Ultrasonography revealed similar skin thicknesses in laser-exposed and untreated control areas. It is concluded that normal-mode ruby laser treatment is safe for hair removal in skin types I-IV.

  17. Cyclotron resonance maser experiments in a bifilar helical waveguide

    Science.gov (United States)

    Aharony; Drori; Jerby

    2000-11-01

    Oscillator and amplifier cyclotron-resonance-maser (CRM) experiments in a spiral bifilar waveguide are presented in this paper. The slow-wave CRM device employs a low-energy low-current electron beam (2-12 keV, approximately 0.5 A). The pitch angle of the helical waveguide is relatively small; hence, the phase velocity in this waveguide, V(ph) congruent with0.8c (where c is the speed of light), is much faster than the axial velocity of the electrons, V(ez)traveling-wave-tube-type interactions are eliminated in this device. According to the CRM theory, the dominant effect in this operating regime, V(ez)2%). The wide tunable range of this CRM device due to the nondispersive bifilar helix is discussed.

  18. Entropy production and thermalization in the one-atom maser

    Science.gov (United States)

    Solano-Carrillo, E.

    2016-12-01

    In the configuration in which two-level atoms with an initial thermal distribution of their states are sent in succession to a cavity sustaining a single mode of electromagnetic radiation, one atom leaving the cavity as the next one enters it (as in the one-atom maser), Jaynes and Cummings showed that the steady state of the field, when many atoms have traversed the cavity, is thermal with a temperature different than that of the atoms in the off-resonant situation. Having an interaction between two subsystems which maintains them at different temperatures was then understood as leading to an apparent violation of energy conservation. Here we show, by calculating the quantum entropy production in the system, that this difference of temperatures is consistent with having the subsystems adiabatically insulated from each other as the steady state is approached. At resonance the insulation is removed and equilibration of the temperatures is achieved.

  19. Electron Cyclotron Maser Emissions from Evolving Fast Electron Beams

    CERN Document Server

    Tang, J F; Chen, L; Zhao, G Q; Tan, C M

    2016-01-01

    Fast electron beams (FEBs) are common products of solar active phenomena. Solar radio bursts are an important diagnostic tool in the understanding of FEBs as well as the solar plasma environment in which they are propagating along solar magnetic fields. In particular, the evolutions of the energy spectrum and velocity distribution of FEBs due to the interaction with the ambient plasma and field when propagating can significantly influence the efficiency and property of their emissions. In this paper, we discuss some possible evolutions of the energy spectrum and velocity distribution of FEBs due to the energy loss processes and the pitch-angle effect caused by the magnetic field inhomogeneity, and analyze the effects of these evolutions on electron cyclotron maser (ECM) emission, which is one of the most important mechanisms of producing solar radio bursts by FEBs. The results show that the growth rates all decrease with the energy loss factor $Q$, but increase with the magnetic mirror ratio $\\sigma$ as well ...

  20. Active nuclear spin maser oscillation with double cell

    Directory of Open Access Journals (Sweden)

    Hikota E.

    2014-03-01

    Full Text Available Uncertainty in the frequency precision of the planned experiment to search for a 129Xe atomic electric dipole moment is dominated by drifts in the frequency shift due to contact interaction of 129Xe with polarized Rb valence electrons. In order to suppress the frequency shift, a double-cell geometry has been adopted for the confinement of 129Xe gas. A new process has been identified to take part in the optical detection of spin precession. The parameters controlling the oscillation of the maser in this new double-cell arrangement were optimized. As a result, the frequency shift has been reduced by a factor of 10 or more from the former single-cell geometry.

  1. Microwave signal processing in two-frequency domain for ROF systems implementation: training course

    Science.gov (United States)

    Morozov, Oleg G.; Morozov, Gennady A.

    2014-04-01

    This article is presented materials from two tutorials: "Optical two-frequency domain reflectometry1, 2" and "Microwave technologies in industry, living systems and telecommunications3". These materials were prepared for master training courses and listed in the "SPIE Optical Education Directory" for 2013/2014. The main its theme is microwave photonics. Microwave photonics has been defined as the study of photonic devices operating at microwave frequencies and their application to microwave and optical systems. Its initial rationale was to use the advantages of photonic technologies to provide functions in microwave systems that are very complex or even impossible to carry out directly in the radiofrequency domain. But microwave photonics is also succeeding in incorporating a variety of techniques used in microwave engineering to improve the performance of photonic communication networks and systems. Three parts of this chapter are devoted to applications and construction principles of systems forming microwave photonic filters, measuring instantaneous frequency of microwave heterodyne signals and characterizing stimulated Mandelstam- Brillouin scattering spectrum in ROF systems. The main emphasis is on the use of the two-frequency symmetric radiation, generated by the Il'in-Morozov's method4, in given systems. It is forming radiation for the synthesis of optical filters coefficients, it's application and processing determine the increase in the signal-to-noise ratio during heterodyne frequencies monitoring and characterization of nonlinear effects spectrum.

  2. High-resolution VLBA Observations of Three 7 mm SiO Masers toward VX Sgr at Five Epochs

    Science.gov (United States)

    Su, J. B.; Shen, Z.-Q.; Chen, X.; Yi, Jiyune; Jiang, D. R.; Yun, Y. J.

    2012-07-01

    VX Sgr is a red supergiant at an adopted distance of 1.6 kpc with intense 43 GHz SiO maser emission. In this paper, we present the high-resolution very long baseline interferometry (VLBI) observations of SiO masers toward VX Sgr at five epochs. We used the Very Long Baseline Array to map the J = 1→0 (v = 1, 2) 28SiO masers and confirmed a ring-like structure. In the first two epochs, the v = 1 masers form a ring, but v = 2 maser spots residing only in the southern and northern regions do not form a complete ring. In the third epoch, the two masers are distributed in a ring structure and the v = 2 masers are a bit closer to the central star. In the last two epochs, many new maser spots appear and overlap each other. These overlapping maser spots can be related to the shock waves and reflect the collisional pumping. We compare the observations with the pumping models and speculate that the real pumping mechanism may be complex in VX Sgr and vary with time. The J = 1→0 (v = 0) 29SiO line emission is also detected, but is too weak to produce any VLBI map.

  3. Quantum and Classical Effects in the Two-Frequency Kicked Rotor with Variable Initial Phase

    CERN Document Server

    Mullins, T G; Sadgrove, M P; Hoogerland, M D; Parkins, A S; Leonhardt, R

    2004-01-01

    We present an investigation into effects exhibited by the two-frequency kicked rotor. Experiments were performed and in addition quantum and classical dynamics were simulated and compared with the experimental results. The experiments involved pulsing the optical standing wave with two pulsing periods of differing frequencies and variable initial phase offset. The ratio of pulsing periods was sampled for rational and irrational values for different experimental runs. In this paper we present these results and examine the measured momentum distributions for the cause of any structures that are seen in the energy as the initial phase offset is changed. Irrational ratios exhibit no significant quantum effects, whereas rational ratios show dynamical localisation (DL) for certain values of the initial phase. However, most of the observed structure is found to be due to classical effects, in particular KAM boundaries, and is therefore not of uniquely quantum origin.

  4. A new method using orthogonal two-frequency grating in online 3D measurement

    Science.gov (United States)

    Peng, Kuang; Cao, Yiping; Wu, Yingchun; Lu, Mingteng

    2016-09-01

    In online 3D measurement, a new method using orthogonal two-frequency grating based on Phase Measuring Profilometry(PMP) is proposed. The modulation of the entire measured object is used to match pixels and this proposed method successfully resolves the contradiction of the demand for different frequency fringes between the extraction of the modulation information and the phase unwrapping. The high-frequency fringe is used to catch the better modulation patterns for pixel matching, and the low-frequency fringe is used to calculate the phase distribution and avoid phase unwrapping error. In addition, to extract the better modulation patterns for pixel matching, the flat filtering window replaces the circular filtering window to avoid the spectrum aliasing phenomenon. The simulations and experiments show its feasibility.

  5. High-frequency signal generation using 1550 nm VCSEL subject to two-frequency optical injection

    Science.gov (United States)

    Consoli, Antonio; Quirce, Ana; Valle, Angel; Esquivias, Ignacio; Pesquera, Luis; García Tijero, Jose Manuel

    2013-03-01

    We experimentally investigate high-frequency microwave signal generation using a 1550 nm single-mode VCSEL subject to two-frequency optical injection. We first consider a situation in which the injected signals come from two similar VCSELs. The polarization of the injected light is parallel to that of the injected VCSEL. We obtain that the VCSEL can be locked to one of the injected signals, but the observed microwave signal is originated by beating at the photodetector. In a second situation we consider injected signals that come from two external cavity tunable lasers with a significant increase of the injected power with respect to the VCSEL-by-VCSEL injection case. The polarization of the injected light is orthogonal to that of the free-running slave VCSEL. We show that in this case it is possible to generate a microwave signal inside the VCSEL cavity.

  6. Properties of Maser-generated Alfvén wave in a Large Laboratory Device

    Science.gov (United States)

    Zhu, Ziyan; Dorfman, Seth; Carter, Troy; Morales, George; Clark, Mary; Rossi, Giovanni

    2016-10-01

    This research is motivated by the investigations of the natural Alfvén wave maser, which refers to the resonant amplification of Alfvén wave in the earth-surrounding plasmas. A resonant cavity that results from applying a locally non-uniform magnetic field to a plasma source region between the anode and cathode of the Large Plasma Device creates the maser. In this research, a lanthanum hexaboride (LaB6)) cathode is used as the plasma source. Above an excitation threshold, selective amplification produces a highly coherent, large amplitude Alfvén wave that propagates out of the resonator through a semitransparent mesh anode into the plasma column where the magnetic field is uniform. The excitation threshold depends on the discharge voltage, and it increases as background magnetic field strength increases; this threshold influences the maser behaviors, including amplitude modulations. The maser with LaB6 source has m = 1 mode and exhibits a right-handed rotation, which is consistent with the electron diamagnetic drift rotation, supporting the possibility of a drift Alfvén wave maser. To distinguish between drift and shear Alfvén waves, a new experiment with the maser cavity excited by a driving circuit was performed. This allows us to access low frequencies (compared to ω*) that cannot be spontaneously driven. The dispersion relation of this driven maser is under investigation. The experimental results will motivate future Alfvén wave study in laboratory devices and thus help better understand space plasma physics such as testing the theory of Alfvén-wave-induced heating of stellar atmosphere. Work supported by the U.S. Department of Energy Office of Science.

  7. Propagation of the two-frequency coherence function in an inhomogeneous background random medium

    Science.gov (United States)

    Kalugin, Alexander; Bronshtein, Alexander; Mazar, Reuven

    2004-07-01

    The spatial and temporal structures of time-dependent signals can be appreciably affected by random changes of the parameters of the medium characteristic of almost all geophysical environments. The dispersive properties of random media cause distortions in the propagating signal, particularly in pulse broadening and time delay. When there is also spatial variation of the background refractive index, the observer can be accessed by a number of background rays. In order to compute the pulse characteristics along each separate ray, there is a need to know the behaviour of the two-frequency mutual coherence function. In this work, we formulate the equation of the two-frequency mutual coherence function along a curved background ray trajectory. To solve this equation, a recently developed reference-wave method is applied. This method is based on embedding the problem into a higher dimensional space and is accompanied by the introduction of additional coordinates. Choosing a proper transform of the extended coordinate system allows us to emphasize 'fast' and 'slow' varying coordinates which are consequently normalized to the scales specific to a given type of problem. Such scaling usually reveals the important expansion parameters defined as ratios of the characteristic scales and allows us to present the proper ordering of terms in the desired equation. The performance of the main order solution is demonstrated for the homogeneous background case when the transverse structure function of the medium can be approximated by a quadratic term. This article is dedicated to the memory of Professor Reuven Mazar, a top notch scientist, whose creativity influenced many random media researchers. Professor Mazar passed away suddenly a few weeks before the publication of this paper.

  8. SiO Masers around WX Psc Mapped with the KVN and VERA Array (KaVA)

    Science.gov (United States)

    Yun, Youngjoo; Cho, Se-Hyung; Imai, Hiroshi; Kim, Jaeheon; Asaki, Yoshiharu; Chibueze, James O.; Choi, Yoon Kyung; Dodson, Richard; Kim, Dong-Jin; Kusuno, Kozue; Matsumoto, Naoko; Min, Cheulhong; Oyadomari, Miyako; Rioja, María J.; Yoon, Dong-Hwan; Byun, Do-Young; Chung, Hyunsoo; Chung, Moon-Hee; Hagiwara, Yoshiaki; Han, Myoung-Hee; Han, Seog-Tae; Hirota, Tomoya; Honma, Mareki; Hwang, Jung-Wook; Je, Do-Heung; Jike, Takaaki; Jung, Dong-Kyu; Jung, Taehyun; Kang, Ji-Hyun; Kang, Jiman; Kang, Yong-Woo; Kan-ya, Yukitoshi; Kanaguchi, Masahiro; Kawaguchi, Noriyuki; Kim, Bong Gyu; Ryoung Kim, Hyo; Kim, Hyun-Goo; Kim, Jongsoo; Kim, Kee-Tae; Kim, Mikyoung; Kobayashi, Hideyuki; Kono, Yusuke; Kurayama, Tomoharu; Lee, Changhoon; Lee, Jeewon; Lee, Jeong Ae; Lee, Jung-Won; Lee, Sang Hyun; Lee, Sang-Sung; Lyo, A.-Ran; Minh, Young Chol; Oh, Chungsik; Oh, Se-Jin; Oyama, Tomoaki; Roh, Duk-Gyoo; Sawada-Satoh, Satoko; Shibata, Katsunori M.; Sohn, Bong Won; Song, Min-Gyu; Tamura, Yoshiaki; Wi, Seog-Oh; Yeom, Jae-Hwan

    2016-05-01

    We present the first images of the v = 1 and v = 2 J = 1 → 0 SiO maser lines taken with KaVA, i.e., the combined array of the Korean Very Long Baseline Interferometry (VLBI) Network and the VLBI Exploration of Radio Astrometry (VERA), toward the OH/IR star WX Psc. The combination of long and short antenna baselines enabled us to detect a large number of maser spots, which exhibit a typical ring-like structure in both the v = 1 and v = 2 J = 1 → 0 SiO masers as those that have been found in previous VLBI observational results of WX Psc. The relative alignment of the v = 1 and v = 2 SiO maser spots are precisely derived from astrometric analysis, due to the absolute coordinates of the reference maser spot that were well determined in an independent astrometric observation with VERA. The superposition of the v = 1 and v = 2 maser spot maps shows a good spatial correlation between the v = 1 and v = 2 SiO maser features. Nevertheless, it is also shown that the v = 2 SiO maser spot is distributed in an inner region compared to the v = 1 SiO maser by about 0.5 mas on average. These results provide good support for the recent theoretical studies of the SiO maser pumping, in which both the collisional and the radiative pumping predict the strong spatial correlation and the small spatial discrepancy between the v = 1 and v = 2 SiO maser.

  9. Springs inventory and estimate of inflow contributions for Ruby Lake National Wildlife Refuge, May 21 -23rd, 2012

    Data.gov (United States)

    US Fish and Wildlife Service, Department of the Interior — Springs at Ruby Lake National Wildlife Refuge were visited in May of 2012 to verify locations of springs from previous mapping efforts and to estimate the total...

  10. Energetic improvement with micro turbines of biogas generated in Rubis WWTP; Aprovechamiento energetico con microturbinas del biogas generado en la EDAR de Rubi

    Energy Technology Data Exchange (ETDEWEB)

    Moragas, L.; Robuste, J.; Vicente, M.; Pozo, A.; Blasco, M.

    2009-07-01

    The WWTP of Rubi (Barcelona, Spain) treats 22.950 m{sup 3}/day by activated sludge system, with mesophilic anaerobic digestion of primary and secondary sludges with a capacity of 3.500 m{sup 3}. Generated biogas is applied by means of indirect heating to digesters at 37 degree centigrade. To improve the energetic performance 2 micro turbines of 65 kW each were installed, with a 29% of unitary electric performance. After 5 months a third turbine was installed to generate more energy in peak hours. this solutions has shown to be very flexible, with reasonable technology and costs. (Author)

  11. Methanol masers probing the ordered magnetic field of W75N

    Science.gov (United States)

    Surcis, G.; Vlemmings, W. H. T.; Dodson, R.; van Langevelde, H. J.

    2009-11-01

    Context: The role of magnetic fields during the protostellar phase of high-mass star-formation is a debated topic. In particular, it is still unclear how magnetic fields influence the formation and dynamic of disks and outflows. Most current information on magnetic fields close to high-mass protostars comes from H2O and OH maser observations. Recently, the first 6.7 GHz methanol maser polarization observations were made, and they reveal strong and ordered magnetic fields. Aims: The morphology of the magnetic field during high-mass star-formation needs to be investigated on small scales, which can only be done using very long baseline interferometry observations. The massive star-forming region W75N contains three radio sources and associated masers, while a large-scale molecular bipolar outflow is also present. Polarization observations of the 6.7 GHz methanol masers at high angular resolution probe the strength and structure of the magnetic field and determine its relation to the outflow. Methods: Eight of the European VLBI network antennas were used to measure the linear polarization and Zeeman-splitting of the 6.7 GHz methanol masers in the star-forming region W75N. Results: We detected 10 methanol maser features, 4 of which were undetected in previous work. All arise near the source VLA 1 of W75N. The linear polarization of the masers reveals a tightly ordered magnetic field over more than 2000 AU around VLA 1 that is exactly aligned with the large-scale molecular outflow. This is consistent with the twisted magnetic field model proposed for explaining dust polarization observations. The Zeeman-splitting measured on 3 of the maser features indicates a dynamically important magnetic field in the maser region of the order of 50 mG. We suggest VLA 1 is the powering sources of the bipolar outflow. Member of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne.

  12. Ruby-sapphire-spinel mineralization in marble of the middle and southern Urals: Geology, mineralogy, and genesis

    Science.gov (United States)

    Kisin, A. Yu.; Murzin, V. V.; Tomilina, A. V.; Pritchin, M. E.

    2016-07-01

    Ruby and spinel occurrences hosted in marble on the eastern slope of the Urals are considered. Ruby- and spinel-bearing marble is a specific rock in granite-gneiss complexes of the East Ural Megazone, which formed at the Late Paleozoic collision stage of the evolution of the Urals. Organogenic marine limestone is the protolith of the marble. No relict sedimentary bedding has been retained in the marble. The observed banding is a secondary phenomenon related to crystallization and is controlled by flow cleavage. Magnesian metasomatism of limestone with the formation of fine-grained dolomite enriched in Cr, V, Ti, Mn, Cu, Zn, Ga, and REE took place at the prograde stage of metamorphism. Dedolomitization of rocks with the formation of background calcite marble also developed at the prograde stage. Mg-calcite marble with spinel and ruby of the first type formed in the metamorphic fluid circulation zone. Magnesian metasomatism with the formation of bicarbonate marble with ruby, pink sapphire, and spinel of the second type developed at the early retrograde stage. The formation of mica-bearing mineralized zones with corundum and spinel of the third type controlled by cleavage fractures is related to the pneumatolytic-hydrothermal stage. The data on ruby-bearing marble in the Urals may be used for forecasting and prospecting of ruby and sapphire deposits hosted in marble worldwide.

  13. Performance evaluation of the Abbott CELL-DYN Ruby and the Sysmex XT-2000i haematology analysers.

    Science.gov (United States)

    Leers, M P G; Goertz, H; Feller, A; Hoffmann, J J M L

    2011-02-01

    Two mid-range haematology analysers (Abbott CELL-DYN Ruby and Sysmex XT-2000i) were evaluated to determine their analytical performance and workflow efficiency in the haematology laboratory. In total 418 samples were processed for determining equivalence of complete blood count (CBC) measurements, and 100 for reticulocyte comparison. Blood smears served for assessing the agreement of the differential counts. Inter-instrument agreement for most parameters was good although small numbers of discrepancies were observed. Systematic biases were found for mean cell volume, reticulocytes, platelets and mean platelet volume. CELL-DYN Ruby WBC differentials were obtained with all samples while the XT-2000i suppressed differentials partially or completely in 13 samples (3.1%). WBC subpopulation counts were otherwise in good agreement with no major outliers. Following first-pass CBC/differential analysis, 88 (21%) of XT-2000i samples required further analyser processing compared to 18 (4.3%) for the CELL-DYN Ruby. Smear referrals for suspected WBC/nucleated red blood cells and platelet abnormalities were indicated for 106 (25.4%) and 95 (22.7%) of the XT-2000i and CELL-DYN Ruby samples respectively. Flagging efficiencies for both analysers were found to be similar. The Sysmex XT-2000i and Abbott CELL-DYN Ruby analysers have broadly comparable analytical performance, but the CELL-DYN Ruby showed superior first-pass efficiency. © 2010 Blackwell Publishing Ltd.

  14. Discovery of the Zeeman Effect in the 44 GHz Class I methanol maser line

    CERN Document Server

    Sarma, A P

    2011-01-01

    We report the discovery of the Zeeman effect in the 44 GHz Class I methanol maser line. The observations were carried out with 22 antennas of the EVLA toward a star forming region in OMC-2. Based on our adopted Zeeman splitting factor of z = 1.0 Hz/mG, we detect a line of sight magnetic field of 18.4 +/- 1.1 mG toward this source. Since such 44 GHz methanol masers arise from shocks in the outflows of star forming regions, we can relate our measurement of the post-shock magnetic field to field strengths indicated by species tracing pre-shock regions, and thus characterize the large scale magnetic field. Moreover, since Class I masers trace regions more remote from the star forming core than Class II masers, and possibly earlier phases, magnetic fields detected in 6.7 GHz Class II and 36 GHz and 44 GHz Class I methanol maser lines together offer the potential of providing a more complete picture of the magnetic field. This motivates further observations at high angular resolution to find the positional relation...

  15. Generation of the jovian radio emission by the maser cyclotron instability: first lessons from JUNO

    Science.gov (United States)

    Louarn, Philippe; Allegrini, Frederic; Kurth, WilliamS.; Valek, Philips. W.; McComas, Dave; Bagenal, Fran; Bolton, Scott; Connerney, John; Ebert, Robert W.; Levin, Steven; Szalay, Jamey; Wilson, Robert; Zink, Jenna; André, Nicolas; Imai, Masafumi

    2017-04-01

    Using JUNO plasma and wave observations (JADE and Waves instruments), the scenario for the generation of jovian auroral radio emissions are analyzed. The sources of radiation are identified by localized intensifications of the radio flux at frequencies close to the electron gyrofrequency. Not surprisingly, it is shown that the cyclotron maser instability is perfectly adapted to the plasma conditions prevailing in the radio sources. However, it appears that different forms of activation of the cyclotron maser are observed. For radiation at hectometric wavelengths (one of the main emissions), pronounced loss-cones in the electron distribution functions are likely the source of free energy. The sources would be extended over several thousand km in directions traverse to the magnetic field. The applications of the theory reveals that sufficient growth rates are obtained from the distributions functions that are actually measured by JADE. This differs from the Earth scenario for which 'trapped' distribution functions drive the maser. More localized sources are also observed, possibly linked to local acceleration process. These examples may present analogies with the 'Earth' scenario, with other forms of free energy than the loss-cone. A first lesson of these direct in-situ JADE and RPWS observations is thus to confirm the maser cyclotron scenario with, however, conditions for the wave amplification and detailed maser processes that appear to be different than at Earth.

  16. A Catalog of Methanol Masers in Massive Star-forming Regions. III. The Molecular Outflow Sample

    CERN Document Server

    Gómez-Ruiz, A I; Araya, E D; Hofner, P; Loinard, L

    2016-01-01

    We present an interferometric survey of the 44 GHz class I methanol maser transition toward a sample of 69 sources consisting of High Mass Protostellar Object candidates and Ultracompact (UC) H II regions. We found a 38% detection rate (16 of 42) in the HMPO candidates and a 54% detection rate (13 of 24) for the regions with ionized gas. This result indicates that class I methanol maser emission is more common toward more evolved young stellar objects of our sample. Comparing with similar interferometric data sets, our observations show narrower linewidths, likely due to our higher spatial resolution. Based on a comparison between molecular outflow tracers and the maser positions, we find several cases where the masers appear to be located at the outflow interface with the surrounding core. Unlike previous surveys, we also find several cases where the masers appear to be located close to the base of the molecular outflow, although we can not discard projection effects. This and other surveys of class I methan...

  17. Distance and proper motion measurement of water masers in Shapless 269 IRS 2w

    CERN Document Server

    Asaki, Yoshiharu; Sobolev, Andrej Mikhailovich; Parfenov, Sergey Yurievich

    2014-01-01

    We present astrometric analysis of archival data of water masers in the star-forming region Sharpless 269 (S269) IRS 2w, observed with the VLBI Exploration of Radio Astrometry. An annual parallax of one of the bright maser features in this region was previously reported to be 0.189+/-0.008 milliarcsecond (mas) using part of the same archival data as we used. However, we found that this maser feature is not the best to represent the annual parallax to S269 IRS 2w because the morphology is remarkably elongated in the east-west direction. For this study we have selected another maser feature showing simpler morphology. This makes the new annual parallax estimate more credible. Our newly obtained annual parallax is 0.247+/-0.034 mas, corresponding to 4.05+0.65-0.49 kpc. This value is well consistent with the 3.7-3.8 kpc obtained using the kinematic distance estimates and photometric distance modulus. We considered two hypotheses for the water maser spatial distribution, a bipolar outflow and an expanding ring, in...

  18. Models of class II methanol masers based on improved molecular data

    CERN Document Server

    Cragg, D M; Godfrey, P D

    2005-01-01

    The class II masers of methanol are associated with the early stages of formation of high-mass stars. Modelling of these dense, dusty environments has demonstrated that pumping by infrared radiation can account for the observed masers. Collisions with other molecules in the ambient gas also play a significant role, but have not been well modelled in the past. Here we examine the effects on the maser models of newly available collision rate coefficients for methanol. The new collision data does not alter which transitions become masers in the models, but does influence their brightness and the conditions under which they switch on and off. At gas temperatures above 100 K the effects are broadly consistent with a reduction in the overall collision cross-section. This means, for example, that a slightly higher gas density than identified previously can account for most of the observed masers in W3(OH). We have also examined the effects of including more excited state energy levels in the models, and find that th...

  19. The Megamaser Cosmology Project.IX. Black hole masses for three maser galaxies

    CERN Document Server

    Gao, F; Reid, M J; Condon, J J; Greene, J E; Henkel, C; Impellizzeri, C M V; Lo, K Y; Kuo, C Y; Pesce, D W; Wagner, J; Zhao, W

    2016-01-01

    As part of the Megamaser Cosmology Project (MCP), we present VLBI maps of nuclear water masers toward five galaxies. The masers originate in sub-parsec circumnuclear disks. For three of the galaxies, we fit Keplerian rotation curves to estimate their supermassive black hole (SMBH) masses, and determine (2.9 $\\pm$ 0.3) $\\times~10^{6}M_\\odot$ for J0437+2456, (1.7 $\\pm$ 0.1) $\\times~10^{7}M_\\odot$ for ESO 558$-$G009, and (1.1 $\\pm$ 0.2) $\\times~10^{7}M_\\odot$ for NGC 5495. In the other two galaxies, Mrk 1029 and NGC 1320, the geometry and dynamics are more complicated and preclude robust black hole mass estimates. Including our new results, we compiled a list of 15 VLBI-confirmed disk maser galaxies with robust SMBH mass measurements. With this sample, we confirm the empirical relation of $R_{out} \\propto 0.3 M_{SMBH}$ reported in Wardle & Yusef-Zadeh (2012). We also find a tentative correlation between maser disk outer radii and WISE luminosity. We find no correlations of maser disk size with X-ray 2-10 keV...

  20. Response of circumnuclear water masers to luminosity changes in an active galactic nucleus

    CERN Document Server

    Neufeld, D A

    2000-01-01

    Circumnuclear water masers can respond in two ways to changes in the luminosity of an active galactic nucleus. First, an increase in the X-ray luminosity can lead to an increase in the maser emissivity; and second, an increase in the intrinsic bolometric luminosity may result in a temporary decrease in the difference between the gas and dust temperature and a consequent decrease in the maser output. Whilst the latter effect can occur over a period shorter than the thermal timescale, the former effect cannot. Quantitative estimates of the response of the water maser emissivity to changes in either the X-ray or bolometric luminosity are presented, together with estimates of the relevant timescales. Either mechanism could account for recent observations by Gallimore et al. which suggest that the water maser variability in two widely separated regions of the circumnuclear gas in NGC 1068 have been coordinated by a signal from the active nucleus. For either mechanism, a minimum H2 density ~ 1.E+8 cm-3 is needed to...

  1. The electron-cyclotron maser instability as a source of plasma radiation. [Solar radio bursts

    Science.gov (United States)

    Winglee, R. M.; Dulk, G. A.

    1986-01-01

    The generation of continuum bursts from the sun at dm and m wavelengths (in particular, type IV bursts) via the electron-cyclotron-maser instability is examined. The maser instability can be driven by an electron distribution with either a loss-cone anisotropy or a peak at large pitch angles. For omega(p)/Omega(e) much greater than 1, the maser emission is produced by electrons interacting through a harmonic (cyclotron) resonance and is electrostatic, being in the upper hybrid mode at frequencies approximately equal to omega(p). Coalescence processes are required to convert the electrostatic waves into transverse radiation which can escape from the source region. Whether the resultant spectrum is nearly a smooth continuum or has a zebra-stripe pattern (both of which occur in type IV bursts) depends on the form of the electron distribution, inhomogeneities in the density and magnetic field, and whether the maser reaches saturation. For at least the case of some type IV dm bursts with fine structure, comparison with observations seems to indicate that the electrons producing the emission are more likely to have a loss-cone distribution, and that the maser instability is not at saturation.

  2. The magnetic field around late-type stars revealed by the circumstellar H2O masers

    CERN Document Server

    Vlemmings, W H T; Diamond, P J

    2005-01-01

    Through polarization observations, circumstellar masers are excellent probes of the magnetic field in the envelopes of late-type stars. Whereas observations of the polarization of the SiO masers close to the star and on the OH masers much further out were fairly commonplace, observations of the magnetic field strength in the intermediate density and temperature region where the 22 GHz water masers occur have only recently become possible. Here we present the analysis of the circular polarization, due to Zeeman splitting, of the water masers around the Mira variable stars U Her and U Ori and the supergiant VX Sgr. We present an upper limit of the field around U Her that is lower but consistent with previous measurements, reflecting possible changes in the circumstellar envelope. The field strengths around U Ori and VX Sgr are shown to be of the order of several Gauss. Moreover, we show for the first time that large scale magnetic fields permeate the circumstellar envelopes of an evolved star; the polarization ...

  3. Probing the circumstellar environments of very young low-mass stars using water masers

    Science.gov (United States)

    Terebey, S.; Vogel, S. N.; Myers, P. C.

    1992-01-01

    The VLA is used to search nearby very young low-mass stars for water maser emission. The sample consists of 26 low-luminosity IRAS sources embedded in dense molecular cores, a class of sources suspected to be newly forming low-mass stars on the order of a few hundred thousand years old. Three sources were detected. High spatial resolution maps show the region of maser emission is generally confined to an area smaller than about 0.5 arcsec near the star, and the velocities of individual components span intervals ranging from 20 to 40 km/s. It is inferred from the fact that the maser velocities are too large to be due to gravitational motions in at least two of the sources that the masers are associated with the winds from the young low-mass stars. A comparison of the high spatial resolution maser data to lower-resolution CO data shows no evidence for higher collimation close to the star; the stellar wind cavity appears to have similar collimation at 10 exp 15 cm as at 10 exp 7 to 10 exp 18 cm.

  4. HIGH-RESOLUTION IMAGING OF WATER MASER EMISSION IN THE ACTIVE GALAXIES NGC 6240 AND M51

    Energy Technology Data Exchange (ETDEWEB)

    Hagiwara, Yoshiaki [Natural Science Laboratory, Toyo University, 5-28-20, Hakusan, Bunkyo-ku, Tokyo 112-8606 (Japan); Edwards, Philip G., E-mail: yhagiwara@toyo.jp, E-mail: Philip.Edwards@csiro.au [CSIRO Astronomy and Space Science, P.O. Box 76, Epping NSW 1710 (Australia)

    2015-12-20

    We present the results of observations of 22 GHz H{sub 2}O maser emission in NGC 6240 and M51 made with the Karl G. Jansky Very Large Array. Two major H{sub 2}O maser features and several minor features are detected toward the southern nucleus of NGC 6240. These features are redshifted by about 300 km s{sup −1} from the galaxy’s systemic velocity and remain unresolved at the synthesized beam size. A combination of our two-epoch observations and published data reveals an apparent correlation between the strength of the maser and the 22 GHz radio continuum emission, implying that the maser excitation relates to the activity of an active galactic nucleus in the southern nucleus rather than star-forming activity. The star-forming galaxy M51 hosts H{sub 2}O maser emission in the center of the galaxy; however, the origin of the maser has been an open question. We report the first detection of 22 GHz nuclear radio continuum emission in M51. The continuum emission is co-located with the maser position, which indicates that the maser arises from nuclear active galactic nucleus-activity and not from star-forming activity in the galaxy.

  5. Ruby fluorescence lifetime measurements for temperature determinations at high (p, T)

    Science.gov (United States)

    Bauer, Johannes D.; Bayarjargal, Lkhamsuren; Winkler, Björn

    2012-06-01

    The lifetime of the ruby R1 fluorescence line was measured as a function of pressure (up to about 20 GPa) and temperature (550 K) in an externally heated diamond anvil cell (DAC). At constant temperatures, the lifetime is increasing linearly with increasing pressure. The slope of the pressure dependence is constant up to a temperature of 450 K and it is decreasing at higher temperatures. At constant pressure, the lifetime is exponentially decreasing with increasing temperature. The (p, T)-dependence can be parametrized by the combination of a linear and an exponential function. This allows an accurate p, T-determination by the combination of fluorescence spectroscopy using Sm2+-doped strontium tetraborate and lifetime measurements of ruby, as the energy of the Sm2+ fluorescence is nearly temperature-independent.

  6. MVC ARCHITECTURE: A COMPARITIVE STUDY BETWEEN RUBY ON RAILS AND LARAVEL

    Directory of Open Access Journals (Sweden)

    Archit Verma

    2014-10-01

    Full Text Available Model View Controller (MVC architecture is a standard design pattern used in website design or in web application development. It divides a given software application into three interconnected parts, so as to separate internal representations of information from the ways that information is presented to or accepted from the user. The central component, the model, consists of application data, business rules, logic and functions. A view can be any output representation of information, such as a chart or a diagram. Multiple views of the same information are possible, such as a bar chart for management and a tabular view for accountants. The third part, the controller, accepts input and converts it to commands for the model or view. In this the two popular MVC Frameworks, Laravel which uses the language PHP and Ruby on Rails which uses the language Ruby are compared and analyzed.

  7. Treatment of tattoos by Q-switched ruby laser. A dose-response study

    Energy Technology Data Exchange (ETDEWEB)

    Taylor, C.R.; Gange, R.W.; Dover, J.S.; Flotte, T.J.; Gonzalez, E.; Michaud, N.; Anderson, R.R. (Massachusetts General Hospital, Boston (USA))

    1990-07-01

    Tattoo treatment with Q-switched ruby laser pulses (694 nm, 40 to 80 nanoseconds) was studied by clinical assessment and light and electron microscopy. Fifty-seven blue-black tattoos or portions thereof (35 amateur and 22 professional) were irradiated with 1.5 to 8.0 J/cm2 at a mean interval of 3 weeks. Substantial lightening or total clearing occurred in 18 (78%) of 23 amateur tattoos and 3 (23%) of 13 professional tattoos in which the protocol was completed. Response was related to exposure dose. Scarring occurred in one case, and persistent confettilike hypopigmentation was frequent. Optimal fluence was 4 to 8 J/cm2. Clinicohistologic correlation was poor. Q-switched ruby laser pulses can provide an effective treatment for tattoos.

  8. Extragalactic H2O Megamaser Sources:Central Black Holes,Nuclear X-ray and Maser Emissions

    Institute of Scientific and Technical Information of China (English)

    Jiang-Bo Su; Jiang-Shui Zhang; Jun-Hui Fan

    2008-01-01

    Extragalactic H2O megamasers are typically found within the innermost few parsecs of active galaxy nuclei (AGN) and the maser emission is considered to be excited most likely by the X-ray irradiation of the AGN.We investigate a comprehensive sample of extragalactic H2O masers in a sample of 38 maser host AGN to check potential correlations of the megamaser emission with parameters of the AGN,such as X-ray luminosity and black hole (BH) masses.We find a relation between the maser luminosities and BH masses,LH2O∝ M3.64-0.4 BH,which supports basically the theoretical prediction.The relation between the maser emission and X-ray emission is also confirmed.

  9. Generation of Interstellar Class Ⅱ 72-81A+ and 72-81A-Methanol Masers

    Institute of Scientific and Technical Information of China (English)

    2007-01-01

    New methanol maser lines at 72→63A-(86.6 GHz) and 72→63A+(86.9GHz) together with two candidate methanol maser lines at 72→81A-(80.99 GHz) and 72→81A+(111.29GHz) have been detected in W3(OH). We use a pumping mechanism, i.e., methanol masers without population inversion, to explain the formation of weak methanol masers of 72→81A+and 72→81A-. We explain well why the line-shape of the transition 72→81A+is not typical. A similar argument can be applied to the A-type level system 72A→, 63A-and 81A-, as well as to the 72→81A- 80.99 GHz masers.

  10. Under the Radar: The First Woman in Radio Astronomy, Ruby Payne-Scott

    Science.gov (United States)

    Miller Goss, W.

    2012-05-01

    Under the Radar, the First Woman in Radio Astronomy, Ruby Payne-Scott W. Miller Goss, NRAO Socorro NM Ruby Payne-Scott (1912-1981) was an eminent Australian scientist who made major contributions to the WWII radar effort (CSIR) from 1941 to 1945. In late 1945, she pioneered radio astronomy efforts at Dover Heights in Sydney, Australia at a beautiful cliff top overlooking the Tasman Sea. Again at Dover Heights, Payne-Scott carried out the first interferometry in radio astronomy using an Australian Army radar antenna as a radio telescope at sun-rise, 26 January 1946. She continued these ground breaking activities until 1951. Ruby Payne-Scott played a major role in discovering and elucidating the properties of Type III bursts from the sun, the most common of the five classes of transient phenomena from the solar corona. These bursts are one of the most intensively studied forms of radio emission in all of astronomy. She is also one of the inventors of aperture synthesis in radio astronomy. I examine her career at the University of Sydney and her conflicts with the CSIR hierarchy concerning the rights of women in the work place, specifically equal wages and the lack of permanent status for married women. I also explore her membership in the Communist Party of Australia as well as her partially released Australian Scientific Intelligence Organization file. Payne-Scott’s role as a major participant in the flourishing radio astronomy research of the post war era remains a remarkable story. She had a number of strong collaborations with the pioneers of early radio astronomy in Australia: Pawsey, Mills, Christiansen, Bolton and Little. I am currently working on a popular version of the Payne-Scott story; “Making Waves, The Story of Ruby Payne-Scott: Australian Pioneer Radio Astronomer” will be published in 2013 by Springer in the Astronomers’ Universe Series.

  11. Advances in Trace Element “Fingerprinting” of Gem Corundum, Ruby and Sapphire, Mogok Area, Myanmar

    Directory of Open Access Journals (Sweden)

    F. Lin Sutherland

    2014-12-01

    Full Text Available Mogok gem corundum samples from twelve localities were analyzed for trace element signatures (LA-ICP-MS method and oxygen isotope values (δ18O, by laser fluorination. The study augmented earlier findings on Mogok gem suites that suggested the Mogok tract forms a high vanadium gem corundum area and also identified rare alluvial ruby and sapphire grains characterised by unusually high silicon, calcium and gallium, presence of noticeable boron, tin and niobium and very low iron, titanium and magnesium contents. Oxygen isotope values (δ18O for the ruby and high Si-Ca-Ga corundum (20‰–25‰ and for sapphire (10‰–20‰ indicate typical crustal values, with values >20‰ being typical of carbonate genesis. The high Si-Ca-Ga ruby has high chromium (up to 3.2 wt % Cr and gallium (up to 0. 08 wt % Ga compared to most Mogok ruby (<2 wt % Cr; <0.02 wt % Ga. In trace element ratio plots the Si-Ca-Ga-rich corundum falls into separate fields from the typical Mogok metamorphic fields. The high Ga/Mg ratios (46–521 lie well within the magmatic range (>6, and with other features suggest a potential skarn-like, carbonate-related genesis with a high degree of magmatic fluid input The overall trace element results widen the range of different signatures identified within Mogok gem corundum suites and indicate complex genesis. The expanded geochemical platform, related to a variety of metamorphic, metasomatic and magmatic sources, now provides a wider base for geographic typing of Mogok gem corundum suites. It allows more detailed comparisons with suites from other deposits and will assist identification of Mogok gem corundum sources used in jewelry.

  12. Measurement of R Line Fluorescence in Ruby Using the Diamond Anvil Cell at Low Temperature

    Institute of Scientific and Technical Information of China (English)

    XU Li-Wen; CHE Rong-Zheng; JIN Chang-Qing

    2000-01-01

    Using our custom-built high-pressure cryostat we have performed the measurements of the R line fluorescence of ruby in the diamond anvil cell from room temperature down to 90K. The maximum pressure was 11.1 GPa. By computer curve fitting, different equations have been found for functions of wavenumber versus temperature between ambient pressure and 2.7 GPa. The changes of the shape and linewidth of R lines were observed.

  13. Ruby on rails开发框架的实际应用

    Institute of Scientific and Technical Information of China (English)

    刘继

    2015-01-01

    Ruby on Rails是一个可以开发、部署、维护web应用程序使其变得简单的框架。是一个相对较新的Web应用程序框架,构建在Ruby语言之上。它有其自己的MVC设计模式,能够非常清晰、专一的构建项目架构。

  14. Refractive Q-switching of a ruby laser by a moving plasma

    Energy Technology Data Exchange (ETDEWEB)

    Dembinski, M.; John, P.K.

    1982-10-15

    A ruby laser was Q-switched by means of a plasma. The plasma, which had a density of up to 10/sup 18/ cm/sup -3/, was produced in an electromagnetic shock tube. The density gradient created by the reflected plasma was large enough to produce measurable refraction of the laser beam. The laser cavity, which was initially misaligned, attained perfect alignment when the plasma was introduced into the cavity.

  15. Galactic masers: kinematics, spiral structure and the disk dynamic state

    CERN Document Server

    Rastorguev, A S; Dambis, A K; Utkin, N D; Bajkova, A T; Bobylev, V V

    2016-01-01

    We investigate the kinematics of 131 Milky-Way masers associated with star-forming regions and with trigonometric parallaxes measured by Very Large Baseline Radio Interferometry. We developed a new algorithm for computing the structural and kinematic parameters of the Galactic disk, which implements the currently most comprehensive version of the statistical-parallax technique. To take into account the variation of the form and size of the ellipsoid of residual velocities as a function of Galactocentric distance, we assume that radial velocity dispersion is related to disk surface density and apply the Jeans hydrodynamic equations. We compute the Galactic rotation curve over the Galactocentric distance interval from 3 to 14 kpc and find the local circular rotation velocity to be 243 +/- 10 km/s, and we also determine a full set of kinematical parameters, including the parameters of the four-armed spiral pattern with the pitch angle i ~ -10.45 +/- 0.30 deg. The galactocentric distance is found to be R0 = 8.40 ...

  16. An in vivo comparison of two frequency-based electronic apex locators.

    Science.gov (United States)

    Welk, Aaron R; Baumgartner, J Craig; Marshall, J Gordon

    2003-08-01

    The purpose of this study was to compare the accuracy of a two-frequency (Root ZX) and a five-frequency (Endo Analyzer Model 8005) electronic apex locator under clinical conditions. Thirty-two teeth planned for extraction were used. The coronal portion of each canal was flared using Gates Glidden drills and Orifice Shapers. The canals were irrigated with 2.6% sodium hypochlorite. A K-type file was used to determine a separate working length in each canal using the electronic apex locators. The teeth were extracted and the apical 4 mm of each root canal was exposed along the long axis of the tooth. Photographic slides of each canal were projected and the file position in relation to the minor diameter was determined by two investigators. The mean distance between the electronic apex locator working length and minor diameter was 1.03 mm for the Endo Analyzer and 0.19 mm for the Root ZX. A paired sample t test showed that the Endo Analyzer had significantly longer readings beyond the minor diameter than the Root ZX (p locate the minor diameter (+/- 0.5 mm) was 90.7% for the Root ZX and 34.4% for the Endo Analyzer Model 8005.

  17. Parametrically Excited Surface Waves Two-Frequency Forcing, Normal Form Symmetries, and Pattern Selection

    CERN Document Server

    Silber, M; Silber, Mary; Skeldon, Anne C.

    1999-01-01

    Motivated by experimental observations of exotic standing wave patterns in the two-frequency Faraday experiment, we investigate the role of normal form symmetries in the pattern selection problem. With forcing frequency components in ratio m/n, where m and n are co-prime integers, there is the possibility that both harmonic and subharmonic waves may lose stability simultaneously, each with a different wavenumber. We focus on this situation and compare the case where the harmonic waves have a longer wavelength than the subharmonic waves with the case where the harmonic waves have a shorter wavelength. We show that in the former case a normal form transformation can be used to remove all quadratic terms from the amplitude equations governing the relevant resonant triad interactions. Thus the role of resonant triads in the pattern selection problem is greatly diminished in this situation. We verify our general results within the example of one-dimensional surface wave solutions of the Zhang-Vinals model of the t...

  18. Intermittent maser flare around the high-mass young stellar object G353.273+0.641

    Science.gov (United States)

    Motogi, Kazuhito; Sorai, Kazuo; Fujisawa, Kenta; Sugiyama, Koichiro; Honma, Mareki

    2012-07-01

    The water maser site associated with G353.273+0.641 is classified as a dominant blueshifted H2O maser, which shows an extremely wide velocity range (+/- 100 km s-1) with almost all flux concentrated in the highly blueshifted emission. The previous study has proposed that this peculiar H2O maser site is excited by a pole-on jet from high mass protostellar object. We report on the monitoring of 22-GHz H2O maser emission from G353.273+0.641 with the VLBI Exploration of Radio Astrometry (VERA) and the Tomakamai 11-m radio telescope. Our VLBI imaging has shown that all maser features are distributed within a very small area of 200 × 200 au2, in spite of the wide velocity range (> 100 km s-1). The light curve obtained by weekly single-dish monitoring shows notably intermittent variation. We have detected three maser flares during three years. Frequent VLBI monitoring has revealed that these flare activities have been accompanied by a significant change of the maser alignments. We have also detected synchronized linear acceleration (-5 km s-1yr-1) of two isolated velocity components, suggesting a lower-limit momentum rate of 10-3 M⊙ km s-1yr-1 for the maser acceleration. All our results support the previously proposed pole-on jet scenario, and finally, a radio jet itself has been detected in our follow-up ATCA observation. If highly intermittent maser flares directly reflect episodic jet-launchings, G353.273+0.641 and similar dominant blueshifted water maser sources can be suitable targets for a time-resolved study of high mass protostellar jet.

  19. The Motion of Water Masers in the Pre-Planetary Nebula IRAS 16342-3814

    CERN Document Server

    Claussen, M J; Morris, M R

    2008-01-01

    We present high angular resolution observations, using the Very Long Baseline Array (VLBA) of the NRAO, of the high-velocity water masers toward the "water-fountain" pre-planetary nebula, IRAS 16342-3814. The detailed structure of the water masers appears to be that of bow shocks on either side of a highly collimated jet. The proper motions of the water masers are approximately equal to the radial velocities; the three-dimensional velocities are approximately +/-180 km/s, which leads to a very short dynamical time-scale of ~100 years. Although we do not find direct evidence for precession of the fast collimated jet, there may be indirect evidence for such precession.

  20. EVN observations of 6.7 GHz methanol masers from Medicina survey

    CERN Document Server

    Voronkov, M A; Palagi, F; Tofani, G

    2002-01-01

    We report VLBI observations of methanol masers in the brightest 5(1)-6(0) A+ transition at 6.7 GHz in NGC 281W, 18151-1208 and 19388+2357. Using the fringe rate method absolute positions were obtained for all observed sources. A linear ordered structure with a velocity gradient was revealed in NGC 281W. Under assumption that such structure is an edge-on Keplerian disk around the central object with a mass of 30Msun located at a distance of 3.5 kpc from the Sun, we estimated that methanol masers are situated at the distance about 400 a.u. from the center of the disk. A second epoch of observations was reported for L1206, GL2789 and 20062+3550. The upper limits on the relative motions of maser spots are estimated to be 4.7 km/s and 28 km/s for L1206 and GL2789 respectively.

  1. Circular Polarization of Water Masers in the Circumstellar Envelopes of Late Type Stars

    CERN Document Server

    Vlemmings, W H T; Van Langevelde, H J

    2002-01-01

    We present circular polarization measurements of circumstellar H_2O masers. The circular polarization detected in the (6_{16}-5_{23}) rotational transition of the H_{2}O maser can be attributed to Zeeman splitting in the intermediate temperature and density regime. The magnetic fields are derived using a general, LTE Zeeman analysis as well as a full radiative transfer method (non-LTE), which includes a treatment of all hyperfine components simultaneously as well as the effects of saturation and unequal populations of the magnetic substates. The differences and relevances of these interpretations are discussed extensively. The field strengths are compared with previous detections of the magnetic field on the SiO and OH masers. We show that the magnetic pressure dominates the thermal pressure by a factor of 20 or more.

  2. Low-cost electron-gun pulser for table-top maser experiments

    Science.gov (United States)

    Grinberg, V.; Jerby, E.; Shahadi, A.

    1995-04-01

    A simple 10 kV electron-gun pulser for small-scale maser experiments is presented. This low-cost pulser has operated successfully in various table-top cyclotron-resonance maser (CRM) and free-electron maser (FEM) experiments. It consists of a low-voltage capacitor bank, an SCR control circuit and a transformer bank (car ignition coils) connected directly to the e-gun. The pulser produces a current of 3 A at 10 kV voltage in a Gaussian like shape of 1 ms pulse width. The voltage sweep during the pulse provides a useful tool to locate resonances of CRM and FEM interactions. Analytical expressions for the pulser design and experimental measurements are presented.

  3. Measuring the Distance of VX Sagittarii with SiO Maser Proper Motions

    Institute of Scientific and Technical Information of China (English)

    2007-01-01

    We report on 43 GHz v=1, J=1-0 SiO maser proper motions in the circumstellar envelope of the M-type semi-regular variable star VX Sgr, observed by Very Long Baseline Array (VLBA) at 3 epochs during 1999 April-May. Applying the statistical parallax analysis to these proper motions, we estimated a distance of VX Sgr of 1.57±0.27 kpc, which is consistent with that based on the proper motions of H2O masers, or on the assumption that VX Sgr belongs to the Sgr OB1 association. At this distance, VX Sgr can be classified as a red supergiant. Comparing the statistical parallax method with those of model fitting and annual parallax, we think that the statistical parallax method may be a good way of estimating SiO maser distances at present.

  4. Magnetic fields around late-type stars using water maser observations

    CERN Document Server

    Vlemmings, W H T; Diamond, P J

    2005-01-01

    We present the analysis of the circular polarization, due to Zeeman splitting, of the water masers around a sample of late-type stars to determine the magnetic fields in their circumstellar envelopes. The magnetic field strengths in the water maser regions around the Mira variable stars U Ori and U Her are shown to be several Gauss while those of the supergiants S Per, NML Cyg and VY CMa are several hundred mG. We also show that large scale magnetic fields permeate the CSE of an evolved star; the polarization of the water masers around VX Sgr reveals a dipole field structure. We shortly discuss the coupling of the magnetic field with the stellar outflow, as such fields could possibly be the cause of distinctly aspherical mass-loss and the resulting aspherical planetary nebulae.

  5. Measuring the Distance of VX Sagittarii with SiO Maser Proper Motions

    Science.gov (United States)

    Chen, Xi; Shen, Zhi-Qiang; Xu, Ye

    2007-08-01

    We report on 43 GHz v=1, J=1--0 SiO maser proper motions in the circumstellar envelope of the M-type semi-regular variable star VX Sgr, observed by Very Long Baseline Array (VLBA) at 3 epochs during 1999 April--May. Applying the statistical parallax analysis to these proper motions, we estimated a distance of VX Sgr of 1.57±0.27 kpc, which is consistent with that based on the proper motions of H2O masers, or on the assumption that VX Sgr belongs to the Sgr OB1 association. At this distance, VX Sgr can be classified as a red supergiant. Comparing the statistical parallax method with those of model fitting and annual parallax, we think that the statistical parallax method may be a good way of estimating SiO maser distances at present.

  6. Development of cross-correlation spectrometry and the coherent structures of maser sources

    CERN Document Server

    Takefuji, Kazuhiro; Sekido, Mamoru

    2016-01-01

    We have developed a new method of data processing for radio telescope observation data to measure time-dependent temporal coherence, and we named it cross-correlation spectrometry (XCS). XCS is an autocorrelation procedure that expands time lags over the integration time and is applied to data obtained from a single-dish observation. The temporal coherence property of received signals is enhanced by XCS. We tested the XCS technique using the data of strong H2O masers in W3 (H2O), W49N and W75N. We obtained the temporal coherent lengths of the maser emission to be 17.95 $\\pm$ 0.33 {\\mu}s, 26.89 $\\pm$ 0.49 {\\mu}s and 15.95 $\\pm$ 0.46 {\\mu}s for W3 (H2O), W49N and W75N, respectively. These results may indicate the existence of a coherent astrophysical maser.

  7. Development of cross-correlation spectrometry and the coherent structures of maser sources

    Science.gov (United States)

    Takefuji, Kazuhiro; Imai, Hiroshi; Sekido, Mamoru

    2016-10-01

    We have developed a new method of data processing for radio telescope observation data to measure time-dependent temporal coherence, and we have named it "cross-correlation spectrometry" (XCS). XCS is an autocorrelation procedure that expands time lags over the integration time and is applied to data obtained from a single-dish observation. The temporal coherence property of received signals is enhanced by XCS. We tested the XCS technique using the data of strong H2O masers in W 3 (H2O), W 49 N, and W 75 N. We obtained the temporal coherent lengths of the maser emission to be 17.95 ± 0.33 μs, 26.89 ± 0.49 μs, and 15.95 ± 0.46 μs for W 3 (H2O), W 49 N, and W 75 N, respectively. These results may indicate the existence of a coherent astrophysical maser.

  8. The Circumstellar Environment of Evolved Stars as Revealed by Studies of Circumstellar Water Masers

    Science.gov (United States)

    Marvel, K.

    1997-11-01

    This dissertation presents the results of a multi-epoch very long baseline interferometric (VLBI) study of water masers located in the extended atmospheres of seven evolved stars. The research was performed using the Very Long Baseline Array and Very Large Array of the National Radio Astronomy Observatory. Water masers are found to exist in the atmospheres of evolved, oxygen-rich stars where a population inversion of the rotational transition at 22 GHz can be maintained by collisional pumping. The masers are identified as individual pockets or filaments of gas, which have good velocity coherence and may be imaged using radio interferometry. Stellar winds are initiated in these sources by dust formation and acceleration of the gas through momentum coupling. The typical wind speeds in the region of the water masers are 10 to 20 \\kms. The water masers in several evolved stars (VY CMa, VX Sgr, S Per, U Her, IK Tau, RX Boo and NML Cyg) have been observed at three epochs and exhibit proper motions consistent with the assumed source distances and the measured outflow velocity in the water maser region. Estimates of the distance to the sources using statistical approximation are in agreement with the currently accepted distances to the stars. The following stars had reliable distances determined using proper motion data: S Per (2.3 +/- 0.5 kpc), VY CMa (1.4 +/- 0.2 kpc), VX Sgr (1.4 +/- 0.3 kpc). An upper limit for the distance of NML Cyg was obtained ( 3.5 kpc). The remaining stars had too few maser detections (RX BOO, IK Tau) or were not strong enough at all epochs (U Her) to self-calibrate using the VLBA. A detailed kinematic model was used to describe the flow motions of the gas in the maser region. The regions are found to be complex and not well modeled by uniform radial outflow, radial outflow with rotation, or radial outflow with acceleration. The reasons for this are explored and include the probable presence of anisotropic velocity fields induced through non

  9. The OH Maser Line Receiving System for the Urumqi 25m Radio Telescope

    Institute of Scientific and Technical Information of China (English)

    Hong-Bo Zhang; Jarken Esimbek; Jian-Jun Zhou; Xing-Wu Zhen; Xi-Zhen Zhang; Wen-Jie Yang

    2005-01-01

    A maser spectral line system is newly implemented on the Urumqi 25m Radio Telescope. The system consists mainly of a cooling receiver and a 4096channels digital correlation spectrometer. The frequency resolution of the spectrometer at the maximum signal bandwidth of 80 MHz is 19.5 kHz. After careful calibrations observation at the 1665MHz OH maser emission was made towards a number of sources, including W49N and W75N. The observed results demonstrate that the digital correlation spectrometer is suitable for astronomical spectral line observations.

  10. Resonant electron diffusion as a saturation process of the synchrotron maser instability. [of auroral kilometric radiation

    Science.gov (United States)

    Lee, M. C.; Kuo, S. P.

    1986-01-01

    The theory of resonant electron diffusion as an effective saturation process of the auroral kilometric radiation has been formulated. The auroral kilometric radiation is assumed to be amplified by the synchrotron maser instability that is driven by an electron distribution of the loss-cone type. The calculated intensity of the saturated radiation is found to have a significantly lower value in comparison with that caused by the quasi-linear diffusion process as an alternative saturation process. This indicates that resonant electron diffusion dominates over quasi-linear diffusion in saturating the synchrotron maser instability.

  11. Probing AGN with Masers and X-Rays-SAX Proposals

    Science.gov (United States)

    Wilkes, Belinda J.; White, Nicholas (Technical Monitor)

    2001-01-01

    We have made BeppoSAX observations of the Seyfert 2/1.9 galaxy ESO103-G35, which contains a nuclear maser source and is known to be heavily absorbed in the X-rays. Analysis of the X-ray spectra observed by SAX in October 1996 and 1997 yields an energy index = 0.74 +/- 0.07, typical of Seyfert galaxies and consistent with earlier observations of this source. The strong, soft X-ray absorption has a column density, N_H of (1.79 +/- 0.09)E23 cmE-02, again consistent with earlier results. The best fitting spectrum is that of a power law with a high energy cutoff at 29 +/- 10 keV, a cold (E=6.3 +/- 0.1 keV, rest frame), marginally resolved (sigma = 0.35 +/- 0.14 keV, FWHM approximately (31 +/- 12)E03 km/s) FeKalpha line with EW 290 +100 -80 eV (1996) and a mildly ionized Fe K-edge at 7.37 +0.15 -0.21 keV, tau 0.24 +0.06 -0.09. The Fe Kalpha line and cold absorption are consistent with origin in a accretion disk/torus through which our line-of-sight passes at a radial distance of approximately 0.01 pc. The Fe K-edge is mildly ionized suggesting the presence of ionized gas probably in the inner accretion disk, close to the central source or in a separate warm absorber. The data quality is too low to distinguish between these possibilities but the edge-on geometry implied by the water maser emission favors the former. Comparison with earlier observations of ESO103-G35 shows little/no change in spectral parameters while the flux changes by factors of a few on timescales of a few months. The 2-10 keV flux decreased by a factor of approximately 2.7 between Oct 1996 and Oct 1997 with no detectable change in the count rate greater than 20 keV (i.e. the PDS data). Spectral fits to the combined datasets indicate either a significant hardening of the spectrum (energy index approximately 0.5) or an approximate constant or delayed response reflection component. The high energy cutoff (29 +/- 10 keV) is lower than the typical approximately 300 keV values seen in Seyfert galaxies. A

  12. Hybrid planar free-electron maser in the magnetoresonance regime

    Directory of Open Access Journals (Sweden)

    Vitaliy A. Goryashko

    2009-10-01

    Full Text Available We study the operation regime of a hybrid planar free-electron maser (FEM amplifier near the magnetoresonant value of the uniform longitudinal (guide magnetic field. Using analytical expressions for individual test electron trajectories and normal frequencies of their three-dimensional oscillations in the magnetostatic field of the hybrid planar FEM, an analytical condition of chaotization of motion is established and shown to be given by the Chirikov resonance-overlap criterion applied to the normal undulator and cyclotron frequencies with respect to the coupling induced by the undulator magnetic field. It is also shown analytically that, in spite of the well-known drop for the exact magnetoresonance, the gain attains its maximal value in the zone of regular dynamics slightly above the magnetoresonant value of the guide magnetic field. Under the condition of undulator resonance, it is practically independent of the amplitude of the undulator magnetic field and the wavelength of amplified signal. To account for space-charge effects, we propose a theoretical model of a weakly relativistic FEM, which accommodates not only potential but also rotational parts of the nonradiated electromagnetic field of a moving charged particle. It turns out that the rotational part of nonradiated field diminishes the defocusing influence of the potential part on the beam bunching. Numeric simulation of the nonlinear stage of amplification is fulfilled, taking into consideration adiabatic entrance of the electron beam to the interaction region and initial electron velocity spread. We find that nonradiated field and initial electron velocity spread do not influence essentially the efficiency of hybrid planar FEM amplification if parameters of the beam-microwave interaction correspond to the operational regime in the zone of regular dynamics near the magnetoresonance.

  13. VLBI observations of the 6.7 and 12.2 GHz methanol masers associated with NGC 6334F

    CERN Document Server

    Ellingsen, S P; Diamond, P J; McCulloch, P M; Amy, S W; Beasley, A J; Ferris, R H; Gough, R G; King, E A; Lovell, J E J; Reynolds, J E; Tzioumis, A K; Troup, E R; Wark, R M; Wieringa, M H

    1996-01-01

    We present milliarcsecond resolution images of the 6.7 and 12.2 GHz methanol maser emission associated with the well-known star formation region NGC 6334F. The images agree well with previous lower resolution observations, but detect approximately double the number of spots seen in the earlier work. Comparison of the relative positions of the 6.7 and 12.2 GHz maser spots shows that five of them are coincident to within the positional accuracy of these observations (approximately 4 milli-arcsec). Menten et al. (1992) observed similar positional coincidence for W3(OH) and in each case the flux density of the 6.7 GHz maser spot was greater than that of the 12.2 GHz methanol maser spot. However, for NGC 6334F several of the coincident maser spots have a larger flux density at 12.2 GHz than at 6.7 GHz. We also detected several 12.2 GHz methanol maser spots with no coincident 6.7 GHz emission. This implies that, although the 6.7 GHz methanol masers usually have a greater flux density than their 12.2 GHz counterpart...

  14. Discovery of periodic and alternating flares of the methanol and water masers in G107.298+5.639

    CERN Document Server

    Szymczak, M; Wolak, P; Bartkiewicz, A; Gawronski, M

    2016-01-01

    Methanol and water vapour masers are signposts of early stages of high-mass star formation but it is generally thought that due to different excitation processes they probe distinct parts of stellar environments. Here we present observations of the intermediate-mass young stellar object G107.298+5.639, revealing for the first time that 34.4 d flares of the 6.7 GHz methanol maser emission alternate with flares of individual features of the 22 GHz water maser. High angular resolution data reveal that a few components of both maser species showing periodic behaviour coincide in position and velocity and all the periodic water maser components appear in the methanol maser region of size of 360 au. The maser flares could be caused by variations in the infrared radiation field induced by cyclic accretion instabilities in a circumstellar or protobinary disc. The observations do not support either the stellar pulsations or the seed photon flux variations as the underlying mechanisms of the periodicity in the source.

  15. The mid-infrared environments of 6.7 GHz Methanol Masers from the Methanol Multi-Beam Survey

    CERN Document Server

    Gallaway, M; Lucas, P W; Fuller, G A; Caswell, J L; Green, J A; Voronkov, M A; Breen, S L; Quinn, L; Ellingsen, S P; Avison, A; Ward-Thompson, D; Cox, J

    2012-01-01

    We present a study of the mid-infrared environments and association with star formation tracers of 6.7 GHz methanol masers taken from the Methanol Multi-Beam (MMB) Survey. Our ultimate goal is to establish the mass of the host star and its evolutionary stage for each maser site. As a first step, the GLIMPSE survey of the Galactic Plane is utilised to investigate the environment of 776 methanol masers and we find that while the majority of the masers are associated with mid-infrared counterparts, a significant fraction (17%) are not associated with any detectable mid-infrared emission. A number of the maser counterparts are clearly extended with respect to the GLIMPSE point spread function and we implement an adaptive non-circular aperture photometry (ANCAP) technique to determine the fluxes of the maser counterparts. The ANCAP technique doubles the number of masers with flux information at all four wavelengths compared to the number of the corresponding counterparts obtained from the GLIMPSE Point Source Cata...

  16. Geology, geochemistry and Ar Ar geochronology of the Nangimali ruby deposit, Nanga Parbat Himalaya (Azad Kashmir, Pakistan)

    Science.gov (United States)

    Pêcher, A.; Giuliani, G.; Garnier, V.; Maluski, H.; Kausar, A. B.; Malik, R. H.; Muntaz, H. R.

    2002-12-01

    The Nangimali ruby deposit in the southern part of the Nanga Parbat Himalaya, has been investigated through field work, geochemistry, stable and radiogenic isotopes. It outcrops in the Shontar valley in a large north-vergent syncline consisting of high-grade metamorphic gneisses capped by a metasedimentary series dominated by marbles and amphibolites. The ore-body is stratiform. Ruby is found within 0.1-2 cm thick shear-veinlets and gash veins cutting dolomitic marbles and carbonate-bearing bands. The marbles of the Nangimali Formation display restricted ranges in δ18O (from 23.6 to 27.6‰ relative to SMOW) and in δ13C (from -1.9 to 2.6‰ relative to PDB). Fluid infiltration along the shear-zone in the marble has no effect on the isotopic signatures of the carbonates. Fluids are metamorphic and CO 2 is derived from the decarbonation of marbles. Mass-balance and geochemical analyses suggest that the mobilisation by the fluids of aluminium and chromium in the marbles is sufficient to enable the formation of ruby in the shear-zone. Rubies have been indirectly dated using a stepwise 40Ar- 39Ar laser heating technique on syngenetic phlogopites. The Miocene age records a Neogene cooling in the South of the Nanga Parbat massif and a minimum formation age for ruby of 16 Ma.

  17. A 20-year H2O maser monitoring program with the Medicina 32-m telescope

    Science.gov (United States)

    Brand, J.; Felli, M.; Cesaroni, R.; Codella, C.; Comoretto, G.; Di Franco, S.; Massi, F.; Moscadelli, L.; Nesti, R.; Olmi, L.; Palagi, F.; Palla, F.; Panella, D.; Valdettaro, R.

    2007-03-01

    The Arcetri/Bologna H2O maser group has been monitoring the 1.3-cm water maser emission from a sample of 43 star-forming regions (SFRs) and 22 late-type stars for about 20 years at a sampling rate of 4-5 observations each year, using the 32-m Medicina Radio Telescope (HPBW 1.‧9 at 22 GHz). For the late-type stars we observe representative samples of OH/IR-stars, Mira's, semi-regular variables, and supergiants. The SFR-sample spans a large interval in FIR luminosity of the associated Young Stellar Object (YSO), from 20 L to 1.5 × 106 L, and offers a unique data base for the study of the long-term (years) variability of the maser emission in regions of star formation. This presentation concerns only the masers in SFRs. The information obtained from single-dish monitoring is complementary to what is extracted from higher-resolution (VLA and VLBI) observations, and can better explore the velocity domain and the long-term variability therein. We characterize the variability of the sources in various ways and we study how it depends on the luminosity and other properties of the associated YSO and its environment.

  18. First mm-wave generation in the FOM free electron maser

    NARCIS (Netherlands)

    Verhoeven, A. G. A.; Bongers, W. A.; Bratman, V. L.; Caplan, M.; Denisov, G. G.; van der Geer, C. A. J.; Manintveld, P.; Poelman, A. J.; Plomp, J.; Savilov, A. V.; Smeets, P. H. M.; Sterk, A. B.; Urbanus, W. H.

    1999-01-01

    A free electron maser (FEM) has been built as a pilot mm-wave source for applications on future fusion research devices such as international tokamak experimental reactor (ITER), A unique feature of the Dutch FEM is the possibility to tune the frequency over the entire range from 130 to 260 GHz at a

  19. Water in Massive protostellar objects: first detection of THz water maser and water inner abundance.

    Science.gov (United States)

    Herpin, Fabrice

    2014-10-01

    The formation massive stars is still not well understood. Despite numerous water line observations with Herschel telescope, over a broad range of energies, in most of the observed sources the WISH-KP (Water In Star-forming regions with Herschel, Co-PI: F. Herpin) observations were not able to trace the emission from the hot core. Moreover, water maser model predict that several THz water maser should be detectable in these objects. We aim to detect for the first time the THz maser lines o-H2O 8(2,7)- 7(3,4) at 1296.41106 GHz and p-H2O 7(2,6)- 6(3,3) at 1440.78167 GHz as predicted by the model. We propose two sources for a northern flight as first priority and two other sources for a possible southern flight. This will 1) constrain the maser theory, 2) constrain the physical conditions and water abundance in the inner layers of the prostellar environnement. In addition, we will use the p-H2O 3(3,1)- 4(0,4) thermal line at 1893.68651 GHz (L2 channel) in order to probe the physical conditions and water abundance in the inner layers of the prostellar objects where HIFI-Herschel has partially failed.

  20. A survey for water maser emission towards planetary nebulae. New detection in IRAS 17347-3139

    CERN Document Server

    De Gregorio-Monsalvo, I; Anglada, G; Cesaroni, R; Miranda, L F; Gómez, J F; Torrelles, J M; Gregorio-Monsalvo, Itziar de; Gomez, Yolanda; Anglada, Guillem; Cesaroni, Riccardo; Miranda, Luis F.; Gomez, Jose F.; Torrelles, Jose M.

    2004-01-01

    We report on a water maser survey towards a sample of 27 planetary nebulae (PNe) using the Robledo de Chavela and Medicina single-dish antennas, as well as the Very Large Array (VLA). Two detections have been obtained: the already known water maser emission in K 3-35, and a new cluster of masers in IRAS 17347-3139. This low rate of detections is compatible with the short life-time of water molecules in PNe (~100 yr). The water maser cluster at IRAS 17347-3139 are distributed on a ellipse of size ~ 0.2" x 0.1", spatially associated with compact 1.3 cm continuum emission (simultaneously observed with the VLA). From archive VLA continuum data at 4.9, 8.4, and 14.9 GHz, a spectral index alpha = 0.76 +- 0.03 is derived for this radio source, which is consistent with either a partially optically thick ionized region or with an ionized wind. However, the latter scenario can be ruled out on mass-loss considerations, thus indicating that this source is probably a young PN. The spatial distribution and the radial veloc...

  1. Low-loss electron beam transport in a high-power, electrostatic free-electron maser

    NARCIS (Netherlands)

    Valentini, M.; van der Geer, C. A. J.; Verhoeven, A. G. A.; van der Wiel, M. J.; Urbanus, W. H.

    1997-01-01

    At the FOM Institute for Plasma Physics ''Rijnhuizen'', The Netherlands, the commissioning of a high-power, electrostatic free-electron maser is in progress. The design target is the generation of 1 MW microwave power in the frequency range 130-260 GHz. The foreseen application o

  2. Formaldehyde and H110a observations towards 6.7 GHz methanol maser sources

    CERN Document Server

    Okoh, Daniel; Zhou, Jian Jun; Tang, Xin Di; Chukwude, Augustine; Urama, Johnson; Okeke, Pius

    2014-01-01

    Intriguing work on observations of 4.83 GHz formaldehyde (H2CO) absorptions and 4.87 GHz H110a radio recombination lines (RRLs) towards 6.7 GHz methanol (CH3OH) maser sources is presented. Methanol masers provide ideal sites to probe the earliest stages of massive star formation, while 4.8 GHz formaldehyde absorptions are accurate probes of physical conditions in dense $(10^{3} - 10^{5} cm^{-3})$ and low temperature molecular clouds towards massive star forming regions. The work is aimed at studying feature similarities between the formaldehyde absorptions and the methanol masers so as to expand knowledge of events and physical conditions in massive star forming regions. A total of 176 methanol maser sources were observed for formaldehyde absorptions, and formaldehyde absorptions were detected 138 of them. 53 of the formaldehyde absorptions were newly detected. We noted a poor correlation between the methanol and formaldehyde intensities, an indication that the signals (though arise from about the same region...

  3. Evolution of the Water Maser Expanding Shell in W75N VLA 2

    CERN Document Server

    Kim, Jeong-Sook; Kurayama, Tomoharu; Honma, Mareki; Sasao, Tesuo; Surcis, Gabriele; Canto, Jorge; Torrelles, Jose M; Kim, Sang Joon

    2013-01-01

    We present Very Long Baseline Interferometry (VLBI) observations of 22 GHz H$_2$O masers in the high-mass star-forming region of \\objectname{W75N}, carried out with VLBI Exploration of Radio Astrometry (VERA) for three-epochs in 2007 with an angular resolution of $\\sim$ 1 mas. We detected H$_2$O maser emission toward the radio jet in VLA 1 and the expanding shell-like structure in VLA 2. .......... We have made elliptical fits to the VLA 2 H$_2$O maser shell-like structure observed in the different epochs (1999, 2005, and 2007), and found that the shell is still expanding eight years after its discovery. From the difference in the size of the semi-major axes of the fitted ellipses in the epochs 1999 ($\\simeq$ 71$\\pm$1 mas), 2005 ($\\simeq$ 97$\\pm$3 mas), and 2007 ($\\simeq$ 111$\\pm$1 mas), we estimate an average expanding velocity of $\\sim$ 5 mas yr$^{-1}$, similar to the proper motions measured in the individual H$_2$O maser features. A kinematic age of $\\sim$ 20 yr is derived for this structure. In addition, ...

  4. Discovery of periodic class II methanol masers associated with G339.986-0.425 region

    CERN Document Server

    Maswanganye, J P; Goedhart, S; Gaylard, M J

    2015-01-01

    Ten new class II methanol masers from the 6.7-GHz Methanol Multibeam survey catalogues III and IV were selected for a monitoring programme at both 6.7 and 12.2 GHz with the 26m Hartebeesthoek Radio Astronomy Observatory (HartRAO) radio telescope for two years and nine months, from August 2012 to May 2015. In the sample, only masers associated with G339.986-0.425 were found to show periodic variability at both 6.7 and 12.2 GHz. The existence of periodic variation was tested with four independent methods. The analytical method gave the best estimation of the period, which was 246 $\\pm$ 1 days. The time series of G339.986-0.425 show strong correlations across velocity channels and between the 6.7 and 12.2 GHz masers. The time delay was also measured across channels and shows structure across the spectrum which is continuous between different maser components.

  5. The z Distribution of Hydrogen Clouds and Masers with Kinematic Distances

    CERN Document Server

    Bobylev, V V

    2016-01-01

    Data on HII regions, molecular clouds, and methanol masers have been used to estimate the Sun's distance from the symmetry plane zo and the vertical disk scale height h. Kinematic distance estimates are available for all objects in these samples. The Local-arm (Orion-arm) objects are shown to affect noticeably the pattern of the z distribution. The deviations from the distribution symmetry are particularly pronounced for the sample of masers with measured trigonometric parallaxes, where the fraction of Local-arm masers is large. The situation with the sample of HII regions in the solar neighborhood is similar. We have concluded that it is better to exclude the Local arm from consideration. Based on the model of a self-gravitating isothermal disk, we have obtained the following estimates from objects located in the inner region of the Galaxy (R<= Ro): zo= -5.7+/-0.5 pc and h2=24.1+/-0.9 pc from the sample of 639 methanol masers, zo=-7.6+/-0.4 pc and h2=28.6+/-0.5 pc from 878 HII regions, zo=-10.1+/-0.5 pc a...

  6. European VLBI Network imaging of 6.7 GHz methanol masers

    CERN Document Server

    Bartkiewicz, Anna; van Langevelde, Huib J

    2016-01-01

    Methanol masers at 6.7 GHz are well known tracers of high-mass star-forming regions. However, their origin is still not clearly understood. We aimed to determine the morphology and velocity structure for a large sample of the maser emission with generally lower peak flux densities than those in previous surveys. Using the European VLBI Network we imaged the remaining sources (17) from a sample of sources that were selected from the unbiased survey using the Torun 32 m dish. Together they form a database of a total of 63 source images with high sensitivity, milliarcsecond angular resolution and very good spectral resolution for detailed studies. We studied in detail the properties of the maser clouds and calculated the mean and median values of the projected size (17.4 au and 5.5 au, respectively) as well as the FWHM of the line (0.373 km s$^{-1}$ and 0.315 km s$^{-1}$ for the mean and median values, respectively), testing whether it was consistent with Gaussian profile. We also found maser clouds with velocit...

  7. The Zeeman Effect in the 44 GHz Class I Methanol Maser Line toward DR21(OH)

    Science.gov (United States)

    Momjian, E.; Sarma, A. P.

    2017-01-01

    We report detection of the Zeeman effect in the 44 GHz Class I methanol maser line, toward the star-forming region DR21(OH). In a 219 Jy beam‑1 maser centered at an LSR velocity of 0.83 km s‑1, we find a 20-σ detection of zBlos = 53.5 ± 2.7 Hz. If 44 GHz methanol masers are excited at n ∼ 107–8 cm‑3, then the B versus n1/2 relation would imply, from comparison with Zeeman effect detections in the CN(1 ‑ 0) line toward DR21(OH), that magnetic fields traced by 44 GHz methanol masers in DR21(OH) should be ∼10 mG. Combined with our detected zBlos = 53.5 Hz, this would imply that the value of the 44 GHz methanol Zeeman splitting factor z is ∼5 Hz mG‑1. Such small values of z would not be a surprise, as the methanol molecule is non-paramagnetic, like H2O. Empirical attempts to determine z, as demonstrated, are important because there currently are no laboratory measurements or theoretically calculated values of z for the 44 GHz CH3OH transition. Data from observations of a larger number of sources are needed to make such empirical determinations robust.

  8. Ammonia and CO Outflow around 6.7 GHz Methanol Masers

    CERN Document Server

    Li, F C; Wu, Y W; Yang, J; Lu, D R; Menten, K M; Henkel, C

    2016-01-01

    Single point observations are presented in NH3 (1,1) and (2,2) inversion transitions using the Effelsberg 100 m telescope for a sample of 100 6.7 GHz methanol masers and mapping observations in the 12CO and 13CO (1-0) transitions using the PMO Delingha 13.7 m telescope for 82 sample sources with detected ammonia. A further 62 sources were selected for either 12CO or 13CO line outflow identification, producing 45 outflow candidates, 29 using 12CO and 16 using 13CO data. Twenty-two of the outflow candidates were newly identified, and 23 had trigonometric parallax distances. Physical properties were derived from ammonia lines and CO outflow parameters calculated. Histograms and statistical correlations for ammonia, CO outflow parameters, and 6.7 GHz methanol maser luminosities are also presented. No significant correlation was found between ammonia and maser luminosity. However, weak correlations were found between outflow properties and maser luminosities, which may indicate that outflows are physically associa...

  9. The Zeeman Effect in the 44 GHz Class I Methanol Maser Line toward DR21(OH)

    CERN Document Server

    Momjian, E

    2016-01-01

    We report the detection of the Zeeman effect in the 44 GHz Class I methanol maser line toward the star forming region DR21(OH). In a 219 Jy/beam maser centered at an LSR velocity of 0.83 km s$^{-1}$, we find a 20-$\\sigma$ detection of $zB_{\\text{los}} = 53.5 \\pm 2.7$ Hz. If 44 GHz methanol masers are excited at $n \\sim 10^{7-8}$ cm$^{-3}$, then the $B~vs.~n^{1/2}$ relation would imply from comparison with Zeeman effect detections in the CN($1-0$) line toward DR21(OH) that magnetic fields traced by 44 GHz methanol masers in DR21(OH) should be $\\sim$10 mG. Together with our detected $zB_{\\text{los}} = 53.5$ Hz, this would imply that the value of the 44 GHz methanol Zeeman splitting factor $z$ is $\\sim$5 Hz mG$^{-1}$. Such small values of $z$ would not be a surprise, as the methanol molecule is non paramagnetic, like H$_2$O. Empirical attempts to determine $z$, as demonstrated, are important because currently there are no laboratory measurements or theoretically calculated values of $z$ for the 44 GHz methanol t...

  10. A general catalogue of 6.7 GHz methanol masers. I: data

    CERN Document Server

    Pestalozzi, M; Booth, R

    2004-01-01

    Methanol masers are often detected in regions of intense star formation. Several studies in the last decade indicate that they may even be the earliest signpost of a high-mass star-forming region. Their powerful emission make them very good candidates for observations using both single--dish telescopes and interferometers, the latter allows detailed structural and dynamical studies of these objects. We have prepared a catalogue of all known 6.7-GHz methanol masers, discovered both by surveys that targeted possible associated objects and unbiased surveys covering a large fraction of galactic longitudes across the Galactic plane (-0.5deg <= b <= 0.5deg for most of the regions). The catalogue contains 519 sources which are listed with their kinematic (galactocentric and heliocentric) distances as well as possibly associated IR objects. We find that 6.7-GHz methanol masers clearly trace the molecular ring of our Galaxy, where most of the OB associations are located. The present list of masers also reports d...

  11. 6.7GHz Methanol Maser Associated Outflows: An evolutionary sequence

    CERN Document Server

    de Villiers, H M; Thompson, M A; Urquhart, J S; Breen, S L; Burton, M G; Ellingsen, S P; Fuller, G A; Pestalozzi, M; Voronkov, M A; Ward-Thompson, D

    2015-01-01

    We present a continuing study of a sample 44 molecular outflows, observed in 13CO lines, closely associated with 6.7GHz methanol masers, hence called Methanol Maser Associated Outflows (MMAOs). We compare MMAO properties with those of outflows from other surveys in the literature. In general, MMAOs follow similar trends, but show a deficit in number at low masses and momenta, with a corresponding higher fraction at the high end of the distributions. A similar trend is seen for the dynamical timescales of MMAOs. We argue that the lack of relatively low mass and young flows in MMAOs is due to the inherent selection-bias in the sample, i.e. its direct association with 6.7GHz methanol masers. This implies that methanol masers must switch on after the onset of outflows (hence accretion), and not before a sufficient abundance of methanol is liberated from icy dust mantles. Consequently the average dynamical age of MMAOs is older than for the general population of molecular outflows. We propose an adjusted evolution...

  12. H$_2$O Masers and Protoplanetary Disk Dynamics in IC 1396 N

    CERN Document Server

    Bayandina, O S; Kurtz, S E; Rudnitskij, G M; Alakoz, A V

    2016-01-01

    We report H$_2$O maser line observations of the bright-rimmed globule IC 1396 N using a ground-space interferometer with the 10-m RadioAstron radio telescope as the space-based element. The source was not detected on projected baselines >2.3 Earth diameters, which indicates a lower limit on the maser size of L >0.03 AU and an upper limit on the brightness temperature of 6.25 x 10$^{12}$ K. Positions and flux densities of maser spots were determined by fringe rate mapping. Multiple low-velocity features from -4.5 km/s to +0.7 km/s are seen, and two high-velocity features of V$_{LSR}$=-9.4 km/s and +4.4 km/s are found at projected distances of 157 AU and 70 AU, respectively, from the strongest low-velocity feature at V$_{LSR}$=$\\sim$0.3 km/s. Maser components from the central part of the spectrum fall into four velocity groups but into three spatial groups. Three spatial groups of low-velocity features detected in the 2014 observations are arranged in a linear structure about 200 AU in length. Two of these grou...

  13. First mm-wave generation in the FOM free electron maser

    NARCIS (Netherlands)

    Verhoeven, A. G. A.; Bongers, W. A.; Bratman, V. L.; Caplan, M.; Denisov, G. G.; van der Geer, C. A. J.; Manintveld, P.; Poelman, A. J.; Plomp, J.; Savilov, A. V.; Smeets, P. H. M.; Sterk, A. B.; Urbanus, W. H.

    1999-01-01

    A free electron maser (FEM) has been built as a pilot mm-wave source for applications on future fusion research devices such as international tokamak experimental reactor (ITER), A unique feature of the Dutch FEM is the possibility to tune the frequency over the entire range from 130 to 260 GHz at

  14. EVOLUTION OF THE WATER MASER EXPANDING SHELL IN W75N VLA 2

    Energy Technology Data Exchange (ETDEWEB)

    Kim, Jeong-Sook; Kim, Sang Joon [School of Space Science, Kyunghee University, Seocheon-dong, Giheung-si, Gyeonggi-do, 446-701 (Korea, Republic of); Kim, Soon-Wook [Korea Astronomy and Space Science Institute, 776 Daedeokdaero, Yuseong, Daejeon 305-348 (Korea, Republic of); Kurayama, Tomoharu [Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065 (Japan); Honma, Mareki [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Sasao, Tesuo [Yaeyama Star Club, Ookawa, Ishigaki, Okinawa 904-0022 (Japan); Surcis, Gabriele [Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo (Netherlands); Canto, Jorge [Instituto de Astronomia (UNAM), Apartado 70-264, 04510 Mexico D. F. (Mexico); Torrelles, Jose M., E-mail: evony@kasi.re.kr, E-mail: skim@kasi.re.kr [Instituto de Ciencias del Espacio (CSIC)-UB/IEEC, Universitat de Barcelona, Marti i Franques 1, E-08028 Barcelona (Spain)

    2013-04-10

    We present Very Long Baseline Interferometry (VLBI) observations of 22 GHz H{sub 2}O masers in the high-mass star-forming region of W75N, carried out with VLBI Exploration of Radio Astrometry (VERA) for three epochs in 2007 with an angular resolution of {approx}1 mas. We detected H{sub 2}O maser emission toward the radio jet in VLA 1 and the expanding shell-like structure in VLA 2. The spatial distribution of the H{sub 2}O masers detected with VERA and measured proper motions around VLA 1 and VLA 2 are similar to those found with previous VLBI observations in epochs 1999 and 2005, with the masers in VLA 1 mainly distributed along a linear structure parallel to the radio jet and, on the other hand, forming a shell-like structure around VLA 2. We have made elliptical fits to the VLA 2 H{sub 2}O maser shell-like structure observed in the different epochs (1999, 2005, and 2007), and found that the shell is still expanding eight years after its discovery. From the difference in the size of the semi-major axes of the fitted ellipses in epochs 1999 ({approx_equal}71 {+-} 1 mas), 2005 ({approx_equal}97 {+-} 3 mas), and 2007 ({approx_equal}111 {+-} 1 mas), we estimate an average expanding velocity of {approx}5 mas yr{sup -1}, similar to the proper motions measured in the individual H{sub 2}O maser features. A kinematic age of {approx}20 yr is derived for this structure. In addition, our VERA observations indicate an increase in the ellipticity of the expanding shell around VLA 2 from epochs 1999 to 2007. In fact, the elliptical fit of the VERA data shows a ratio of the minor and major axes of {approx}0.6, in contrast with an almost circular shape for the shell detected in 1999 and 2005 (b/a {approx} 0.9). This suggests that we are probably observing the formation of a jet-driven H{sub 2}O maser structure in VLA2, evolving from a non-collimated pulsed-outflow event during the first stages of evolution of a massive young stellar object (YSO). This may support predictions made

  15. High-mass star-forming cloud G0.38+0.04 in the Galactic Center Dust Ridge contains H2CO and SiO masers

    CERN Document Server

    Ginsburg, Adam; Henkel, Christian; Jones, Paul A; Cunningham, Maria; Kauffmann, Jens; Pillai, Thushara; Mills, Elisabeth A C; Ott, Juergen; Kruijssen, J M Diederik; Menten, Karl M; Battersby, Cara; Rathborne, Jill; Contreras, Yanett; Longmore, Steven; Walker, Daniel; Dawson, Joanne

    2015-01-01

    We have discovered a new H$_2$CO (formaldehyde) $1_{1,0}-1_{1,1}$ 4.82966 GHz maser in Galactic Center Cloud C, G0.38+0.04. At the time of submission, this is the eighth region containing an H$_2$CO maser detected in the Galaxy. Cloud C is one of only two sites of confirmed high-mass star formation along the Galactic Center Ridge, affirming that H$_2$CO masers are exclusively associated with high-mass star formation. This discovery led us to search for other masers, among which we found new SiO vibrationally excited masers, making this the fourth star-forming region in the Galaxy to exhibit SiO maser emission. Cloud C is also a known source of CH$_3$OH Class-II and OH maser emission. There are now two known SiO and H$_2$CO maser containing regions in the CMZ, compared to two and six respectively in the Galactic disk, while there is a relative dearth of H$_2$O and CH$_3$OH Class-II masers in the CMZ. SiO and H$_2$CO masers may be preferentially excited in the CMZ, perhaps due to higher gas-phase abundances fro...

  16. RUBI -a Reference mUltiscale Boiling Investigation for the Fluid Science Laboratory

    Science.gov (United States)

    Schweizer, Nils; Stelzer, Marco; Schoele-Schulz, Olaf; Picker, Gerold; Ranebo, Hans; Dettmann, Jan; Minster, Olivier; Toth, Balazs; Winter, Josef; Tadrist, Lounes; Stephan, Peter; Grassi, Walter; di Marco, Paolo; Colin, Catherine; Piero Celata, Gian; Thome, John; Kabov, Oleg

    Boiling is a two-phase heat transfer process where large heat fluxes can be transferred with small driving temperature differences. The high performance of boiling makes the process very interesting for heat transfer applications and it is widely used in industry for example in power plants, refrigeration systems, and electronics cooling. Nevertheless, due to the large number of involved phenomena and their often highly dynamic nature a fundamental understanding and closed theoretical description is not yet accomplished. The design of systems incorporating the process is generally based on empirical correlations, which are commonly accompanied by large uncertainties and, thus, has to be verified by expensive test campaigns. Hence, strong efforts are currently made to develop applicable numerical tools for a reliable prediction of the boiling heat transfer performance and limits. In order to support and validate this development and, in particular as a precondition, to enhance the basic knowledge about boiling the comprehensive multi-scale experiment RUBI (Reference mUlti-scale Boiling Investigation) for the Fluid Science Laboratory on board the ISS is currently in preparation. The scientific objectives and requirements of RUBI have been defined by the members of the ESA topical team "Boiling and Multiphase Flow" and addresses fundamental aspects of boiling phenomena. The main objectives are the measurement of wall temperature and heat flux distribution underneath vapour bubbles with high spatial and tem-poral resolution by means of IR thermography accompanied by the synchronized high-speed observation of the bubble shapes. Furthermore, the fluid temperature in the vicinity and inside of the bubbles will be measured by a micro sensor array. Additional stimuli are the generation of an electric field above the heating surface and a shear flow created by a forced convection loop. The objective of these stimuli is to impose forces on the bubbles and investigate the

  17. Fabry-perot modes enhanced pump-probe coupling in gold micro-disk patterned ruby thin film

    Science.gov (United States)

    Kumari, Satchi; Khare, Alika; Gupta, Reema; Tomar, Monika; Gupta, Vinay

    2017-10-01

    Enhanced pump-probe coupling has been experimentally observed in epitaxial Ruby thin film patterned with equidistant gold micro-disks (∼100 μm), as compared to pure Ruby film. This has been attributed to Fabry-Perot and surface plasmon modes in Ruby/gold film. In case of S polarized pump and probe beam, Fabry-Perot modes leads to a two-wave mixing gain of ∼1.35. Moreover gain was ∼1.62 in P-polarization case, it has been attributed to coupling of Fabry-Perot and surface plasmon modes. Enhanced coupling for P-polarization can lead to improved nonlinear response in the thin film geometry. It can find applications in thin film based compact photonic devices.

  18. OBSERVATIONAL STUDY OF THE CONTINUUM AND WATER MASER EMISSION IN THE IRAS 19217+1651 REGION

    Energy Technology Data Exchange (ETDEWEB)

    Rodriguez-Esnard, T.; Trinidad, M. A. [Departamento de Astronomia, Universidad de Guanajuato, Apdo Postal 144, Guanajuato, GTO, Mexico CP 36000 (Mexico); Migenes, V., E-mail: tatiana@iga.cu, E-mail: trinidad@astro.ugto.mx, E-mail: vmigenes@byu.edu [Department of Physics and Astronomy, Brigham Young University, ESC-N145, Provo, UT 84602 (United States)

    2012-12-20

    We report interferometric observations of the high-mass star-forming region IRAS 19217+1651. We observed the radio continuum (1.3 cm and 3.6 cm) and water maser emission using the Very Large Array (VLA-EVLA) in transition mode (configuration A). Two radio continuum sources were detected at both wavelengths, I19217-A and I19217-B. In addition, 17 maser spots were observed distributed mainly in two groups, M1 and M2, and one isolated maser. This latter could be indicating the relative position of another continuum source which we did not detect. The results indicate that I19217-A appears to be consistent with an ultracompact H II region associated with a zero-age main-sequence B0-type star. Furthermore, the 1.3 cm continuum emission of this source suggests a cometary morphology. In addition, I19217-B appears to be an H II region consisting of at least two stars, which may be contributing to its complex structure. It was also found that the H{sub 2}O masers of the group M1 are apparently associated with the continuum source I19217-A. These are tracing motions which are not gravitationally bound according to their spatial distribution and kinematics. They also seem to be describing outflows in the direction of the elongated cometary region. On the other hand, the second maser group, M2, could be tracing the base of a jet. Finally, infrared data from Spitzer, Midcourse Space Experiment, and IRIS show that IRAS 19217+1651 is embedded inside a large open bubble, like a broken ring, which possibly has affected the morphology of the cometary H II region observed at 1.3 cm.

  19. Diversidad de cepas de Agrobacterium rubi aisladas de arándanos

    Directory of Open Access Journals (Sweden)

    Eliana Abrahamovich

    Full Text Available Se estudió la diversidad de una colección de cepas de Agrobacterium rubi aisladas de arándanos provenientes de distintas regiones de la República Argentina estableciendo su grado de heterogeneidad mediante pruebas microbiológicas clásicas y técnicas de biología molecular. Los resultados obtenidos en las pruebas bioquímicas y fisiológicas, así como mediante rep-PCR y RFLP del gen 23S ADNr, demostraron una alta variabilidad intraespecífica, tanto fenotípica como genotípica.

  20. Ethephon use and application timing of abscisic acid for improving color of 'Rubi' table grape

    Directory of Open Access Journals (Sweden)

    Sergio Ruffo Roberto

    2013-07-01

    Full Text Available The objective of this work was to evaluate the effect of ethephon and of abscisic acid (ABA application timing on the color of 'Rubi' Table grape. Eight treatments were evaluated: control, without application; ethephon 500 mg L‑1 applied seven days after veraison (7 DAV; and two concentrations of ABA (200 and 400 mg L‑1 arranged with three application timings at 7 DAV, at 15 days before harvest (DBH, and at 7 DAV + 15 DBH. ABA does not modify physical‑chemical characteristics of the cluster and improves the color of grapes, especially when applied twice (7 DAV + 15 DBH at the concentration of 400 mg L‑1.

  1. Topological Insulators on the Ruby Lattice with Rashba Spin-Orbit Coupling

    Institute of Scientific and Technical Information of China (English)

    HOU Jing-Min; WANG Guo-Xiang

    2013-01-01

    We investigate a tight-binding model of the ruby lattice with Rashba spin-orbit coupling.We calculate the band structure of the lattice and evaluate the Z2 topological indices.According to the Z2 topological indices and the band structure,we present the phase diagrams of the lattice with different filling fractions.We find.that topological insulators occur in some range of parameters at 1/6,1/3,1/2,2/3 and 5/6 filling fractions.We analyze and discuss the characteristics of these topological insulators and their edge states.

  2. Nano-scale proteomics approach using two-dimensional fibrin zymography combined with fluorescent SYPRO ruby dye.

    Science.gov (United States)

    Choi, Nack-Shick; Yoo, Ki-Hyun; Yoon, Kab-Seog; Maeng, Pil Jae; Kim, Seung-Ho

    2004-05-31

    In general, a SYPRO Ruby dye is well known as a sensitive fluorescence-based method for detecting proteins by one-or two-dimensional SDS-PAGE (1-DE or 2-DE). Based on the SYPRO Ruby dye system, the combined two-dimensional fibrin zymography (2-D FZ) with SYPRO Ruby staining was newly developed to identify the Bacillus sp. proteases. Namely, complex protein mixtures from Bacillus sp. DJ-4, which were screened from Doen-Jang (Korean traditional fermented food), showed activity on the zymogram gel. The gel spots on the SYPRO Ruby gel, which corresponded to the active spots showing on the 2-D FZ gel, were analyzed by a matrix-assisted laser desorption ionization time of flight (MALDI-TOF) mass spectrometric analysis. Five intracellular fibrinolytic enzymes of Bacillus sp. DJ-4 were detected through 2-D FZ. The gel spots on the SYPRO Ruby dye stained 2-D gel corresponding to 2-D FZ were then analyzed by MALID-TOF MS. Three of the five gel spots proved to be quite similar to the ATP-dependent protease, extracellular neutral metalloprotease, and protease of Bacillus subtilis. Also, the extracellular proteases of Bacillus sp. DJ-4 employing this combined system were identified on three gels (e.g., casein, fibrin, and gelatin) and the proteolytic maps were established. This combined system of 2-D zymography and SYPRO Ruby dye should be useful for searching the specific protease from complex protein mixtures of many other sources (e.g., yeast and cancer cell lines).

  3. The effect of pressure on the nuclear quadrupole resonance and ruby fluorescence in a NiCrAl pressure cell

    Energy Technology Data Exchange (ETDEWEB)

    Fujiwara, N [Graduate School of Human and Environmental Studies, Kyoto University, Yoshida-nihonmatsu-cho, Sakyo-ku, Kyoto 606-8501 (Japan); Koyama-Nakazawa, K [Institute for Solid State Physics, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8581 (Japan); Matsumoto, T [National Institute for Materials Science, Tsukuba 305-0047 (Japan); Hisada, A [Graduate School of Human and Environmental Studies, Kyoto University, Yoshida-nihonmatsu-cho, Sakyo-ku, Kyoto 606-8501 (Japan); Uwatoko, Y [Institute for Solid State Physics, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8581 (Japan)

    2007-10-24

    A pressure of 4.0 GPa was achieved using a piston-cylinder-type NiCrAl pressure cell which possesses a large sample space of 4.4 mm diameter x 15 mm length at ambient pressure. As monitors of the pressure, the {sup 63}Cu nuclear quadrupole resonance (NQR) of Cu{sub 2}O and ruby fluorescence were studied at the same time. The relation between the NQR frequency and the R1 line of the ruby fluorescence was investigated at pressures below 3.2 GPa.

  4. The 6-GHz methanol multibeam maser catalogue IV: Galactic longitudes 186 to 330 including the Orion-Monoceros region

    OpenAIRE

    Green, J. A.; Caswell, J.L.; Fuller, G. A.; Avison, A.; Breen, S. L.; Ellingsen, S. P.; Gray, M. D.; Pestalozzi, M.; Quinn, L.; Thompson, M A; Voronkov, M. A.

    2012-01-01

    We present the fourth portion of a Galactic Plane survey of methanol masers at 6668 MHz, spanning the longitude range 186 degrees to 330 degrees. We report 207 maser detections, 89 new to the survey. This completes the southern sky part of the Methanol Multibeam survey and includes a large proportion of new sources, 43%. We also include results from blind observations of the Orion-Monoceros star forming region, formally outside the latitude range of the Methanol Multibeam survey; only the fou...

  5. [Determination of ellagic acid, flavonoids and goshonoside-F5 in Rubi Fructus by HPLC].

    Science.gov (United States)

    He, Jian-Ming; Sun, Nan; Wu, Wen-Dan; Fan, Li-Jiao; Guo, Mei-Li

    2013-12-01

    High-performance liquid chromatographic coupled with variable wavelength detection (HPLC-VWD) has been developed for simultaneous determination of 5 analytes including ellagic acid, quercetin, kaempferol-3-O-beta-D-rutinoside, tiliroside and kaempferol, and high-performance liquid chromatographic with an evaporative light scattering detector (HPLC-ELSD) has been established to determine goshonoside-F5 in extract of Rubi Fructus. Chromatographic separations were carried out on an Agilent ZORBAX SB-C18 column (4.6 mm x 250 mm, 5.0 microm). All calibration curves of reference standards revealed good linearity (R2 > 0.999 5) within the concentration ranges tested. The method limits of detection ranged 0.297-90.144 ng and the method limits ofquantitation ranged 0.990-300.480 ng, respectively. Recoveries of 6 analytes were from 97.11% to 101.7%, with RSD less than 2.1%. The result shows that amounts of the 6 analytes in the samples from 16 localities were found to be different. The higher latitude of growing environment, the more ellagic acid in herb. The content of total flavonoids in sample from east localities were higher than that in middle and west localities, and the content of goshonoside-F5 in Bozhou, Anhui province was higher than others. This method was found to be simple, accurate, sensitive with good repeatability. Those results might serve as a sound foundation for further study, quality control and application of Rubi Fructus.

  6. Evolution of basin and range structure in the Ruby Mountains and vicinity, Nevada

    Science.gov (United States)

    Blackwell, D. D.; Reese, N. M.; Kelley, S. A.

    Results from various age dating techniques, seismic reflection profiling hydrocarbon maturation studies, and structural analysis were used to evaluate the Cenozoic deformation in the Ruby Mountains and adjoining ranges (pinyon Range and Cortez Range) in Elko and Eureka Counties, Nevada. Age dating techniques used include potassium-argon ages of biotites from granites published by Kistler et al. (1981) and fission track ages from apatite and zircon. Fission track ages from apatite reflect a closing temperature of 100 plus or minus 20 deg C. Zircon fission track ages reflect a closing temperature of 175 plus or minus 25 deg C and potassium-argon ages from brotite reflect a closing temperature of 250 plus or minus 30 deg C. Thus these results allow a reasonably precise tracking of the evolution of the ranges during the Cenozoic. Seismic reflection data are available from Huntington Valley. Access to seismic reflection data directly to the west of the Harrison Pass Pluton in the central Ruby Mountains was obtained. In addition results are available from several deep exploration holes in Huntington Valley.

  7. N and Cr ion implantation of natural ruby surfaces and their characterization

    Energy Technology Data Exchange (ETDEWEB)

    Rao, K. Sudheendra; Sahoo, Rakesh K.; Dash, Tapan [CSIR-Institute of Minerals and Materials Technology, Bhubaneswar 751013 (India); Magudapathy, P.; Panigrahi, B.K. [Materials Science Group, Indira Gandhi Centre for Atomic Research, Kalpakkam 603102 (India); Nayak, B.B.; Mishra, B.K. [CSIR-Institute of Minerals and Materials Technology, Bhubaneswar 751013 (India)

    2016-04-15

    Highlights: • Cr and N ion implantation on natural rubies of low aesthetic quality. • Cr-ion implantation improves colour tone from red to deep red (pigeon eye red). • N-ion implantation at fluence of 3 × 10{sup 17} causes blue coloration on surface. • Certain extent of amorphization is observed in the case of N-ion implantation. - Abstract: Energetic ions of N and Cr were used to implant the surfaces of natural rubies (low aesthetic quality). Surface colours of the specimens were found to change after ion implantation. The samples without and with ion implantation were characterized by diffuse reflectance spectra in ultra violet and visible region (DRS-UV–Vis), field emission scanning electron microscopy (FESEM), selected area electron diffraction (SAED) and nano-indentation. While the Cr-ion implantation produced deep red surface colour (pigeon eye red) in polished raw sample (without heat treatment), the N-ion implantation produced a mixed tone of dark blue, greenish blue and violet surface colour in the heat treated sample. In the case of heat treated sample at 3 × 10{sup 17} N-ions/cm{sup 2} fluence, formation of colour centres (F{sup +}, F{sub 2}, F{sub 2}{sup +} and F{sub 2}{sup 2+}) by ion implantation process is attributed to explain the development of the modified surface colours. Certain degree of surface amorphization was observed to be associated with the above N-ion implantation.

  8. Formation of highly toxic hydrogen cyanide upon ruby laser irradiation of the tattoo pigment phthalocyanine blue

    Science.gov (United States)

    Schreiver, Ines; Hutzler, Christoph; Laux, Peter; Berlien, Hans-Peter; Luch, Andreas

    2015-08-01

    Since laser treatment of tattoos is the favored method for the removing of no longer wanted permanent skin paintings, analytical, biokinetics and toxicological data on the fragmentation pattern of commonly used pigments are urgently required for health safety reasons. Applying dynamic headspace—gas chromatography with mass spectrometric detection (DHS—GC/MS) and comprehensive two-dimensional gas chromatography coupled to time-of-flight mass spectrometry (GCxGC—ToF-MS), we identified 1,2-benzene dicarbonitrile, benzonitrile, benzene, and the poisonous gas hydrogen cyanide (HCN) as main fragmentation products emerging dose-dependently upon ruby laser irradiation of the popular blue pigment copper phthalocyanine in suspension. Skin cell viability was found to be significantly compromised at cyanide levels of ≥1 mM liberated during ruby laser irradiation of >1.5 mg/ml phthalocyanine blue. Further, for the first time we introduce pyrolysis-GC/MS as method suitable to simulate pigment fragmentation that may occur spontaneously or during laser removal of organic pigments in the living skin of tattooed people. According to the literature such regular tattoos hold up to 9 mg pigment/cm2 skin.

  9. Making waves the story of Ruby Payne-Scott : Australian pioneer radio astronomer

    CERN Document Server

    Goss, M

    2013-01-01

    This book is an abbreviated, partly re-written version of "Under the Radar - The First Woman in Radio Astronomy: Ruby Payne-Scott." It addresses a general readership interested in historical and sociological aspects of astronomy and presents the biography of Ruby Payne-Scott (1912 – 1981). As the first female radio astronomer (and one of the first people in the world to consider radio astronomy), she made classic contributions to solar radio physics. She also played a major role in the design of the Australian government's Council for Scientific and Industrial Research radars, which were in turn of vital importance in the Southwest Pacific Theatre in World War II. These radars were used by military personnel from Australia, the United States and New Zealand. From a sociological perspective, her career offers many examples of the perils of being a female academic in the first half of the 20th century. Written in an engaging style and complemented by many historical photographs, this book offers fascinating...

  10. Formation of highly toxic hydrogen cyanide upon ruby laser irradiation of the tattoo pigment phthalocyanine blue.

    Science.gov (United States)

    Schreiver, Ines; Hutzler, Christoph; Laux, Peter; Berlien, Hans-Peter; Luch, Andreas

    2015-08-05

    Since laser treatment of tattoos is the favored method for the removing of no longer wanted permanent skin paintings, analytical, biokinetics and toxicological data on the fragmentation pattern of commonly used pigments are urgently required for health safety reasons. Applying dynamic headspace-gas chromatography with mass spectrometric detection (DHS-GC/MS) and comprehensive two-dimensional gas chromatography coupled to time-of-flight mass spectrometry (GCxGC-ToF-MS), we identified 1,2-benzene dicarbonitrile, benzonitrile, benzene, and the poisonous gas hydrogen cyanide (HCN) as main fragmentation products emerging dose-dependently upon ruby laser irradiation of the popular blue pigment copper phthalocyanine in suspension. Skin cell viability was found to be significantly compromised at cyanide levels of ≥1 mM liberated during ruby laser irradiation of >1.5 mg/ml phthalocyanine blue. Further, for the first time we introduce pyrolysis-GC/MS as method suitable to simulate pigment fragmentation that may occur spontaneously or during laser removal of organic pigments in the living skin of tattooed people. According to the literature such regular tattoos hold up to 9 mg pigment/cm(2) skin.

  11. Treatment of infraorbital dark circles using 694-nm fractional Q-switched ruby laser.

    Science.gov (United States)

    Xu, Tian-Hua; Li, Yuan-Hong; Chen, John Z S; Gao, Xing-Hua; Chen, Hong-Duo

    2016-12-01

    The objective of this study was to evaluate the efficacy and safety of using a 694-nm fractional Q-switched ruby laser to treat infraorbital dark circles. Thirty women with infraorbital dark circles (predominant color: dark/brown) participated in this open-labeled study. The participants received eight sessions of 694-nm fractional Q-switched ruby laser treatment using a fluence of 3.0-3.5 J/cm(2), at an interval of 7 days. The melanin deposition in the lesional skin was observed in vivo using reflectance confocal microscopy (RCM). The morphological changes were evaluated using a global evaluation, an overall self-assessment, and a Mexameter. Twenty-eight of the 30 patients showed global improvements that they rated as excellent or good. Twenty-six patients rated their overall satisfaction as excellent or good. The melanin index indicated a substantial decrease from 240.44 (baseline) to 194.56 (P dark/brown infraorbital dark circles is caused by increased melanin deposition in the upper dermis. The treatment of these infraorbital dark circles using a 694-nm fractional QSR laser is safe and effective.

  12. The Cascading Impacts of Technology Selection: Incorporating Ruby on Rails into ECHO

    Science.gov (United States)

    Pilone, D.; Cechini, M.

    2010-12-01

    NASA’s Earth Observing System (EOS) ClearingHOuse (ECHO) is a SOA based Earth Science Data search and order system implemented in Java with one significant exception: the web client used by 98% of our users is written in Perl. After several decades of maintenance the Perl based application had reached the end of its serviceable life and ECHO was tasked with implementing a replacement. Despite a broad investment in Java, the ECHO team conducted a survey of modern development technologies including Flex, Python/Django, JSF2/Spring and Ruby on Rails. The team ultimately chose Ruby on Rails (RoR) with Cucumber for testing due to its perceived applicability to web application development and corresponding development efficiency gains. Both positive and negative impacts on the entire ECHO team, including our stakeholders, were immediate and sometimes subtle. The technology selection caused shifts in our architecture and design, development and deployment procedures, requirement definition approach, testing approach, and, somewhat surprisingly, our project team structure and software process. This presentation discusses our experiences, including technical, process, and psychological, using RoR on a production system. During this session we will discuss: - Real impacts of introducing a dynamic language to a Java team - Real and perceived efficiency advantages - Impediments to adoption and effectiveness - Impacts of transition from Test Driven Development to Behavior Driven Development - Leveraging Cucumber to provide fully executable requirement documents - Impacts on team structure and roles

  13. Pilot VLBI Survey of SiO v=3 J=1--0 Maser Emission around Evolved Stars

    CERN Document Server

    Imai, Hiroshi; Chong, Sze Ning; Nakagawa, Akiharu; Kurayama, Tomoharu; Nakashima, Jun-ichi; Matsumoto, Naoko; Nagayama, Takumi; Oyama, Tomoaki; Mizuno, Shota; Deguchi, Shuji; Cho, Se-Hyung

    2012-01-01

    In this Letter, we report detections of SiO v=3 J=1--0 maser emission in very long baseline interferometric (VLBI) observations towards 4 out of 12 long-period variable stars: WX Psc, R Leo, W Hya, and T Cep. The detections towards WX Psc and T Cep are new ones. We also present successful astrometric observations of SiO v=2 and v=3 J=1--0 maser emissions associated with two stars: WX Psc and W Hya and their position-reference continuum sources: J010746.0+131205 and J135146.8-291218 with the VLBI Exploration of Radio Astrometry (VERA). The relative coordinates of the position-reference continuum source and SiO v=3 maser spots were measured with respect to those of an SiO v=2 maser spot adopted as fringe-phase reference. Thus the faint continuum sources were inversely phase-referenced to the bright maser sources. It implies possible registration of multiple SiO maser line maps onto a common coordinate system with 10 microarcsecond-level accuracy.

  14. Probing the Evolution of Massive Young Stellar Objects using Weak Class II 6.7GHz Methanol Maser Emission

    Science.gov (United States)

    Ludwig, Bethany Ann; Cunningham, Nichol

    2017-01-01

    We present results from an investigation of class II 6.7GHz methanol masers towards four Massive Young Stellar Objects (MYSOs). The sources, selected from the Red MSX Source (RMS) Survey (Lumsden et al. 2013), were previously understood to be non-detections for class II methanol maser emission in the methanol multi-beam (MMB) Survey (Caswell et al. 2010.) Class II methanol masers are a well-known sign post of massive star forming regions and may be utilized to probe their relatively poorly understood formation. It is possible that these non-detections are simply weak masers that are potentially associated with a younger evolutionary phase of MYSOs as hypothesized by Olmi et al. (2014). The sources were chosen to sample various stages of evolution, having similar 21 to 8 micron flux ratios and bolometric luminosities as other MYSOs with previous class II methanol maser detections. We observed all 4 MYSOs with ATCA (~2" resolution) at 10 times deeper sensitivity than previously obtained with the MMB survey and have a spectral resolution of 0.087kms^-1 . The raw data is reduced using the program Miriad (Sault, R. J., et al., 1995) and deconvolutioned using the program CASA (McMullin, J. P., et al. 2007.) We determine one of the four observed MYSOs is harboring a weak class II methanol maser. We discuss the possibility of sensitivity limitations on the remaining sources as well as environmental and evolutionary differences between the sources.

  15. Studies of circumstellar shells in AGB stars by multifrequency (sub)mm-VLBI observations of maser emission

    Science.gov (United States)

    Colomer, F.; Desmurs, J. F.; Bujarrabal, V.; Baudry, A.; de Vicente, P.; Soria-Ruiz, R.; Alcolea, J.; Diaz-Pulido, A.; Gómez, M.

    2017-03-01

    VLBI observations of maser emission are a basic tool to study the circumstellar envelopes (CSEs) around evolved stars, mainly around AGB and post-AGB stars. The maser lines of water and silicon monoxide are particularly intense. They provide us with high spatial resolution data on the very inner CSEs around AGB stars, including the pulsating layers previous to grain formation and outer regions where the fast expansion characteristic of such envelopes is already present. The analysis of the pumping mechanism of SiO masers and of the physical conditions in the emitting clumps requires accurate maps of the various lines, which show different excitation requirements. A large observational effort is being done to obtain (quasi-)simultaneous multiline data at the highest spatial resolution, using VLBI techniques, which makes possible to compare the relative distribution of the maser lines. We present the state-of-the-art in the field, and discuss preliminary results of SiO masers observed with the Global Millimeter VLBI Array (GMVA) which provide a new view into the physics of these AGB envelopes. The participation of ALMA in these VLBI arrays will boost the study of these masers, at higher frequencies.

  16. Water maser variability over 20 years in a large sample of star-forming regions: the complete database

    CERN Document Server

    Felli, M; Cesaroni, R; Codella, C; Comoretto, G; Di Franco, S; Massi, F; Moscadelli, L; Nesti, R; Olmi, L; Palagi, F; Panella, D; Valdettaro, R

    2007-01-01

    Context. Water vapor emission at 22 GHz from masers associated with star-forming regions is highly variable. Aims. We present a database of up to 20 years of monitoring of a sample of 43 masers within star-forming regions. The sample covers a large range of luminosities of the associated IRAS source and is representative of the entire population of H2O masers of this type. The database forms a good starting point for any further study of H2O maser variability. Methods. The observations were obtained with the Medicina 32-m radiotelescope, at a rate of 4-5 observations per year. Results. To provide a database that can be easily accessed through the web, we give for each source: plots of the calibrated spectra, the velocity-time-flux density plot, the light curve of the integrated flux, the lower and upper envelopes of the maser emission, the mean spectrum, and the rate of the maser occurrence as a function of velocity. Figures for just one source are given in the text for representative purposes. Figures for al...

  17. Water maser variability over 20 years in a large sample of star-forming regions: the complete database

    Science.gov (United States)

    Felli, M.; Brand, J.; Cesaroni, R.; Codella, C.; Comoretto, G.; Di Franco, S.; Massi, F.; Moscadelli, L.; Nesti, R.; Olmi, L.; Palagi, F.; Panella, D.; Valdettaro, R.

    2007-12-01

    Context: Water vapor emission at 22 GHz from masers associated with star-forming regions is highly variable. Aims: We present a database of up to 20 years of monitoring of a sample of 43 masers within star-forming regions. The sample covers a large range of luminosities of the associated IRAS source and is representative of the entire population of H2O masers of this type. The database forms a good starting point for any further study of H2O maser variability. Methods: The observations were obtained with the Medicina 32-m radiotelescope, at a rate of 4-5 observations per year. Results: To provide a database that can be easily accessed through the web, we give for each source: plots of the calibrated spectra, the velocity-time-flux density plot, the light curve of the integrated flux, the lower and upper envelopes of the maser emission, the mean spectrum, and the rate of the maser occurrence as a function of velocity. Figures for just one source are given in the text for representative purposes. Figures for all the sources are given in electronic form the appendix. A discussion of the main properties of the H2O variability in our sample will be presented in a forthcoming paper. Based on observations with the Medicina radiotelescope operated by INAF - Istituto di Radioastronomia.

  18. OH 1720-MHz lines as tracers of bipolar outflows in the vicinity of Class I methanol masers

    Science.gov (United States)

    Litovchenko, I. D.; Bayandina, O. S.; Alakoz, A. V.; Val'tss, I. E.; Larionov, G. M.; Mukha, D. V.; Nabatov, A. S.; Konovalenko, A. A.; Zakharenko, V. V.; Alekseev, E. V.; Nikolaenko, V. S.; Kulishenko, V. F.; Odintsov, S. A.

    2012-07-01

    A sample of Class I methanol masers (MMI) has been surveyed at 1720 MHz to search for possible associations between MMI and 1720-MHz OH masers, which should be formed by the same collisional pumping mechanism. If the model for methanol masers is correct, the sample should contain a statistically significant number of 1720-MHz OH masers at the positions of MMI. The observations were conducted on the 70-meter radio telescope of the National Academy of Sciences of Ukraine (NASU). The results show that ˜50% of 72 MMI are associated with OH emission at 1720 MHz. In many sources, strong absorption lines are also observed. In most cases, the OH (1720) lines are narrow (linewidths of <2 km/s) suggesting they may be maser lines. The OH column densities obtained from Gaussian fitting of these narrow OH lines are, on average, 1.5 × 1017 cm-2. TheH2 density in the emitting medium reaches 107 cm-3 if the region of the OH (1720) emission has been subject to interaction with a bipolar-outflow front. This is sufficient to excite MMI, and the presence of narrow, possibly masing OH (1720) lines at the MMI velocities indicates the likely presence of shocks from bipolar outflows in the vicinity of the maser condensations, supporting models in which these molecules are collisionally pumped.

  19. A Class I and Class II Methanol Maser Survey of Extended Green Objects (EGOs) from the GLIMPSE Survey

    CERN Document Server

    Cyganowski, C J; Hunter, T R; Churchwell, E

    2009-01-01

    We present the results of a high angular resolution Very Large Array (VLA) Class I 44 GHz and Class II 6.7 GHz methanol maser survey of a sample of ~20 massive young stellar object (MYSO) outflow candidates selected on the basis of extended 4.5 micron emission in Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) images. These 4.5 micron-selected candidates are referred to as extended green objects (EGOs), for the common coding of this band as green in three-color IRAC images. The detection rate of 6.7 GHz Class II methanol masers, which are associated exclusively with massive YSOs, towards EGOs is greater than ~64%--nearly double the detection rate of surveys using other MYSO selection criteria. The detection rate of Class I 44 GHz methanol masers, which trace molecular outflows, is ~89% towards EGOs associated with 6.7 GHz methanol masers. The two types of methanol masers exhibit different spatial distributions: 6.7 GHz masers are centrally concentrated and usually coincide with 24 m...

  20. H2O masers and protoplanetary disk dynamics in IC 1396 N

    Science.gov (United States)

    Bayandina, O. S.; Val'tts, I. E.; Kurtz, S. E.; Rudnitskij, G. M.; Alakoz, A. V.

    2017-06-01

    We report H2O maser line observations of the bright-rimmed globule IC 1396 N using a ground-space interferometer with the 10-m RadioAstron radio telescope as the space-based element. The source was not detected on projected baselines >2.3. Earth diameters, which indicates a lower limit on the maser size of L > 0.03 AU and an upper limit on the brightness temperature of 6.25 × 1012 K. Fringe-rate maps are prepared based on data from ground-ground baselines. Positions, velocities and flux densities of maser spots were determined. Multiple low-velocity features from -4.5 km/s to +0.7 km/s are seen, and two high-velocity features of V LSR = -9.4 km/s and V LSR = +4.4 km/s are found at projected distances of 157 AU and 70 AU, respectively, from the strongest low-velocity feature at V LSR = +0.3 km/s. Maser components from the central part of the spectrum fall into four velocity groups but into three spatial groups. Three spatial groups of low-velocity features detected in the 2014 observations are arranged in a linear structure about 200 AU in length. Two of these groups were not detected in 1996 and possibly are jets which formed between 1996 and 2014. The putative jet seems to have changed direction in 18 years, which we explain by the precession of the jet under the influence of the gravity of material surrounding the globule. The jet collimation can be provided by a circumstellar protoplanetary disk. There is a straight line orientation in the " V LSR-Right Ascension" diagram between the jet and the maser group at V LSR = +0.3 km/s. However, the central group with the same position but at the velocity V LSR -3.4 km/s falls on a straight line between two high-velocity components detected in 2014. Comparison of the low-velocity positions from 2014 and 1996, based on the same V LSR-Right Ascension diagram for low-velocity features, shows that the majority of the masers maintain their positions near the central velocity V LSR = 0.3 km/s during the 18 year period.

  1. Reflectivity of the gyroid biophotonic crystals in the ventral wing scales of the Green Hairstreak butterfly, Callophrys rubi

    NARCIS (Netherlands)

    Michielsen, K.; De Raedt, H.; Stavenga, D. G.

    2010-01-01

    We present a comparison of the computer simulation data of gyroid nanostructures with optical measurements (reflectivity spectra and scattering diagrams) of ventral wing scales of the Green Hairstreak butterfly, Callophrys rubi. We demonstrate that the omnidirectional green colour arises from the gy

  2. Exogenous gibberellins inhibit coffee (Coffea arabica cv. Rubi) seed germination and cause cell death in the embryo

    NARCIS (Netherlands)

    Silva, Da E.A.A.; Toorop, P.E.; Nijsse, J.; Bewley, J.D.; Hilhorst, H.W.M.

    2005-01-01

    The mechanism of inhibition of coffee (Coffea arabica cv. Rubi) seed germination by exogenous gibberellins (GAs) and the requirement of germination for endogenous GA were studied. Exogenous GA4+7 inhibited coffee seed germination. The response to GA4+7 showed two sensitivity thresholds: a lower one

  3. Abscisic acid controls embryo growth potential and endosperm cap weakening during coffee (Coffea arabica cv. Rubi) seed germination

    NARCIS (Netherlands)

    Silva, da E.A.A.; Toorop, P.E.; Aelst, van A.C.; Hilhorst, H.W.M.

    2004-01-01

    The mechanism and regulation of coffee seed germination were studied in Coffea arabica L. cv. Rubi. The coffee embryo grew inside the endosperm prior to radicle protrusion and abscisic acid (ABA) inhibited the increase in its pressure potential. There were two steps of endosperm cap weakening. An in

  4. The strength of ruby from X-ray diffraction under non-hydrostatic compression to 68 GPa

    Science.gov (United States)

    Dong, Haini; Dorfman, Susannah M.; Wang, Jianghua; He, Duanwei; Duffy, Thomas S.

    2014-07-01

    Polycrystalline ruby (α-Al2O3:Cr3+), a widely used pressure calibrant in high-pressure experiments, was compressed to 68.1 GPa at room temperature under non-hydrostatic conditions in a diamond anvil cell. Angle-dispersive X-ray diffraction experiments in a radial geometry were conducted at beamline X17C of the National Synchrotron Light Source. The stress state of ruby at high pressure and room temperature was analyzed based on the measured lattice strain. The differential stress of ruby increases with pressure from ~3.4 % of the shear modulus at 18.5 GPa to ~6.5 % at 68.1 GPa. The polycrystalline ruby sample can support a maximum differential stress of ~16 GPa at 68.1 GPa under non-hydrostatic compression. The results of this study provide a better understanding of the mechanical properties of this important material for high-pressure science. From a synthesis of existing data for strong ceramic materials, we find that the high-pressure yield strength correlates well with the ambient pressure Vickers hardness.

  5. Pathogenicity, fungicide resistance, and genetic variability of Phytophthora rubi isolates from raspberry (Rubus idaeus) in the Western United States

    Science.gov (United States)

    Root rot of raspberry (Rubus idaeus), thought to be primarily caused by Phytophthora rubi, is an economically important disease in the western United States. The objectives of this study were to determine which Phytophthora species are involved in root rot, examine the efficacy of different isolatio...

  6. Calcium rubies: a family of red-emitting functionalizable indicators suitable for two-photon Ca2+ imaging.

    Science.gov (United States)

    Collot, Mayeul; Loukou, Christina; Yakovlev, Aleksey V; Wilms, Christian D; Li, Dongdong; Evrard, Alexis; Zamaleeva, Alsu; Bourdieu, Laurent; Léger, Jean-François; Ropert, Nicole; Eilers, Jens; Oheim, Martin; Feltz, Anne; Mallet, Jean-Maurice

    2012-09-12

    We designed Calcium Rubies, a family of functionalizable BAPTA-based red-fluorescent calcium (Ca(2+)) indicators as new tools for biological Ca(2+) imaging. The specificity of this Ca(2+)-indicator family is its side arm, attached on the ethylene glycol bridge that allows coupling the indicator to various groups while leaving open the possibility of aromatic substitutions on the BAPTA core for tuning the Ca(2+)-binding affinity. Using this possibility we now synthesize and characterize three different CaRubies with affinities between 3 and 22 μM. Their long excitation and emission wavelengths (peaks at 586/604 nm) allow their use in otherwise challenging multicolor experiments, e.g., when combining Ca(2+) uncaging or optogenetic stimulation with Ca(2+) imaging in cells expressing fluorescent proteins. We illustrate this capacity by the detection of Ca(2+) transients evoked by blue light in cultured astrocytes expressing CatCh, a light-sensitive Ca(2+)-translocating channelrhodopsin linked to yellow fluorescent protein. Using time-correlated single-photon counting, we measured fluorescence lifetimes for all CaRubies and demonstrate a 10-fold increase in the average lifetime upon Ca(2+) chelation. Since only the fluorescence quantum yield but not the absorbance of the CaRubies is Ca(2+)-dependent, calibrated two-photon fluorescence excitation measurements of absolute Ca(2+) concentrations are feasible.

  7. Abscisic acid controls embryo growth potential and endosperm cap weakening during coffee (Coffea arabica cv. Rubi) seed germination

    NARCIS (Netherlands)

    Silva, da E.A.A.; Toorop, P.E.; Aelst, van A.C.; Hilhorst, H.W.M.

    2004-01-01

    The mechanism and regulation of coffee seed germination were studied in Coffea arabica L. cv. Rubi. The coffee embryo grew inside the endosperm prior to radicle protrusion and abscisic acid (ABA) inhibited the increase in its pressure potential. There were two steps of endosperm cap weakening. An in

  8. Influence of form IA RubisCO and environmental dissolved inorganic carbon on the delta13C of the clam-chemoautotroph symbiosis Solemya velum.

    Science.gov (United States)

    Scott, Kathleen M; Schwedock, Julie; Schrag, Daniel P; Cavanaugh, Colleen M

    2004-12-01

    Many nutritive symbioses between chemoautotrophic bacteria and invertebrates, such as Solemya velum, have delta(13)C values of approximately -30 to -35%, considerably more depleted than phytoplankton. Most of the chemoautotrophic symbionts fix carbon with a form IA ribulose 1,5-bisphosphate carboxylase (RubisCO). We hypothesized that this form of RubisCO discriminates against (13)CO(2) to a greater extent than other forms. Solemya velum symbiont RubisCO was cloned and expressed in Escherichia coli, purified and characterized. Enzyme from this recombinant system fixed carbon most rapidly at pH 7.5 and 20-25 degrees C. Surprisingly, this RubisCO had an epsilon-value (proportional to the degree to which the enzyme discriminates against (13)CO(2)) of 24.4 per thousand, similar to form IB RubisCOs, and higher than form II RubisCOs. Samples of interstitial water from S. velum's habitat were collected to determine whether the dissolved inorganic carbon (DIC) could contribute to the negative delta(13)C values. Solemya velum habitat DIC was present at high concentrations (up to approximately 5 mM) and isotopically depleted, with delta(13)C values as low as approximately -6%. Thus environmental DIC, coupled with a high degree of isotopic fractionation by symbiont RubisCO likely contribute to the isotopically depleted delta(13)C values of S. velum biomass, highlighting the necessity of considering factors at all levels (from environmental to enzymatic) in interpreting stable isotope ratios.

  9. Kinetic simulation of the electron-cyclotron maser instability: effect of a finite source size

    CERN Document Server

    Kuznetsov, A A

    2012-01-01

    The electron-cyclotron maser instability is widespread in the Universe, producing, e.g., radio emission of the magnetized planets and cool substellar objects. Diagnosing the parameters of astrophysical radio sources requires comprehensive nonlinear simulations of the radiation process. We simulate the electron-cyclotron maser instability in a very low-beta plasma. The model used takes into account the radiation escape from the source region and the particle flow through this region. We developed a kinetic code to simulate the time evolution of an electron distribution in a radio emission source. The model includes the terms describing the particle injection to and escape from the emission source region. The spatial escape of the emission from the source is taken into account by using a finite amplification time. The unstable electron distribution of the horseshoe type is considered. A number of simulations were performed for different parameter sets typical of the magnetospheres of planets and ultracool dwarf...

  10. EDM measurement in {sup 129}Xe atom using dual active feedback nuclear spin maser

    Energy Technology Data Exchange (ETDEWEB)

    Sato, T., E-mail: sato@yap.nucl.ap.titech.ac.jp [Tokyo Institute of Technology, Department of Physics (Japan); Ichikawa, Y. [RIKEN Nishina Center (Japan); Ohtomo, Y.; Sakamoto, Y.; Kojima, S.; Funayama, C.; Suzuki, T.; Chikamori, M.; Hikota, E.; Tsuchiya, M. [Tokyo Institute of Technology, Department of Physics (Japan); Furukawa, T. [Tokyo Metropolitan University, Department of Physics (Japan); Yoshimi, A. [Okayama University, Research Core for Extreme Quantum World (Japan); Bidinosti, C. P. [University of Winnipeg, Department Physics (Canada); Ino, T. [Institute of Material Structure Science, KEK (Japan); Ueno, H. [RIKEN Nishina Center (Japan); Matsuo, Y. [Hosei University, Department of Advanced Sciences (Japan); Fukuyama, T. [Osaka University, RCNP (Japan); Asahi, K. [Tokyo Institute of Technology, Department of Physics (Japan)

    2015-04-15

    The technique of an active nuclear spin maser is adopted in the search for electric dipole moment in a diamagnetic atom {sup 129}Xe. In order to reduce systematic uncertainties arising from long-term drifts of the external magnetic field and from the contact interaction between longitudinal polarized Rb atoms and {sup 129}Xe spin, a {sup 3}He comagnetometer with a double-cell geometry was employed. The remaining shift, which turned out to show some correlation with the cell temperature, was mitigated by stabilizing the cell temperature. As a result, the frequency drift of the {sup 129}Xe maser was reduced from 12 mHz to 700 μHz, and the determination precision of frequency of 8.7 nHz was obtained for a 2×10{sup 4} s measurement time using the double-cell geometry cell.

  11. Effects of correlated turbulent velocity fields on the formation of maser lines

    CERN Document Server

    Boeger, R; Hegmann, M

    2003-01-01

    The microturbulent approximation of turbulent motions is widely used in radiative transfer calculations. Mainly motivated by its simple computational application it is probably in many cases an oversimplified treatment of the dynamical processes involved. This aspect is in particular important in the analysis of maser lines, since the strong amplification of radiation leads to a sensitive dependence of the radiation field on the overall velocity structure. To demonstrate the influence of large scale motions on the formation of maser lines we present a simple stochastic model which takes velocity correlations into account. For a quantitative analysis of correlation effects, we generate in a Monte Carlo simulation individual realizations of a turbulent velocity field along a line of sight. Depending on the size of the velocity correlation length we find huge deviations between the resulting random profiles in respect of line shape, intensity and position of single spectral components. Finally, we simulate the e...

  12. Major structures of the inner Galaxy delineated by 6.7-GHz methanol masers

    CERN Document Server

    Green, J A; McClure-Griffiths, N M; Avison, A; Breen, S L; Burton, M G; Ellingsen, S P; Fuller, G A; Gray, M D; Pestalozzi, M; Thompson, M A; Voronkov, M A

    2011-01-01

    We explore the longitude-velocity distribution of 6.7-GHz methanol masers in the context of the inner structure of our Galaxy. We analyse the correlation in velocities within this distribution and identify density enhancements indicating large-scale regions of enhanced star formation. These are interpreted as the starting points of the spiral arms and the interaction of the Galactic bar with the 3-kpc arms. The methanol masers support the presence of a long thin bar with a 45 degree orientation. Signatures of the full 3-kpc arm structure are seen, including a prominent tangent at approximately -22 degrees Galactic longitude. We compare this distribution with existing models of the gas dynamics of our Galaxy. The 3-kpc arm structure appears likely to correspond to the radius of corotation resonance of the bar, with the bar on its inner surface and the starting points of the spiral arms on its outer surface.

  13. First observations of the water masers with the Urumqi 25m radio telescope

    Institute of Scientific and Technical Information of China (English)

    ZHENG; Xingwu

    2001-01-01

    [1]Moran, J. M., Cosmic masers—— A powerful tool for astrophysics, in Modern Radio Science (ed. Hamelin, J. H.), Oxford: Oxford University Press, 1996, 275.[2]Miyoshi, M., Moran, J. M., Herrnstein J. Et al., Evidence for a massive black hole from high rotational velocities in a sub-parsec region of NGC 4258, Nature, 1995, 373: 127.[3]Comoretto, G., Palagi, F., Cesaroni, R. Et al., The Arccetri atlas of H2O maser sources, A & As, 1996, 84: 17.[4]Braatz, J. A., Wilson, A. S., Henkel, C., A survey for H2O megamasers in active galactic nuclei, ApJS, 1996, 106: 51.[5]Wang, J., Zheng, X., Liang, Z. Et al., Interstellar H2O masers a tracer of galactic spiral structure, Ap. & Sp. S., 1992, 200: 163.[6]Greenhill, L. J., Hernstein, J. R., Moran, J. M. Et al., A search for H2O maser emission toward AGN, Ap. J., 1997, 481: L23.[7]Jack, M. A., Paige, E. G. S., Fourier transformation processors based on surface acoustic wave chirp filters, Wave Electronics, 1978, 3: 329.[8]Jack, M. A., Grant, P. M., Collins, J. H., The theory, design, and application of surface-acoustic-wave Fourier-transform processor, Proc. Of IEEE, 1989, 68: 4.[9]Liljestrom, T., Mattila, K., Toriseva, M. Et al., W49N water maser: spectral atlas of time variability during 1981-1985, A & Ap. Sup., 1989, 79: 19-39.[10]Chen, D., Gong, J., Zhou, X. Et al., A new type of radio astronomical spectrometer-saw spectrometer, Acta Astrophysica Sinica, 1990, 13: 85.

  14. VizieR Online Data Catalog: Database of circumstellar OH masers (Engels+, 2015)

    Science.gov (United States)

    Engels, D.; Bunzel, F.

    2015-08-01

    We present a new database of circumstellar OH masers at 1612, 1665, and 1667MHz in the Milky Way galaxy in tabular form. The database (version 2.4) contains 13655 observations and 2341 different stars detected in at least one transition and includes published data until end of 2014. Interferometric follow-up observations and monitor programs are stored in two auxiliary tables. (3 data files).

  15. VLA positions and distributions of H2O masers associated with 15 Mira and semiregular variables

    Science.gov (United States)

    Bowers, P. F.; Johnston, K. J.

    1994-05-01

    Results of VLA observations of 22 GHz H2O masers associated with 15 Mira and semiregular variables are reported. The combination of angular resolution (approximately equals 70 mas), spectral resolution (0.3 km/sec), rms sensitivity (+/- 35 mJy/beam), and hour-angle coverage is the best yet obtained for H2O masers from a significant sample of stars. Comparison of accurate optical positions of the stars with estimates from the masers yields total differences typically less than or equal to 0 sec .15-an improvement over previous comparisons by a factor of about 2. There are indications of some combination of nonuniformities in the density distribution, deviations from sphericity, and anisotropies in the velocity field, but it is difficult to disentangle the effects of these phenomena and achieve unique interpretation. A plausible model is clumps or filaments distributed at radii which vary with direction from the star. From the angular distributions and velocity ranges, there is good evidence that at least some parcels of gas are accelerated to the terminal outflow velocity at rho greater than or equal to 20 AU and that there is a component of outflow at rho approximately equals 10 to 15 AU; some gas probably is fully accelerated at radii less than 10 AU. To illustrate the problems of interpretation, the well-known case of VX Sgr is reexamined. The data do not support a simple model of increasing outflow velocity with increasing maser shell radius. It is proposed that the outflow is weakly bipolar.

  16. Phonon-assisted gain in a semiconductor double quantum dot maser.

    Science.gov (United States)

    Gullans, M J; Liu, Y-Y; Stehlik, J; Petta, J R; Taylor, J M

    2015-05-15

    We develop a microscopic model for the recently demonstrated double-quantum-dot maser. In characterizing the gain of this device we find that, in addition to the direct stimulated emission of photons, there is a large contribution from the simultaneous emission of a photon and a phonon, i.e., the phonon sideband. We show that this phonon-assisted gain typically dominates the overall gain, which leads to masing. Recent experimental data are well fit with our model.

  17. Nuclear Spin Maser Oscillation of {sup 129}Xe by Means of Optical-Detection Feedback

    Energy Technology Data Exchange (ETDEWEB)

    Yoshimi, A., E-mail: yoshimi@rarfaxp.riken.jp; Asahi, K. [RIKEN (Japan); Emori, S.; Tsukui, M.; Oshima, S. [Tokyo Institute of Technology, Department of Physics (Japan)

    2004-12-15

    We have developed the nuclear spin maser oscillating at a low frequency of 34 Hz with highly polarized nuclear spins of the noble gas element {sup 129}Xe. The system is advantageous for detecting a small frequency shift of the nuclear spin precession. We are thus planning to apply this system to the search for an atomic electric dipole moment of {sup 129}Xe. We here report the development of the system and its performance.

  18. RUBY-1

    DEFF Research Database (Denmark)

    Steg, Ph Gabriel; Mehta, Shamir R; Jukema, J Wouter

    2011-01-01

    To establish the safety, tolerability and most promising regimen of darexaban (YM150), a novel, oral, direct factor Xa inhibitor, for prevention of ischaemic events in acute coronary syndrome (ACS)....

  19. IDEA Ruby

    Institute of Scientific and Technical Information of China (English)

    段胜春

    2007-01-01

    作为一个强大的IDE,IDEA对Ruby的支持只要足够好,就已经使其捷足先登,走在别人的前面。IDEA对类似Ruby的面向对象的语言的支持还只限于一个良好的语法高亮和错误高亮。使用IDEA可以通过输入类名或方法名来打开脚本,也可以通过输入文件名的方法来打开用rspec丁文件是最通用的版本交流方式。

  20. On the Relation of Silicates and SiO Maser in Evolved Stars

    Science.gov (United States)

    Liu, Jiaming; Jiang, Biwei

    2017-04-01

    The SiO molecule is one of the candidates for the seed of silicate dust in the circumstellar envelope of evolved stars, but this opinion is challenged. In this work we investigate the relation of the SiO maser emission power and the silicate dust emission power. With both our own observation by using the PMO/Delingha 13.7 m telescope and archive data, a sample is assembled of 21 SiO v = 1, J = 2 - 1 sources and 28 SiO v = 1, J = 1 - 0 sources that exhibit silicate emission features in the ISO/SWS spectrum as well. The analysis of their SiO maser and silicate emission power indicates a clear correlation, which is not against the hypothesis that the SiO molecules are the seed nuclei of silicate dust. On the other hand, no correlation is found between SiO maser and silicate crystallinity, which may imply that silicate crystallinity does not correlate with mass-loss rate.

  1. A sensitive search for predicted methanol maser transitions with the Australia Telescope Compact Array

    CERN Document Server

    Chipman, Antony; Sobolev, Andrej; Cragg, Dinah

    2016-01-01

    We have used the Australia Telescope Compact Array (ATCA) to search for a number of centimetre wavelength methanol transitions which are predicted to show weak maser emission towards star formation regions. Sensitive, high spatial and spectral resolution observations towards four high-mass star formation regions which show emission in a large number of class II methanol maser transitions did not result in any detections. From these observations we are able to place an upper limit of <~1300K on the brightness temperature of any emission from the $3_1$A$^+$-$3_1$A$^-$, $17_{-2}$-$18_{-3}$E ($v_t=1$), $12_4$-$13_3$A$^-$, $12_4$-$13_3$A$^+$ and $4_1$A$^+$-$4_1$A$^-$ transitions of methanol in these sources on angular scales of 2 arcseconds. This upper limit is consistent with current models for class II methanol masers in high-mass star formation regions and better constraints than those provided here will likely require observations with next-generation radio telescopes.

  2. Detection of 36 GHz class I methanol maser emission towards NGCS253

    CERN Document Server

    Ellingsen, Simon; Qiao, Hai-Hua; Baan, Willem; An, Tao; Li, Juan; Breen, Shari

    2014-01-01

    We have used the Australia Telescope Compact Array (ATCA) to search for emission from the $4_{-1} \\rightarrow 3_{0}E$ transition of methanol (36.2 GHz) towards the center of the nearby starburst galaxy NGC253. Two regions of emission were detected, offset from the nucleus along the same position angle as the inner spiral arms. The emission is largely unresolved on a scale of 5 arcsec, has a full-width half maximum (FWHM) line width of < 30 km s$^{-1}$, and an isotropic luminosity orders of magnitude larger than that observed in any Galactic star formation regions. These characteristics suggest that the 36.2 GHz methanol emission is most likely a maser, although observations with higher angular and spectral resolution are required to confirm this. If it is a maser this represents the first detection of a class I methanol maser outside the Milky Way. The 36.2 GHz methanol emission in NGC253 has more than an order of magnitude higher isotropic luminosity than the widespread emission recently detected towards ...

  3. DETECTION OF 36 GHz CLASS I METHANOL MASER EMISSION TOWARD NGC 253

    Energy Technology Data Exchange (ETDEWEB)

    Ellingsen, Simon P. [School of Physical Sciences, University of Tasmania, Hobart, Tasmania (Australia); Chen, Xi; Qiao, Hai-Hua; Baan, Willem; An, Tao; Li, Juan [Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030 (China); Breen, Shari L., E-mail: Simon.Ellingsen@utas.edu.au [CSIRO Astronomy and Space Science, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710 (Australia)

    2014-08-01

    We have used the Australia Telescope Compact Array to search for emission from the 4{sub –1} → 3{sub 0} E transition of methanol (36.2 GHz) toward the center of the nearby starburst galaxy NGC 253. Two regions of emission were detected, offset from the nucleus along the same position angle as the inner spiral arms. The emission is largely unresolved on a scale of 5'', has a FWHM line width of <30 km s{sup –1}, and an isotropic luminosity orders of a magnitude larger than that observed in any Galactic star formation region. These characteristics suggest that the 36.2 GHz methanol emission is most likely a maser, although observations with higher angular and spectral resolution are required to confirm this. If it is a maser, this represents the first detection of a class I methanol maser outside the Milky Way. The 36.2 GHz methanol emission in NGC 253 has more than an order of magnitude higher isotropic luminosity than the widespread emission recently detected toward the center of the Milky Way. If emission from this transition scales with the nuclear star formation rate, then it may be detectable in the central regions of many starburst galaxies. Detection of methanol emission in ultra-luminous infrared galaxies would open up a new tool for testing for variations in fundamental constants (particularly the proton-to-electron mass ratio) on cosmological scales.

  4. High-power solid-state sapphire whispering gallery mode maser.

    Science.gov (United States)

    Creedon, Daniel L; Benmessaï, Karim; Tobar, Michael E; Hartnett, John G; Bourgeois, Pierre-Yves; Kersale, Yann; Le Floch, Jean-Michel; Giordano, Vincent

    2010-03-01

    We present new results on a cryogenic solid-state maser frequency standard, which relies on the excitation of whispering gallery (WG) modes within a doped monocrystalline sapphire resonator (alpha-Al2O3). Included substitutively within the highest purity HEMEX-grade sapphire crystal lattice are Fe2+ impurities at a concentration of parts per million, an unavoidable result of the manufacturing process. Mass conversion of Fe2+ to Fe3+ ions was achieved by thermally annealing the sapphire in air. Above-threshold maser oscillation was then excited in the resonator at zero applied DC magnetic field by pumping high-Q WG modes coincident in frequency with the electron spin resonance (ESR) energy levels of the Fe3+ spin population. A 2 stage annealing process was undertaken for a sapphire resonator with exceptionally low Fe3+ concentration, resulting in an improvement of 6 orders of magnitude in output power for this particular crystal, and exceeding the previous best implementation of our scheme in another crystal by nearly 20 dB. This represents an output signal 7 orders of magnitude more powerful than a typical commercial hydrogen maser. At this power level, we estimate a limit on the frequency stability of order 1 x 10(-17)/square root(tau) due to the Schawlow-Townes fundamental thermal noise limit.

  5. Ruby pressure scale in a low-temperature diamond anvil cell

    Science.gov (United States)

    Yamaoka, Hitoshi; Zekko, Yumiko; Jarrige, Ignace; Lin, Jung-Fu; Hiraoka, Nozomu; Ishii, Hirofumi; Tsuei, Ku-Ding; Mizuki, Jun'ichiro

    2012-12-01

    Laser-excited N and R fluorescence lines of heavily doped ruby have been studied up to 26 GPa at low temperatures. While the intensity of the R lines at ambient pressure significantly decreases with decreasing temperature, the intensity of N lines originating from exchange-coupled Cr ion pairs is enhanced at low temperatures. The pressure induced wavelength shift of the N lines at 19 K is well fitted with an empirical formula similar to the equation for the R1 line, showing that the intense N line could be used as an alternative pressure scale at low temperatures. We also observe continuous increase in non-hydrostaticity with increasing pressure at low temperatures when silicone oil and 4:1 mixture of methanol and ethanol are used as pressure media.

  6. Refinement of the twinned structure of cymrite from the Ruby Creek deposit (Alaska)

    Science.gov (United States)

    Bolotina, N. B.; Rastsvetaeva, R. K.; Kashaev, A. A.

    2010-07-01

    The mineral cymrite from the Ruby Creek deposit (Alaska) was reinvestigated by X-ray diffraction in a pseudo-orthorhombic unit cell with a = 5.3350(1) Å, b = 36.9258(8) Å, c = 7.6934(1) Å, β = 90.00(1)°. A twin law corresponding to a sixfold axis was revealed for the first time. The structure was refined in the monoclinic space group P1211 to the R factor of 5.4%. The Al and Si atoms are assumed to be ordered within a double layer. The rotation of the cation sublattice by 60° around the c axis leads to the disorder of the T sites in the crystal structure ( T = Al, Si).

  7. Very Large Array Observations of Galactic Center OH 1720 MHz Masers in Sagittarius A East and in the Circumnuclear Disk

    CERN Document Server

    Sjouwerman, L O

    2008-01-01

    We present Very Large Array (VLA) radio interferometry observations of the 1720 MHz OH masers in the Galactic Center (GC). Most 1720 MHz OH masers arise in regions where the supernova remnant Sgr A East is interacting with the interstellar medium. The majority of the newly found 1720 MHz OH masers are located to the northeast, independently indicating and confirming an area of shock interaction with the +50 km/s molecular cloud (M-0.02-0.07) on the far side of Sgr A East. The previously known bright masers in the southeast are suggested to be the result of the interaction between two supernova remnants, instead of between Sgr A East and the surrounding molecular clouds as generally found elsewhere in the Galaxy. Together with masers north of the circumnuclear disk (CND) they outline an interaction on the near side of Sgr A East. In contrast to the interaction between the +50 km/s cloud and Sgr A East, OH absorption data do not support a direct interaction between the CND material and Sgr A East. We also prese...

  8. Methanol Masers Observations in the 3-mm Bandwidth at the Radio Telescope RT-22 CrAO

    CERN Document Server

    Zubrin, S Yu; Myshenko, V V; Shulga, V M

    2007-01-01

    We report the beginning of the astronomical masers investigations in the 3-mm bandwidth at the radio telescope RT-22 (CrAO, Ukraine). For this purpose the special complex for maser lines investigation in 85...115 GHz frequency band is developed. It is made on the base of the low noise cryogenic Shottky-diode receiver and the high resolution Fourier-spectrometer. The cryogenic receiver has the DSB noise temperature less than 100K. The spectral channel separation of the Fourier-spectrometer is about 4kHz and the spectrometer bandwidth is 8 MHz. Results of maser observations of 8$^{0}-7^{1} $A$^{+}$ transition of methanol (95.169 GHz) towards DR-21(OH), DR-21W and NGC7538 are in good agreement with early obtained results by other authors. On the basis of the analysis of the location of masers in the NGC7538 direction we can assume that the origin of all known class I methanol masers in this region is connected with existing molecular outflows from young stars.

  9. Measuring Magnetic Fields from Water Masers in the Synchrotron Protostellar Jet in W3(H$_2$O)

    CERN Document Server

    Goddi, C; Moscadelli, L; Imai, H; Vlemmings, W H T; van Langevelde, H J; Sanna, A

    2016-01-01

    We report full polarimetric VLBA observations of water masers towards the Turner-Welch Object in the W3(OH) high-mass star forming complex. This object drives a synchrotron jet, which is quite exceptional for a high-mass protostar, and is associated with a strongly polarized water maser source, W3(H$_2$O), making it an optimal target to investigate the role of magnetic fields on the innermost scales of protostellar disk-jet systems. The linearly polarized emission from water masers provides clues on the orientation of the local magnetic field, while the measurement of the Zeeman splitting from circular polarization provides its strength. The water masers trace a bipolar, biconical outflow at the center of the synchrotron jet. Although on scales of a few thousand AU the magnetic field inferred from the masers is on average orientated along the flow axis, on smaller scales (10s to 100s of AU), we have revealed a misalignment between the magnetic field and the velocity vectors, which arises from the compression ...

  10. Intermittent maser flare around the high mass young stellar object G353.273+0.641 I: data & overview

    CERN Document Server

    Motogi, K; Honma, M; Minamidani, T; Takekoshi, T; Akiyama, K; Tateuchi, K; Hosaka, K; Ohishi, Y; Watanabe, Y; Habe, A; Kobayashi, H

    2011-01-01

    We have performed VLBI and single-dish monitoring of 22 GHz H$_{2}$O maser emission from the high mass young stellar object G353.273+0.641 with VERA (VLBI Exploration of Radio Astrometry) and Tomakamai 11-m radio telescope. Two maser flares have been detected, separated almost two years. Frequent VLBI monitoring has revealed that these flare activities have been accompanied by structural change of the prominent shock front traced by H2O maser alignments. We have detected only blue-shifted emissions and all maser features have been distributed within very small area of 200 $\\times$ 200 au$^{2}$ in spite of wide velocity range (> 100 km s$^{-1}$). The light curve shows notably intermittent variation and suggests that the H$_{2}$O masers in G353.273+0.641 are excited by episodic radio jet. The time-scale of \\sim2 yr and characteristic velocity of \\sim500 km s$^{-1}$ also support this interpretation. Two isolated velocity components of C50 (-53 \\pm 7 km s$^{-1}$) and C70 (-73 \\pm 7 km s$^{-1}$) have shown synchro...

  11. Water masers in Compton-thick AGN I. Detailed study of the new water megamaser in IRAS15480-0344

    CERN Document Server

    Castangia, P; Caccianiga, A; Severgnini, P; Della Ceca, R

    2016-01-01

    A relationship between the water maser detection rate and large nuclear column densities in AGN has often been cited in the literature. Indeed, detailed studies of luminous water masers, typically associated with the nuclear activity, allow us to investigate the innermost regions of AGN, with an impact on the still debated Unified Model for this class of objects.We have recently entertained a search for maser emission in a well-defined sample of Compton-thick AGN aimed at investigating, on firm statistical bases, the aforementioned relationship. While the survey is still ongoing, and is matter of a forthcoming publication, a new luminous water maser has been detected in the lenticular (field) S0 galaxy IRAS15480-0344, whose origin, associated with an accretion disc or a nuclear outflow/jet, needs to be assessed. Multi-epoch single-dish observations and VLBI measurements were performed to investigate the distribution, spatial extension, and variability of the maser emission in order to infer the main character...

  12. Accurate positions of SiO masers in active star-forming regions - Orion-KL, W51-IRS2, and Sagittarius-B2 MD5

    Science.gov (United States)

    Morita, Koh-Ichiro; Hasegawa, Tetsuo; Ukita, Nobuharu; Okumura, Sachiko K.; Ishiguro, Masato

    1992-08-01

    Accurate positional measurements of SiO J = 1-0 masers in active star-forming regions, Orion-KL, W51-IRS2, and Sgr-B2 MD5, were made with the Nobeyama Millimeter Array. Absolute positional accuracies of 0.12-0.6 arcsec were achieved. The SiO maser in W51-IRS2 is located within 0.4 arcsec (0.5 x 10 exp 17 cm at the distance of W51-IRS2) of the strongest H2O masers. In Sgr-B2 MD5, the SiO maser coincides with the strongest H2O masers, most of the strong OH masers, and the peak of radio continuum emission from the ultracompact H II region within 0.7 arcsec (0.8 x 10 exp 17 cm at the distance of Sgr-B2). Peaks of the emission from hot NH3 were found to exist within about 1 arcsec of the SiO masers in both regions. The precise positional coincidence confirms our former conclusion that the SiO masers in W51-IRS2 and Sgr-B2 MD5 are actually associated with the ongoing activity of star formation, as is the case of Orion-KL.

  13. The mouse ruby-eye 2(d) (ru2(d) /Hps5(ru2-d) ) allele inhibits eumelanin but not pheomelanin synthesis.

    Science.gov (United States)

    Hirobe, Tomohisa; Ito, Shosuke; Wakamatsu, Kazumasa

    2013-09-01

    The novel mutation named ru2(d) /Hps5(ru2-d) , characterized by light-colored coats and ruby-eyes, prohibits differentiation of melanocytes by inhibiting tyrosinase (Tyr) activity, expression of Tyr, Tyr-related protein 1 (Tyrp1), Tyrp2, and Kit. However, it is not known whether the ru2(d) allele affects pheomelanin synthesis in recessive yellow (e/Mc1r(e) ) or in pheomelanic stage in agouti (A) mice. In this study, effects of the ru2(d) allele on pheomelanin synthesis were investigated by chemical analysis of melanin present in dorsal hairs of 5-week-old mice from F2 generation between C57BL/10JHir (B10)-co-isogenic ruby-eye 2(d) and B10-congenic recessive yellow or agouti. Eumelanin content was decreased in ruby-eye 2(d) and ruby-eye 2(d) agouti mice, whereas pheomelanin content in ruby-eye 2(d) recessive yellow and ruby-eye 2(d) agouti mice did not differ from the corresponding Ru2(d) /- mice, suggesting that the ru2(d) allele inhibits eumelanin but not pheomelanin synthesis. © 2013 John Wiley & Sons A/S. Published by John Wiley & Sons Ltd.

  14. THE PROTOCLUSTER G18.67+0.03: A TEST CASE FOR CLASS I CH{sub 3}OH MASERS AS EVOLUTIONARY INDICATORS FOR MASSIVE STAR FORMATION

    Energy Technology Data Exchange (ETDEWEB)

    Cyganowski, C. J.; Zhang, Q. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Brogan, C. L.; Hunter, T. R.; Friesen, R. K.; Indebetouw, R. [NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 (United States); Chandler, C. J., E-mail: ccyganowski@cfa.harvard.edu [NRAO, 1003 Lopezville Road, Socorro, NM 87801 (United States)

    2012-12-01

    We present high angular resolution Submillimeter Array and Karl G. Jansky Very Large Array observations of the massive protocluster G18.67+0.03. Previously targeted in maser surveys of GLIMPSE Extended Green Objects (EGOs), this cluster contains three Class I CH{sub 3}OH maser sources, providing a unique opportunity to test the proposed role of Class I masers as evolutionary indicators for massive star formation. The millimeter observations reveal bipolar molecular outflows, traced by {sup 13}CO(2-1) emission, associated with all three Class I maser sources. Two of these sources (including the EGO) are also associated with 6.7 GHz Class II CH{sub 3}OH masers; the Class II masers are coincident with millimeter continuum cores that exhibit hot core line emission and drive active outflows, as indicated by the detection of SiO(5-4). In these cases, the Class I masers are coincident with outflow lobes, and appear as clear cases of excitation by active outflows. In contrast, the third Class I source is associated with an ultracompact (UC) H II region, and not with Class II masers. The lack of SiO emission suggests that the {sup 13}CO outflow is a relic, consistent with its longer dynamical timescale. Our data show that massive young stellar objects (MYSOs) associated only with Class I masers are not necessarily young and provide the first unambiguous evidence that Class I masers may be excited by both young (hot core) and older (UC H II) MYSOs within the same protocluster.

  15. The 6-GHz methanol multibeam maser catalogue - IV. Galactic longitudes 186°-330° including the Orion-Monoceros region

    Science.gov (United States)

    Green, J. A.; Caswell, J. L.; Fuller, G. A.; Avison, A.; Breen, S. L.; Ellingsen, S. P.; Gray, M. D.; Pestalozzi, M.; Quinn, L.; Thompson, M. A.; Voronkov, M. A.

    2012-03-01

    We present the fourth portion of a Galactic plane survey of methanol masers at 6668 MHz, spanning the longitude range 186°-330°. We report 207 maser detections, 89 new to the survey. This completes the southern sky part of the methanol multibeam survey and includes a large proportion of new sources, 43 per cent. We also include results from blind observations of the Orion-Monoceros star-forming region, formally outside the latitude range of the methanol multibeam survey; only the four previously known methanol emitting sites were detected, of which we present new positions and spectra for masers at Orion A (south) and Orion B, obtained with the Multi-Element Radio Linked Interferometer Network (MERLIN) array.

  16. H2O masers in a jet-driven bowshock: Episodic ejection from a massive young stellar object

    CERN Document Server

    Burns, R A; Nagayama, T; Sunada, K; Omodaka, T

    2016-01-01

    We report the results of VERA multi-epoch VLBI 22 GHz water maser observations of S255IR-SMA1, a massive young stellar object located in the S255 star forming region. By annual parallax the source distance was measured as D = 1.78 +-0.12 kpc and the source systemic motion was (u alpha cos d, u d) = (-0.13 +- 0.20, -0.06 +- 0.27) mas yr-1. Masers appear to trace a U-shaped bow shock whose morphology and proper motions are well reproduced by a jet-driven outflow model with a jet radius of about 6 AU. The maser data, in the context of other works in the literature, reveal ejections from S255IR-SMA1 to be episodic, operating on timescales of ~1000 years.

  17. The 6-GHz methanol multibeam maser catalogue IV: Galactic longitudes 186 to 330 including the Orion-Monoceros region

    CERN Document Server

    Green, J A; Fuller, G A; Avison, A; Breen, S L; Ellingsen, S P; Gray, M D; Pestalozzi, M; Quinn, L; Thompson, M A; Voronkov, M A

    2012-01-01

    We present the fourth portion of a Galactic Plane survey of methanol masers at 6668 MHz, spanning the longitude range 186 degrees to 330 degrees. We report 207 maser detections, 89 new to the survey. This completes the southern sky part of the Methanol Multibeam survey and includes a large proportion of new sources, 43%. We also include results from blind observations of the Orion-Monoceros star forming region, formally outside the latitude range of the Methanol Multibeam survey; only the four previously known methanol emitting sites were detected, of which we present new positions and spectra for masers at Orion-A (south) and Orion-B, obtained with the MERLIN array.

  18. Maser Emission toward the Infrared Dark Cloud G359.94+0.17 Seen in Silhouette against the Galactic Center

    CERN Document Server

    Deguchi, S; Shino, N

    2011-01-01

    The infrared dark cloud G359.94+0.17 is a conspicuous, opaque cloud, which is seen in silhouette against the Galactic center. We found unexpectedly strong (~50 Jy) maser emission of CH3OH at 44 GHz with additional weak 22 GHz H2O maser and 43 GHz SiO thermal emissions toward this cloud. Detections of these molecular lines indicate that strong star forming activities are proceeding in this cloud, which were not reported previously despite of numerous works toward the Galactic center.The line profiles of the NH3 inversion lines at 23 GHz indicate that G359.94+0.17 is composed of three clouds with V(lsr)= 0, 15 and ~80 km/s overlapped on the line of sight. The maser emission is associated with the 15 km/s cloud, suggesting that it is located at the Norma spiral arm.

  19. Laboratory model for the study and treatment of traumatic tattoos with the Q-switched ruby laser

    Science.gov (United States)

    Silverman, Richard T.; Lach, Elliot

    1994-09-01

    The outcome of laser tattoo removal is dependent on the type of laser and characteristics of the tattoo. A rabbit model was developed to study the Q-switched ruby laser in the treatment of traumatic tattooing. On the backs of white New Zealand rabbits, three 3 cm patches were dermabraded and dressed with carbon black and antibiotic ointment. After a healing period of eight weeks, pre-treatment biopsies were obtained, and the rabbits were treated with the Q- switched ruby laser at various fluence settings with a pulse width of 34 nsec. At set intervals, further biopsies were obtained and studied with light and electron microscopic analysis, and photodocumentation was performed. Grossly, clearance of the tattooed areas was noted in the laser treated specimens. More effective clearance was observed with higher fluence treatment. No infections occurred, and hair regrowth was noted in all cases, though the rate seemed to be altered by laser treatment.

  20. A Testing Ground for Polarized Maser Transport: Multi-Epoch Analysis of a π/2 Electric Vector Rotation

    Science.gov (United States)

    Tobin, Taylor; Kemball, Athol J.

    2017-01-01

    The near circumstellar environment (NCSE) around Asymptotic Giant Branch (AGB) stars is chaotic, exhibiting shocks, turbulence, velocity gradients, and a potentially dynamically significant magnetic field (Vlemmings et al. 2005). Very Long Baseline Interferometry (VLBI) of masers emanating from these environments can provide sub-milliarcsecond angular resolution of the NCSE (Kemball 2002). Solidifying the origin of the polarization in these masers may be the key to understanding the magnitude and behavior of these stars' magnetic fields (eg. Goldreich et al. 1973; Elitzur 1996). However, other theories of polarized maser transport do not rely heavily on the magnetic field; some are more dependent on anisotropic pumping (Elitzur 1996; Watson 2009) or anisotropic resonant scattering (Asensio Ramos et al. 2005; Houde 2014). One optimal test of these theories is their ability to account for a π/2 rotation of the Electric Vector Position Angle (EVPA) observed in some maser features. The profile of linear polarization across such a feature varies with the generating mechanism. In this study, we utilize multi-epoch observations of ν=1, J=1-0 SiO maser emission around TX Cam (Diamond & Kemball 2003; Kemball et al. 2009; Gonidakis et al. 2010) to analyze a single feature with a π/2 rotation that persisted for five epochs and compare it to the behavior expected according to various theories of maser polarization. In addition, we analyze the low levels of circular polarization - now achievable due to recent improvements in millimeter-wavelength circular polarization reduction (Kemball & Richter 2011) - and compare their correlation with other parameters to further test these polarization generation theories.