WorldWideScience

Sample records for inaf osservatorio astrofisico

  1. Italy INAF Data Center Report

    Science.gov (United States)

    Negusini, M.; Sarti, P.

    2013-01-01

    This report summarizes the activities of the Italian INAF VLBI Data Center. Our Data Center is located in Bologna, Italy and belongs to the Institute of Radioastronomy, which is part of the National Institute of Astrophysics.

  2. Italy INAF Analysis Center Report

    Science.gov (United States)

    Negusini, M.; Sarti, P.

    2013-01-01

    This report summarizes the activity of the Italian INAF VLBI Analysis Center. Our Analysis Center is located in Bologna, Italy and belongs to the Institute of Radioastronomy, which is part of the National Institute of Astrophysics. IRA runs the observatories of Medicina and Noto, where two 32-m VLBI AZ-EL telescopes are situated. This report contains the AC's VLBI data analysis activities and shortly outlines the investigations into the co-locations of space geodetic instruments.

  3. Reale Osservatorio Vesuviano: the First Volcanological Observatory in the World

    Science.gov (United States)

    Avvisati, Gala; de Vita, Sandro; Di Vito, Mauro Antonio; Marotta, Enrica; Sangianantoni, Agata; Peluso, Rosario; Pasquale Ricciardi, Giovanni; Tulino, Sabrina; Uzzo, Tullia; Ghilardi, Massimo; De Natale, Giuseppe

    2015-04-01

    The Reale Osservatorio Vesuviano (ROV), historic home of the Istituto Nazionale di Geofisica e Vulcanologia (INGV), is the oldest volcanological observatory in the world. It was founded in 1841 by the Bourbon king of Naples. The building is located on the western slope of Mount Vesuvius, one of the most famous and dangerous volcanoes in the world. Since its foundation, the ROV has always attracted researchers, visitors and students from many countries. The ROV site is an elegant neo-classical building which at present hosts permanent exhibitions of part of its inheritance of valuable mineral, scientific instrument and art collections. A radical change is now under way, starting with the structural reinforcement of the building, renewal and upgrading of services, and the redefinition of exhibition itineraries so as to make visits still more enjoyable and informative. This will include the integration of outdoor footpaths and theme-based routes designed for users of differing levels of expertise. This major transformation also involves a study and a number of operations aimed at the possibility of developing self-financed activities. To this end an analysis of tourist movements in Campania was conducted, in part so as to attract to the ROV a larger and more varied group of visitors. In an area that - despite its unique characteristics - is currently significantly degraded and underused, the creation of such a powerful tourist and cultural attraction would serve as a focus for the development of additional activities and services that would greatly enhance it and stimulate growth. These activities would, of course, be compatible with a territory that has a high risk of volcanic hazards - indeed, such growth would constitute an important component in mitigating this risk in the area. The example given illustrates how the restoration and enhancement of a piece of our historic, scientific and cultural heritage could be the driving force behind the economic revival of an

  4. CRIS-INAF as a Result of a Fruitful Collaboration among ITs, Librarians, and Researchers

    Science.gov (United States)

    Konomi, E.; Marra, M.

    2015-04-01

    The Current Research Information System of the Istituto Nazionale di Astrofisica (CRIS-INAF) is an institutional database for the entire scientific and technological output of INAF's staff, which consists of more than 2000 people. It was set up in 2009 in order to provide real-time information and statistics on the global activity of the Institute. The system — which offers the widest global coverage of INAF's research output as compared to other relevant commercial or institutional databases — is the result of the co-operation among four main sets of actors: information technologists, for system development; librarians/documentalists, who provide expertise in library science; administrative personnel, for central and local management of staff and structures; and researchers, mainly for data provision and validation. The original design, maintenance, and implementation of new features have been historically provided by the project coordinator with the help of an advisory committee (1 or 2 members for each research structure) that includes representatives of the four professional set of actors mentioned above. Presently, CRIS-INAF is under revision to reorganize the database structure as well as optimize its interoperability with SAO/NASA ADS and with the institute's administrative databases. The introduction of additional functionalities is being considered. This paper describes some characteristics of the fruitful inter-professional cooperation which has been essential for the functionality and improvements of the system.

  5. L'Osservatorio delle disuguaglianze dell'Azienda USL di Ferrara

    Directory of Open Access Journals (Sweden)

    A. De Togni

    2003-05-01

    Full Text Available

    È ormai riconosciuto che bassa condizione socio-economica e limitato sviluppo culturale possono agire negativamente sul benessere individuale e sul livello di salute collettiva e determinano criticità nell’accesso alle cure, fenomeni che appaiono prevedibili, prevenibili e correggibili per migliorare la qualità e l’efficienza del sistema sanitario. Nell’area ferrarese sono presenti situazioni di svantaggio relativo non riconosciute e di difficile individuazione, il cui miglioramento si tradurrebbe in un beneficio sia per la condizione individuale che per la collettività.

    Obiettivi: la direzione sanitaria ed il Dipartimento di Sanità Pubblica dell’Azienda USL e l’Università degli Studi di Ferrara hanno dato vita al progetto “Osservatorio sulle disuguaglianze” allo scopo di sperimentare nuove modalità informative, più agili e tempestive delle rilevazioni censuarie, per individuare aree geografiche e/o fasce di popolazione verso le quali promuovere azioni di contrasto alle disuguaglianze in salute.

    Metodi: l’osservatorio prevede inizialmente tre sottoprogetti: 1. accesso agli screening femminili per definire i determinanti socio-ambientali e culturali delle donne non rispondenti; 2. salute neonati che, sulla base del nuovo certificato di assistenza al parto (CEDAP, mira a valutare situazioni di disuguaglianza in una fascia di età molto fragile; 3. coinvolgimento di medici di medicina generale (MMG, aderenti volontariamente all’indagine, nella raccolta sistematica di informazioni utili a monitorare il fenomeno delle disuguaglianze nella popolazione ferrarese. Risultati: l’attività dell’osservatorio è iniziata nell’aprile 2003 con l’elaborazione di un questionario da presentare alle donne non aderenti allo screening dei tumori del collo uterino e con la valutazione delle modalità di somministrazione del questionario (postale o telefonico avvalendosi della

  6. Automated processing of thermal infrared images of Osservatorio Vesuviano permanent surveillance network by using Matlab code

    Science.gov (United States)

    Sansivero, Fabio; Vilardo, Giuseppe; Caputo, Teresa

    2017-04-01

    The permanent thermal infrared surveillance network of Osservatorio Vesuviano (INGV) is composed of 6 stations which acquire IR frames of fumarole fields in the Campi Flegrei caldera and inside the Vesuvius crater (Italy). The IR frames are uploaded to a dedicated server in the Surveillance Center of Osservatorio Vesuviano in order to process the infrared data and to excerpt all the information contained. In a first phase the infrared data are processed by an automated system (A.S.I.R.A. Acq- Automated System of IR Analysis and Acquisition) developed in Matlab environment and with a user-friendly graphic user interface (GUI). ASIRA daily generates time-series of residual temperature values of the maximum temperatures observed in the IR scenes after the removal of seasonal effects. These time-series are displayed in the Surveillance Room of Osservatorio Vesuviano and provide information about the evolution of shallow temperatures field of the observed areas. In particular the features of ASIRA Acq include: a) efficient quality selection of IR scenes, b) IR images co-registration in respect of a reference frame, c) seasonal correction by using a background-removal methodology, a) filing of IR matrices and of the processed data in shared archives accessible to interrogation. The daily archived records can be also processed by ASIRA Plot (Matlab code with GUI) to visualize IR data time-series and to help in evaluating inputs parameters for further data processing and analysis. Additional processing features are accomplished in a second phase by ASIRA Tools which is Matlab code with GUI developed to extract further information from the dataset in automated way. The main functions of ASIRA Tools are: a) the analysis of temperature variations of each pixel of the IR frame in a given time interval, b) the removal of seasonal effects from temperature of every pixel in the IR frames by using an analytic approach (removal of sinusoidal long term seasonal component by using a

  7. Sviluppi di Ricevitori E di Componentistica Per Banda 3 mm Ad INAF-OA Cagliari

    Science.gov (United States)

    Navarrini, Alessandro

    2017-11-01

    L'INAF-OA Cagliari (OACa) sta sviluppando un ricevitore criogenico a basso rumore basato su un mixer SSB (Single Side Band) a superconduttore SIS (Superconductor-Insulator-Superconductor) per la banda 3 mm. Il ricevitore, acquistato da IRAM, è stato fortemente modificato per essere adattato al fuoco Gregoriano di SRT (Sardinia Radio Telescope). Lo strumento è caratterizzato da una nuova criogenia a ciclo chiuso 4 K (per evitare l'uso di elio liquido in antenna), da un nuovo oscillatore locale (di tipo ALMA Banda 3) e da un nuovo sistema di controllo e di monitoraggio basato su schede Raspberry ed Arduino sviluppato ad OACa. Verranno presentati i recenti sviluppi sul ricevitore, inclusi i risultati preliminari della misura della temperatura di rumore, che raggiunge un valore pari a Trec=66 K alla frequenza di 86 GHz, nonostante la criogenia non sia ancora ottimizzata. L'INAF-OACa è coinvolto nel progetto AETHRA (Advanced European Technologies for Heterodyne Receivers for Astronomy) nel quadro del programma Radionet/Horizon2020 per il quale sta contribuendo al WP1 (Work Package 1). Lo scopo del WP1 è di sviluppare e costruire un dimostratore di un array di ricevitori a doppia polarizzazione per la banda 3 mm basato su amplificatori criogenici a basso rumore (LNA) in tecnologia a semiconduttore MMIC. Nell'ambito del WP1 l'OACa ha in carico il progetto di un OrthomodeTransducer (OMT) in guida d'onda o in tecnologia planare per la banda 72-116 GHz che sia integrabile con amplificatori MMICs ed adatto all'integrazione in un array da installare nel piano focale di un radiotelescopio. Verranno presentati i design preliminari degli OMT per AETHRA, che sono basati su prototipi sviluppati in passato da OACa.

  8. What does the InOMN mean to a national research institute like INAF?

    Science.gov (United States)

    Boccato, C.

    2011-10-01

    I could not resist the temptation to use the slogan of InOMN 2011 for the title of this abstract; in addition to the description of our past experience in InOMN 2010, it has offered me the opportunity to share with you why a scientific research institute should promote this kind of event. The National Institute for Astrophysics is the main institute in Italy for research in this field. If, in one the hand, INAF is due to spread its scientific results to the public, then, on the other hand, it follows that an immediate link between public observation of the Moon, using little telescopes, and these results is not present. The reason why we should participate in InOMN can be summarized in one single word: humility. The Moon is the nearer celestial object that everybody can watch; it is the bridge between common people and astronomers. The first thing to do is see the sky, and then you can watch it. These first two steps are affordable to everyone without any additional help. In a third step you can observe it. Only at the very end of this process you can study the sky. These two last steps usually need a support from professionals. Observing the Moon with professionals narrows the gap between scientists and common people and opens the road to comprehension of astrophysical laws. Reaching more than ten thousand people from all over our country, as was the case for InOMN 2010, is not only important, but necessary for our institute; in this way, we raise the social consensus of our work, stimulate the younger generation to follow scientific study, and create a network with astronomy amateurs: all of which are essential to organizing these kinds of events. We used all possible channels to spread news about the event, including the Web and social networks (such as Facebook and Twitter), which we customized according to our language and cultural context. Using this approach, we covered all of Italy, with the additional help of astronomy amateurs and by investing a bit of

  9. San Francisco Syncope Rule, Osservatorio Epidemiologico sulla Sincope nel Lazio risk score, and clinical judgment in the assessment of short-term outcome of syncope.

    Science.gov (United States)

    Dipaola, Franca; Costantino, Giorgio; Perego, Francesca; Borella, Marta; Galli, Andrea; Cantoni, Giulia; Barbic, Franca; Casella, Francesco; Duca, Pier Giorgio; Furlan, Raffaello

    2010-05-01

    The study aimed to compare the efficacy of the Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) risk score, San Francisco Syncope Rule, and clinical judgment in assessing the short-term prognosis of syncope. We studied 488 patients consecutively seen for syncope at the emergency department of 2 general hospitals between January and July 2004. Sensitivity, specificity, predictive values, and likelihood ratios for short-term (within 10 days) severe outcomes were computed for each decision rule and clinical judgment. Severe outcomes comprised death, major therapeutic procedures, and early readmission to hospital. Clinical judgment had a sensitivity of 77%, a specificity of 69%, and would have admitted less patients (34%, P < .05 vs decision rules). The OESIL risk score was characterized by a sensitivity of 88% and a specificity of 60% (admission 43%). San Francisco Syncope Rule sensitivity was 81% and specificity was 63% (admission 40%). According to both clinical rules, no discharged patient would have died. With combined OESIL risk score and clinical judgment, the probability of adverse events was 0.7% for patients with both low risk scores, whereas that for both high risk scores was roughly 16%. Because of a relatively low sensitivity, both risk scores were partially lacking in recognizing patients with short-term high-risk syncope. However, the application of the decision rules would have identified all patients who subsequently died, and OESIL risk score and clinical judgment combined seem to improve the decision-making process concerning the identification of high-risk patients who deserve admission. (c) 2010 Elsevier Inc. All rights reserved.

  10. Thermal inertia of near-Earth asteroids and magnitude of the Yarkovsky effect

    NARCIS (Netherlands)

    Delbo, M.; Dell'Oro, A.; Harris, A. W.; Mottola, S.; Mueller, M.

    2006-01-01

    Thermal inertia of near-Earth asteroids and magnitude of the Yarkovsky effect M. Delbo* (1,2), A. Dell'Oro (2), A. W. Harris (3), S. Mottola (3), M. Mueller (3) (1) Observatoire de la Côte d'Azur B.P. 4229, 06034 Nice Cedex 4, France. (2) INAF-Osservatorio Astr. di Torino, via Osservatorio 20, 10025

  11. Growing Galaxies Gently

    Science.gov (United States)

    2010-10-01

    helium as "heavy elements". [2] By carefully splitting up the faint light coming from a galaxy into its component colours using powerful telescopes and spectrographs, astronomers can identify the fingerprints of different chemicals in remote galaxies, and measure the amounts of heavy elements present. With the SINFONI instrument on the VLT astronomers can go one better and get a separate spectrum for each part of an object. This allows them to make a map that shows the quantity of heavy elements present in different parts of a galaxy and also determine where in the galaxy star formation is occurring most vigorously. More information This research was presented in a paper, Gas accretion in distant galaxies as the origin of chemical abundance gradients, by Cresci et al., to appear in Nature on 14 October 2010. The team is composed of G. Cresci (Osservatorio Astrofisico di Arcetri, Italy), F. Mannucci (Osservatorio Astrofisico di Arcetri, Italy), R. Maiolino (INAF, Osservatorio Astronomico di Roma, Italy), A. Marconi (Universitá di Firenze, Italy), A. Gnerucci (Universitá di Firenze, Italy) and L. Magrini (Osservatorio Astrofisico di Arcetri, Italy). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world's most advanced visible

  12. Workshop on The Golden Age of Cataclysmic Variables and Related Objects - II .

    Directory of Open Access Journals (Sweden)

    Editorial, Foreword

    2015-02-01

    Full Text Available Organizing Institutions:INAF – Istituto di Astrofisica e Planetologia Spaziali, Roma – INAF-IAPS, Roma, ItalyINTA – Dpt. de Cargas Utiles y Ciencias del Espacio, INTA-DCUCE, Madrid, SpainCzech Republic Academy of Sciences – Astronomical Institute, ASCR-AI, Ondřejov, Czech RepublicCzech Technical University, CTU in Prague, Czech RepublicDepartment of Physics, Technion, Haifa, IsraelRussian Academy of Sciences – Institute of Astronomy, RAS-IA, Moscow, RussiaINAF - Osservatorio Astronomico di Capodimonte, INAF-OAC, Napoli, ItalyDepartment of Astronomy, University of Washington, Seattle, WA, USA

  13. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Instituto de Astronomía, Universidad Nacional Autónoma de México, Aptdo. Postal 70-264, México, D.F. 04510, Mexico. INAF, Osservatorio Astronomico di Padova, Vicolo dell Osservatorio 5, 35122 Padova, Italy. Instituto de Astronomía de Andalucía (CSIC), C/ Camino Bajo de Huetor 50, 18008 Granada, ...

  14. DREAMS: a payload on-board the ExoMars EDM Schiaparelli for the characterization of Martian environment during the statistical dust storm season

    Science.gov (United States)

    Molfese, Cesare; Esposito, Francesca; Debei, Stefano; Bettanini, Carlo; Arruego Rodríguez, Ignacio; Colombatti, Giacomo; Harri, Ari-Matty.; Montmessin, Franck; Wilson, Colin; Aboudan, Alessio; Mugnuolo, Raffaele; Pirrotta, Simone; Marchetti, Ernesto; Witasse, Olivier

    2015-04-01

    F. Esposito1, S. Debei2, C. Bettanini2, C. Molfese1, I. Arruego Rodríguez3, G. Colombatti2, A-M. Harri4, F. Montmessin5, C. Wilson6, A. Aboudan2, S. Abbaki5, V. Apestigue3, G. Bellucci7, J-J. Berthelier5, J. R. Brucato8, S. B. Calcutt6, F. Cortecchia1, F. Cucciarrè2, G. Di Achille1, F. Ferri2, F. Forget9, E. Friso2, M. Genzer4, P. Gilbert5, H. Haukka4, J. J. Jiménez3, S. Jiménez10, J-L. Josset11, O. Karatekin12, G. Landis13, R. Lorenz14, J. Martinez3, L. Marty1, V. Mennella1, D. Möhlmann15, D. Moirin5, R. Molinaro1, E. Palomba7, M. Patel16, J-P. Pommereau5, C.I. Popa1, S. Rafkin17, P. Rannou18, N.O. Renno19, P. Schipani1, W. Schmidt4, E. Segato2, S. Silvestro1, F. Simoes20, A. Spiga9, F. Valero21, L. Vázquez21, F. Vivat5, O. Witasse22, R. Mugnuolo23, S. Pirrotta23, E.Marchetti23 1INAF - Osservatorio Astronomico di Capodimonte, Napoli, Italy, 2CISAS - Università degli Studi di Padova, Padova, Italy, 3INTA, Spain, 4Finnish Meteorological Institute (FMI),Helsinki, Finland, 5LATMOS - CNRS/UVSQ/IPSL, France, 6Oxford University, Oxford, United Kingdom, 7INAF - Istituto di Fisica dello Spazio Interplanetario (IFSI), 8INAF-Osservatorio Astrofisico di Arcetri, 9CNRS, LMD, France, 10Universidad Politécnica de Madrid, Spain, 11Space Exploration Institute, Switzerland, 12Royal Observatory of Belgium,Belgium, 13NASA, GRC, USA, 14JHU Applied Physics Lab (JHU-APL), USA, 15DLR PF Leitungsbereich, Berlin, Germany, 16Open University, UK, 17SwRL, Switzerland, 18GSMA, France, 19University of Michigan, USA, 20NASA, GSFC, USA, 21Universidad Complutense de Madrid (UCM), Spain, 22ESA-ESTEC, Noordwijk, The Netherlands, 23Italian Space Agency, Italy DREAMS (Dust characterization, Risk assessment and Environment Analyzer on the Martian Surface) package is an integrated multi-sensor scientific payload dedicated to characterizing the landing site environment in dusty conditions. It will measure pressure, wind speed and direction, relative humidity, temperature, the solar irradiance

  15. The INAF/IAPS Plasma Chamber for ionospheric simulation experiment

    Science.gov (United States)

    Diego, Piero

    2016-04-01

    The plasma chamber is particularly suitable to perform studies for the following applications: - plasma compatibility and functional tests on payloads envisioned to operate in the ionosphere (e.g. sensors onboard satellites, exposed to the external plasma environment); - calibration/testing of plasma diagnostic sensors; - characterization and compatibility tests on components for space applications (e.g. optical elements, harness, satellite paints, photo-voltaic cells, etc.); - experiments on satellite charging in a space plasma environment; - tests on active experiments which use ion, electron or plasma sources (ion thrusters, hollow cathodes, field effect emitters, plasma contactors, etc.); - possible studies relevant to fundamental space plasma physics. The facility consists of a large volume vacuum tank (a cylinder of length 4.5 m and diameter 1.7 m) equipped with a Kaufman type plasma source, operating with Argon gas, capable to generate a plasma beam with parameters (i.e. density and electron temperature) close to the values encountered in the ionosphere at F layer altitudes. The plasma beam (A+ ions and electrons) is accelerated into the chamber at a velocity that reproduces the relative motion between an orbiting satellite and the ionosphere (≈ 8 km/s). This feature, in particular, allows laboratory simulations of the actual compression and depletion phenomena which take place in the ram and wake regions around satellites moving through the ionosphere. The reproduced plasma environment is monitored using Langmuir Probes (LP) and Retarding Potential Analyzers (RPA). These sensors can be automatically moved within the experimental space using a sled mechanism. Such a feature allows the acquisition of the plasma parameters all around the space payload installed into the chamber for testing. The facility is currently in use to test the payloads of CSES satellite (Chinese Seismic Electromagnetic Satellite) devoted to plasma parameters and electric field measurements in a polar orbit at 500 km altitude.

  16. The Gaia-ESO Survey: Low-α element stars in the Galactic bulge

    Science.gov (United States)

    Recio-Blanco, A.; Rojas-Arriagada, A.; de Laverny, P.; Mikolaitis, S.; Hill, V.; Zoccali, M.; Fernández-Trincado, J. G.; Robin, A. C.; Babusiaux, C.; Gilmore, G.; Randich, S.; Alfaro, E.; Allende Prieto, C.; Bragaglia, A.; Carraro, G.; Jofré, P.; Lardo, C.; Monaco, L.; Morbidelli, L.; Zaggia, S.

    2017-06-01

    We take advantage of the Gaia-ESO Survey iDR4 bulge data to search for abundance anomalies that could shed light on the composite nature of the Milky Way bulge. The α-element (Mg, Si, and whenever available, Ca) abundances, and their trends with Fe abundances have been analysed for a total of 776 bulge stars. In addition, the aluminum abundances and their ratio to Fe and Mg have also been examined. Our analysis reveals the existence of low-α element abundance stars with respect to the standard bulge sequence in the [α/ Fe] versus [Fe/H] plane. Eighteen objects present deviations in [α/ Fe] ranging from 2.1 to 5.3σ with respect to the median standard value. Those stars do not show Mg-Al anti-correlation patterns. Incidentally, this sign of the existence of multiple stellar populations is reported firmly for the first time for the bulge globular cluster NGC 6522. The identified low-α abundance stars have chemical patterns that are compatible with those of the thin disc. Their link with massive dwarf galaxies accretion seems unlikely, as larger deviations in α abundance and Al would be expected. The vision of a bulge composite nature and a complex formation process is reinforced by our results. The approach used, which is a multi-method and model-driven analysis of high resolution data, seems crucial to reveal this complexity. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, and prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council.

  17. The Dark Side of Nature: the Crime was Almost Perfect

    Science.gov (United States)

    2006-12-01

    Astrofisico di Arcetri, Italy), Guido Chincarini (INAF, Osservatorio Astronomico di Brera & Università degli Studi di Milano-Bicocca, Italy), Nino Panagia (Space Telescope Science Institute, USA), Gianpiero Tagliaferri, Dino Fugazza, Sergio Campana, Stefano Covino, and Paolo D'Avanzo (INAF, Osservatorio Astronomico di Brera, Italy), Daniele Malesani (SISSA/ISAS, Italy and Dark Cosmology Centre, Copenhagen), Vincenzo Testa, L. Angelo Antonelli, Silvia Piranomonte, and Luigi Stella (INAF, Osservatorio Astronomico di Roma, Italy), Vanessa Mangano (INAF/IASF Palermo, Italy), Kevin Hurley (University of California, Berkeley, USA), I. Felix Mirabel (ESO), and Leonardo J. Pellizza (Instituto de Astronomia y Fisica del Espacio). The Danish-led team is composed of Johan P. U. Fynbo, Darach Watson, Christina C. Thöne, Tamara M. Davis, Jens Hjorth, José Mará Castro Cerón, Brian L. Jensen, Maximilian D. Stritzinger, and Dong Xu (Dark Cosmology Centre, University of Copenhagen, Denmark), Jesper Sollerman (Dark Cosmology Centre and Department of Astronomy, Stockholm University, Sweden), Uffe G. Jørgensen, Tobias C. Hinse, and Kristian G. Woller (Niels Bohr Institute, University of Copenhagen), Joshua S. Bloom, Daniel Kocevski, Daniel Perley (Department of Astronomy, University of California at Berkeley, USA), Páll Jakobsson (Centre for Astrophysics Research, University of Hertfordshire, UK), John F. Graham and Andrew S. Fruchter (Space Telescope Science Institute, Baltimore, USA), David Bersier (Astrophysics Research Institute, Liverpool John Moores University, UK), Lisa Kewley (University of Hawaii, Institute of Astronomy, USA), Arnaud Cassan and Marta Zub (Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Germany), Suzanne Foley (School of Physics, University College Dublin, Ireland), Javier Gorosabel (Instituto de Astrofisica de Andalucia, Granada, Spain), Keith D. Horne (SUPA Physics/Astronomy, University of St Andrews, Scotland, UK), Sylvio

  18. [The management of syncope in the hospital: the OESIL Study (Osservatorio Epidemiologico della Sincope nel Lazio)].

    Science.gov (United States)

    Ammirati, F; Colivicchi, F; Minardi, G; De Lio, L; Terranova, A; Scaffidi, G; Rapino, S; Proietti, F; Bianchi, C; Uguccioni, M; Carunchio, A; Azzolini, P; Neri, R; Accogli, S; Sunseri, L; Orazi, S; Mariani, M; Fraioli, R; Calcagno, S; De Luca, F; Santini, M

    1999-05-01

    While syncope is generally considered a frequent finding in clinical practice, no clear epidemiological evidence is available about the relevance of such an event in the general population of Italy. The OESIL Study was designed and undertaken in 15 hospitals of the Italian region of Latium in order to assess the percentage of emergency-room visits and admissions due to syncope, as well as to analyze the in-hospital diagnostic work-up performed for this condition. During a two-month observation period, 781 (372 males and 409 females, mean age 55.2 (22.8 years) consecutive patients came to the emergency rooms of the 15 hospitals included in the investigation due to a syncope spell (0.9% of emergency room visits); 450/781 patients (57.6%) were subsequently hospitalized (1.3% of all admissions): 48.0% of the admissions were admitted to a general medical ward, 29.3% to an observation ward, 13.3% to a cardiology section, 1.6% to a neurology section and 7.8% to other clinical sections (neurosurgery, general surgery). The mean duration of in-hospital stay was 6.9 (5.8 days; range 1-40 days). During the hospitalization period, 93.1% of patients underwent an ECG, 51.0% an EEG, 44.3% a CT scan of the central nervous system, 40.2% an echocardiogram and 19.5% a tilt-test. The syncope spell was considered to have a cardiovascular origin in 33.8% of the cases and a non-cardiovascular in 11.6% of the cases, while the origin was unknown in 54.4% of the cases. Collected data support the idea that syncope represents a frequent event in the general population and is responsible for a significant percentage of emergency-room visits and hospital admissions. However, the performance of conventional diagnostic work-ups is far from being satisfactory.

  19. GAPS Programme with HARPS-N@TNG: Synergy Between Scientific and Technological INAF Members

    Science.gov (United States)

    Smareglia, R.; Bignamini, A.; Knapic, C.; Molinaro, M.; GAPS Collaboration

    2014-05-01

    GAPS (Global Architecture of Planetary Systems) is an Italian project devoted to understanding the architectural properties of planetary systems in connection with the characteristics of their host stars, taking advantage of the surgical (minus 1 m/s) radial velocity precision provided by HARPS-N@TNG. This project is the result of a concerted collaborative effort of a large fraction of the Italian astronomical community working in the exoplanetary field. This team has joined forces and its long-term expertise in high resolution spectroscopy, stellar rotation and activity, crowded stellar environments, formation of planetary systems, planetary dynamics, and data handling, with the aim to achieve the overarching goals of the program.

  20. The Gaia-ESO Survey: double-, triple-, and quadruple-line spectroscopic binary candidates

    Science.gov (United States)

    Merle, T.; Van Eck, S.; Jorissen, A.; Van der Swaelmen, M.; Masseron, T.; Zwitter, T.; Hatzidimitriou, D.; Klutsch, A.; Pourbaix, D.; Blomme, R.; Worley, C. C.; Sacco, G.; Lewis, J.; Abia, C.; Traven, G.; Sordo, R.; Bragaglia, A.; Smiljanic, R.; Pancino, E.; Damiani, F.; Hourihane, A.; Gilmore, G.; Randich, S.; Koposov, S.; Casey, A.; Morbidelli, L.; Franciosini, E.; Magrini, L.; Jofre, P.; Costado, M. T.; Jeffries, R. D.; Bergemann, M.; Lanzafame, A. C.; Bayo, A.; Carraro, G.; Flaccomio, E.; Monaco, L.; Zaggia, S.

    2017-12-01

    efficient discovery of many new multiple systems. With the detection of the SB1 candidates that will be the subject of a forthcoming paper, the study of the statistical and physical properties of the spectroscopic multiple systems will soon be possible for the entire GES sample. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council.

  1. Meteorological observatory for Antarctic data collection; L`Osservatorio per l`acquisizione dei dati meteorologici in Antartide

    Energy Technology Data Exchange (ETDEWEB)

    Grigioni, P.; De silvestri, L. [ENEA, Centro Ricerche Casaccia, Rome (Italy). Dip. Ambiente; Della Vedova, A.M. [Istituto Nazionale di Geofisica, P.N.R.A., Rome (Italy)

    1996-12-31

    In the last years, a great number of automatic weather stations was installed in Antarctica, with the aim to examine closely the weather and climate of this region and to improve the coverage of measuring points on the Antarctic surface. In 1987 the Italian Antarctic Project started to set up a meteorological network, in an area not completely covered by other countries. Some of the activities performed by the meteorological observatory, concerning technical functions such as maintenance of the AWS`s and the execution of radio soundings, or relating to scientific purposes such as validation and elaboration of collected data, are exposed. Finally, some climatological considerations on the thermal behaviour of the Antarctic troposphere such as `coreless winter`, and on the wind field, including katabatic flows in North Victoria Land are described.

  2. I grandi eventi: un osservatorio privilegiato sulla ricon?gurazione degli spazi. Il caso di Zaragoza 2008

    Directory of Open Access Journals (Sweden)

    Eleonora Mastropietro

    2012-02-01

    The core of the research presented in this paper concerns the analysis of the policies, the strategies and practices promoted by the city of Zaragoza for the Expo 2008 and their consequences in reshaping and reorganizing the city after the conclusion of the event.

  3. Incentivi ai farmaci generici a livello di ASL: l’osservatorio I.H.A.G.O.

    Directory of Open Access Journals (Sweden)

    Silvia Martina

    2002-06-01

    Full Text Available Generic drugs are pharmaceutical products that contain an active substance whose patent-covered period expired and are marketed with the name of the molecule. The public health authorities of most EU countries agree on the importance of generic drugs in rationalising the pharmaceutical market, particularly by favouring reasonable pricing of “mature” products. In contrast with this wide consensus, the market share of generic drugs remains quite poor in Italy, despite recent regulatory incentives for the promotion of their use. The longlasting lack of specific laws - reference-price politics were introduced only in 2001- and the unusually long patent-covered period fixed by the past legislation are among the main reasons for the scarce utilisation of generics in Italy. The awareness of the importance of promoting initiatives conducted on a local (ASL, and not only national (SSN scale conducted to the I.H.A.G.O. project, an observatory on the diffusion of generics in several local health districts. The project analyses the impact, in terms of market share, of local promoting activities (investigated by means of questionnaires conducted during the year 2001 in 11 ASLs (local health districts, deliberately selected among the most active in terms of promotion of the use of generics. The I.H.A.G.O. observation revealed several praiseworthy promotional efforts, particularly of informative and cultural kind, conducted by some of the considered ASLs. Unfortunately, these measures seem not to have had a practical impact on the generics market in the observed districts: the market share increase was superior to the one observed on national scale only in 4 of the considered ASLs, in other 4 it was similar, and in the remaining 3 it resulted even inferior. It appears useful to plan further measures to support the diffusion of generics, maybe by motivating health operators to their prescription with the introduction of “prize/punishment” mechanisms.

  4. Mandolesi, Reno (INAF IASF Bologna) give a talk about the Planck Mission at CERN. Photo taken in the CCC.

    CERN Multimedia

    Maximilien Brice

    2009-01-01

    The European Space Agency’s Planck satellite, launched the 14th of May 2009, is the next-generation space experiment in the field of Cosmic Microwave Background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity and angular resolution. Planck will provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the our Galaxy as well as external galaxies and clusters of galaxies. The ability of Planck to measure polarization across a wide frequency range (30-350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a larger package which describes the technical capabilities of the Planck sc...

  5. The Gaia-ESO Survey: Exploring the complex nature and origins of the Galactic bulge populations

    Science.gov (United States)

    Rojas-Arriagada, A.; Recio-Blanco, A.; de Laverny, P.; Mikolaitis, Š.; Matteucci, F.; Spitoni, E.; Schultheis, M.; Hayden, M.; Hill, V.; Zoccali, M.; Minniti, D.; Gonzalez, O. A.; Gilmore, G.; Randich, S.; Feltzing, S.; Alfaro, E. J.; Babusiaux, C.; Bensby, T.; Bragaglia, A.; Flaccomio, E.; Koposov, S. E.; Pancino, E.; Bayo, A.; Carraro, G.; Casey, A. R.; Costado, M. T.; Damiani, F.; Donati, P.; Franciosini, E.; Hourihane, A.; Jofré, P.; Lardo, C.; Lewis, J.; Lind, K.; Magrini, L.; Morbidelli, L.; Sacco, G. G.; Worley, C. C.; Zaggia, S.

    2017-05-01

    not participate in the X-shape bulge. Their Mg enhancement level and general shape in the [Mg/Fe] vs. [Fe/H] plane is comparable to that of the thick disk sequence. The position at which [Mg/Fe] starts to decrease with [Fe/H], called the "knee", is observed in the metal-poor bulge at [Fe/H] knee = -0.37 ± 0.09, being 0.06 dex higher than that of the thick disk. Although this difference is inside the error bars, it suggest a higher star formation rate (SFR) for the bulge than for the thick disk. We estimate an upper limit for this difference of Δ [Fe/H] knee = 0.24 dex. Finally, we present a chemical evolution model that suitably fits the whole bulge sequence by assuming a fast (poor subpopulation might be the product of an early prompt dissipative collapse dominated by massive stars. Nevertheless, our results do not allow us to firmly rule out the possibility that these stars come from the secular evolution of the early thick disk. This is the first time that an analysis of the bulge MDF and α-abundances has been performed in a large area on the basis of a homogeneous, fully spectroscopic analysis of high-resolution, high S/N data. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council.

  6. The Lord of Rings & the Olmi-Comics: Two cases of non-traditional approach to astronomy

    Science.gov (United States)

    Romaniello, S.; Cavallotti, F.; Sandrelli, S.

    2005-12-01

    Besides its traditional activities, the Public Outreach & Education offi ce (POE) of INAF-Osservatorio Astronomico di Brera (Milan, Italy) is carrying out two experiments in informal education for children aged 10 to 13: "The Lord of Rings - the mysterious case of the stolen rings" and "The Olmi-comics". The former is an astronomical role-playing game. Pupils are requested to discover the burglars of the rings of Saturn by hunting for them in an area where they meet actors playing their parts at distances scaled to the ones of the Solar System. The latter is a writing/ drawing workshop. Pupils try to write stories or draw comics about science. While the two projects are rather different both in content and in format, they have a common goal: making pupils live science, mainly astronomy, both with the mind and the body.

  7. Diagnosing syncope in clinical practice. Implementation of a simplified diagnostic algorithm in a multicentre prospective trial - the OESIL 2 study (Osservatorio Epidemiologico della Sincope nel Lazio)

    Science.gov (United States)

    Ammirati, F; Colivicchi, F; Santini, M

    2000-06-01

    In some patients with syncope health care is inappropriate and ineffective. In a recent observational investigation in community hospitals of the Lazio region of Italy (the OESIL study) 54.4% of patients admitted with syncope from the emergency room were discharged without a conclusive diagnosis. A simplified two-step diagnostic algorithm was developed and prospectively implemented in nine community hospitals of the Lazio region of Italy in order to improve the diagnostic performance of clinicians, thereby reducing the number of undiagnosed patients. The study population included 195 consecutive patients (85 males and 110 females, mean age 62.5 years, range 13-95 years) presenting with a syncopal spell at the emergency room of one of the nine participating hospitals in a 2-month period. The systematic implementation of the proposed diagnostic algorithm resulted in a striking reduction of undiagnosed cases. The percentage of patients discharged without a conclusive diagnosis decreased from 54.4% to 17.5%. Neurally mediated syncope was diagnosed in 35.2% of cases, cardiac syncope in 20.9% and neurological syncope in 13.8%. The use of specific, simplified diagnostic guidelines and algorithms results in an improvement of overall clinical performance. However, the development of such decision-making aids should carefully consider the local circumstances of daily clinical practice. Copyright 2000 The European Society of Cardiology.

  8. PRISMA, Italian network for meteors and atmospheric studies

    Science.gov (United States)

    Gardiol, D.; Cellino, A.; Di Martino, M.

    2016-01-01

    The aim of the PRISMA project is to develop the Italian participation in a network of European observing facilities whose primary targets are bright meteors (the so-called bolides and fireballs) and the recovery of meteorites. Several all-sky cameras have been recently installed in France (FRIPON project), and we propose to do the same in Italy, interconnecting the Italian network with the French one. Such a network is of great interest for the studies of interplanetary bodies and the dynamical and physical evolution of the population of small bodies of the Solar System and for the studies of collected meteorites. Those eventually recovered will be classified and investigated from the petrologic, genetic and evolutionary points of view, analyzed for their spectral characteristics and compared with known asteroids. The possibility to measure the radioactivity of samples shortly after the fall using gamma-ray spectrometers available in the Osservatorio Astrofisico di Torino laboratories, will allow us to reveal the presence of short-lived cosmogenic radioisotopes. PRISMA is also very suitable for the purposes of atmospheric studies. This includes the statistics of cloud coverage and lightning frequencies, as well as the comparison of the optical depth measured using satellites and PRISMA cameras.

  9. Astronomia e fisica a Firenze dalla Specola ad Arcetri

    CERN Document Server

    Bianchi, Simone; Casalbuoni, Roberto; Dominici, Daniele; Mazzoni, Massimo; Pelosi, Giuseppe

    2017-01-01

    La Mostra "Astronomia e Fisica a Firenze" illustra l'evoluzione delle due discipline dal XVIII secolo fino ai primi decenni del Novecento. Teatro cittadino di questo processo, anzi di tutte le scienze, fu l'Imperiale e Reale Museo di Fisica e Storia Naturale, dove adesso ha sede la Mostra. Nell'arco di tempo esaminato tutti gli aspetti dell'indagine della natura erano ugualmente pertinenti ad un'unica figura di studioso, ma verso l'inizio del XX secolo alcuni indirizzi subirono una profonda trasformazione e al prevalente approccio tassonomico e fenomenologico subentrò, soprattutto per Astronomia e Fisica, un'indagine specialistica che finì per differenziare le varie ricerche. Protagonista di questa fase fu lo sviluppo dell'analisi spettroscopica. La Mostra, aperta da dicembre 2016 a marzo 2017, è organizzata dall'Università di Firenze (Museo di Storia Naturale; Dipartimento di Fisica e Astronomia) e dall'Osservatorio Astrofisico di Arcetri, in collaborazione con la Sezione di Firenze dell'INFN, il Museo G...

  10. Sharpest views of Betelgeuse reveal how supergiant stars lose mass-Unveiling the true face of a behemoth

    Science.gov (United States)

    2009-07-01

    supergiant star itself. Their unrivalled observations have led the astronomers to propose that these large-scale gas motions roiling under Betelgeuse's red surface are behind the ejection of the massive plume into space. Notes 1] If Betelgeuse were at the centre of our Solar System it would extend out almost to the orbit of Jupiter, engulfing Mercury, Venus, Earth, Mars and the main asteroid belt. More information This research was presented in two papers to appear in Astronomy and Astrophysics: The close circumstellar environment of Betelgeuse: Adaptive optics spectro-imaging in the near-IR with VLT/NACO, by Pierre Kervella et al., and Spatially resolving the inhomogeneous structure of the dynamical atmosphere of Betelgeuse with VLTI/AMBER, by Keiichi Ohnaka et al. The teams are composed of P. Kervella, G. Perrin, S. Lacour, and X. Haubois (LESIA, Observatoire de Paris, France), T. Verhoelst (K. U. Leuven, Belgium), S. T. Ridgway (National Optical Astronomy Observatories, USA), and J. Cami (University of Western Ontario, Canada), and of K. Ohnaka, K.-H. Hofmann, T. Driebe, F. Millour, D. Schertl, and G. Weigelt (Max-Planck-Institute for Radio Astronomy, Bonn, Germany), M. Benisty (INAF-Osservatorio Astrofisico di Arcetri, Firenze, Italy), A. Chelli (LAOG, Grenoble, France), R. Petrov and F. Vakili (Lab. H. Fizeau, OCA, Nice, France), and Ph. Stee (Lab. H. Fizeau, OCA, Grasse, France). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and

  11. Adding New Colours to Interferometry

    Science.gov (United States)

    2004-04-01

    Another vital step has been accomplished as planned towards full operation of the ESO Very Large Telescope Interferometer (VLTI) at the Paranal Observatory in Chile, one of the world's foremost astronomical facilities. In the night of March 20-21, 2004, a team of astronomers and engineers from France, Italy, Germany and ESO celebrated the successful assembly and completion of the first on-line tests of the latest of the first-generation VLTI instruments, the Astronomical Multiple BEam Recombiner (AMBER). They combined the two beams of light from the southern star Theta Centauri from two test telescopes ("siderostats" with 40-cm aperture, cf. ESO PR 06/01) to produce strong and clear interferometric fringes. Equally successful observations were then obtained on the bright star Sirius, and consistently repeated during the following nights. A joint project This is the most promising result of about 7 years of dedicated work by a team of over 40 astronomers and engineers. The AMBER instrument has been developed by a European consortium of seven research institutes in three ESO member countries, the main partners being: Laboratoire d'Astrophysique de Grenoble (LAOG), Laboratoire Universitaire d'Astrophysique de Nice (LUAN) and Observatoire de la Côte d'Azur in France, Max-Planck-Institut für Radioastronomie (MPIfR) in Bonn, Germany, and Osservatorio Astrofisico di Arcetri (OAA; part of INAF, the Italian National Institute for Astrophysics) in Florence, Italy. The total cost of AMBER is of the order of 5.9 million Euros, mostly contributed by the members of the consortium. It was built through an agreement with ESO, which rewards the consortium solely with guaranteed observing time. According to the contract, the consortium will receive 60 observing nights to be spread among two or three of the four 8.2-m VLT Unit Telescopes and 130 nights with the four Auxiliary Telescopes over a period of eight years. AMBER: soon to join three light beams at once ESO PR Photo 09a/04

  12. The Sky Through Three Giant Eyes

    Science.gov (United States)

    2007-02-01

    precise and careful study of the wind and the shockwave coming from the nova. The stream of results from the VLTI and AMBER is no doubt going to increase in the coming years with the availability of new functionalities. "In addition to the 8.2-m Unit Telescopes, the VLTI can also combine the light from up to 4 movable 1.8-m Auxiliary Telescopes. AMBER fed by three of these AT's will be offered to the user community as of April this year, and from October we will also make FINITO available," said Melnick. "This 'fringe-tracking' device allows us to stabilise changes in the atmospheric conditions and thus to substantially improve the efficiency of the observations. By effectively 'freezing' the interferometric fringes, FINITO allows astronomers to significantly increase the exposure times." The Astronomy & Astrophysics special feature (volume 464 - March II 2007) on AMBER first results includes 11 articles. They are freely available on the A&A web site. More Information The AMBER consortium, led by Romain Petrov (Nice, France), includes researchers from the Laboratoire d'Astrophysique de Grenoble (France), Laboratoire d'Astrophysique Universitaire de Nice (France), Max-Planck Institut für Radioastronomie (Bonn, Germany), INAF-Osservatorio Astrofisico di Arcetri (Italy), and the Observatoire de la Côte d'Azur (Nice, France). In March 2004, the first on-line tests of AMBER (Astronomical Multiple BEam Recombiner) were completed, when astronomers combined the two beams of light from the southern star Theta Centauri from two test 40-cm aperture telescopes (ESO 07/04). It was later used to combine light from two, then three Unit Telescopes of ESO's VLT and light from the Auxiliary Telescopes. AMBER is part of the VLT Interferometer (VLTI) and completes the planned set of first-generation instruments for this facility. It continues the success story of the interferometric mode of the VLT, following the unique initial scientific results obtained by the VINCI and MIDI instruments

  13. DUSTER: collection of meteoric CaO and carbon smoke particles in the upper stratosphere .

    Science.gov (United States)

    Della Corte, V.; Rietmeijer, F. J. M.; Rotundi, A.; Ferrari, M.; Palumbo, P.

    Nanometer- to micrometer-size particles present in the upper stratosphere are a mixture of terrestrial and extra-terrestrial origins. They can be extraterrestrial particles condensed after meteor ablation. Meteoric dust in bolides is occasionally deposited into the lower stratosphere around 20 km altitude. Nanometer CaO and pure carbon smoke particles were collected at 38 km altitude in the upper stratosphere in the Arctic during June 2008 using DUSTER (Dust in the Upper Stratosphere Tracking Experiment and Retrieval), a balloon-borne instrument for the non-destructive collection of solid particles between 200 nm to 40 microns. We report the collection of micron sized CaCO_3 (calcite) grains. Their morphologies show evidence of melting and condensation after vaporization suggest at temperatures of approximately 3500 K. The formation environment of the collected grains was probably a dense dust cloud formed by the disintegration of a carbonaceous meteoroid during deceleration in the Earth� atmosphere. For the first time, DUSTER collected meteor ablation products that were presumably associated with the disintegration of a bolide crossing the Earth's atmosphere. The collected mostly CaO and pure carbon nanoparticles from the debris cloud of a fireball, included: 1) intact fragments; 2) quenched melted grains; and 3) vapor phase condensation products. The DUSTER project was funded by the Italian Space Agency (ASI), PRIN2008/MIUR (Ministero dell'Istruzione dell'Universitá e della Ricerca), PNRA 2013(Piano Nazionale Ricerca Antartide). CNES graciously provided this flight opportunity. We thank E. Zona and S. Inarta at the Laboratorio di Fisica Cosmica INAF, Osservatorio Astronomico di Capodimonte-Universitá di Napoli Parthenope. F.J.M.R. was supported by grant NNX07AI39G from the NASA Cosmochemistry Program. We thank three anonymous reviewers who assisted us in introducing our new instrument.

  14. X-ray mirror prototype based on cold shaping of thin glass foils

    Science.gov (United States)

    Basso, Stefano; Civitani, Marta; Ghigo, Mauro; Hołyszko, Joanna; Pareschi, Giovanni; Salmaso, Bianca; Vecchi, Gabriele; Burwitz, Vadim; Pelliciari, Carlo; Hartner, Gisela D.; Breunig, Elias

    2017-08-01

    The Slumping Glass Optics technology for the fabrication of astronomical X-ray mirrors has been developed in recent years in USA and Europe. The process has been used for making the mirrors of the Nustar, mission. The process starts with very thin glass foils hot formed to copy the profile of replication moulds. At INAF - Osservatorio Astronomico di Brera a process based on cold shaping is being developed, based on an integration method involving the use of interconnecting ribs for making stacks. Each glass foil in the stack is shaped onto a very precise integration mould and the correct shape is frozen by means of glued ribs that act as spacers between one layer and the next one (the first layers being attached to a thick substrate). Therefore, the increasing availability of flexible glass foils with a thickness of a few tens of microns (driven by electronic market for ultra-thin displays) opens new possibilities for the fabrication of X-ray mirrors. This solution appears interesting especially for the fabrication of mirrors for hard X-rays (with energy > 10 keV) based on multilayer coatings, taking advantage from the intrinsic low roughness of the glass foils that should grant a low scattering level. The stress frozen on the glass due to the cold shaping is not negligible, but it is kept into account in the errors of the X-ray optics design. As an exercise, we have considered the requirements and specs of the FORCE hard Xray mission concept (being studied by JAXA) and we have designed the mirror modules assuming the cold slumping as a fabrication method. In the meantime, a prototype (representative of the FORCE mirror modules) is being design and integrated in order to demonstrate the feasibility and the capacity to reach good angular resolution.

  15. The Lord of Rings - the mysterious case of the stolen rings: a critical analysis

    Science.gov (United States)

    Sandrelli, S.

    The Lord of Rings - the mysterious case of the stolen rings: a critical analysis S. Sandrelli INAF - Osservatorio Astronomico di Brera, Milano, Italy (stefano.sandrelli@brera.inaf.it / Fax: 02 72001600 / Phone: +39 02 72320337) "The Lord of Rings - the mysterious case of the stolen rings" is a live astronomical role-playing game for kids aged 10 -13. Its goal is to introduce them to some of the main topics of the Solar System: a) the role of gravity; b) the distribution of mass & light; c) the effects of rotation; d) the distribution of water. The game was held both at the Perugia (2004) and the Genova Science Festival (2005), obtaining great success. Teams of about 6-8 members are introduced to Mr Schioppanelli, the astro-detective of the town (the name is a pun: it reminds Schiaparelli, the famous italian astronomer, and it is a slang expression meaning "ring-breaker"). Mr Schioppanelli has his office in an "gastronomical astronomical observatory", known as The Red Giant Pizzeria. Schioppanelli informs the kids that a mysterious Centaur succeded in stealing the rings of Saturn. The partecipants are appointed astro-detectives in-charge and asked to find the rings by browsing around the Solar System, which is scaled so as to fit the town historical centre or a pedestrian area, going from the Sun to Saturn or beyond, depending on the actual area at disposal. Great care must be taken allowing children playing only in a car-free area of the town. At the right scaled distances, the partecipants meet characters playing as the various planets. The kids can talk to them after solving a riddle, obtaining useful informations. A special characters play as a comet, timely going in and out of the inner solar system. The teams can also talk to some shepherd-moons of the rings. They easily discover that the rings were totally destroyed by the Centaur: a real disaster! They are also suggested to gather the necessary ingredients (gravity, light, rotation, inclination, dust and

  16. The Most Distant Mature Galaxy Cluster - Young, but surprisingly grown-up

    Science.gov (United States)

    2011-03-01

    information This research was presented in a paper, "A mature cluster with X-ray emission at z = 2.07", by R. Gobat et al., published in the journal Astronomy & Astrophysics. The team is composed of R. Gobat (Laboratoire AIM-Paris-Saclay, France), E. Daddi (AIM-Paris), M. Onodera (ETH Zürich, Switzerland), A. Finoguenov (Max-Planck-Institut für extraterrestrische Physik [MPE], Garching, Germany), A. Renzini (INAF-Osservatorio Astronomico di Padova), N. Arimoto (National Astronomical Observatory of Japan), R. Bouwens (Lick Observatory, Santa Cruz, USA), M. Brusa (MPE), R.-R. Chary (California Institute of Technology, USA), A. Cimatti (Università di Bologna, Italy), M. Dickinson (NOAO, Tucson, USA), X. Kong (University of Science and Technology of China), and M.Mignoli (INAF - Osservatorio Astronomico di Bologna, Italy). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 15 countries: Austria, Belgium, Brazil, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world's most advanced visible-light astronomical observatory and VISTA, the world's largest survey telescope. ESO is the European partner of a revolutionary astronomical telescope ALMA, the largest astronomical project in existence. ESO is currently planning a 42-metre European Extremely Large optical/near-infrared Telescope, the E-ELT, which will become "the

  17. The Connection between Radio Halos and Cluster Mergers and the ...

    Indian Academy of Sciences (India)

    1Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127, Bologna, Italy. 2IRA-INAF, via Gobetti 101, 40129 Bologna, Italy. ∗ e-mail: rcassano@ira.inaf. .... Chandra archive X-ray data of a sub-sample of GMRT clusters provided a quantita- tive measure of the degree of the cluster disturbance adopting three ...

  18. "europe Towards the Stars"

    Science.gov (United States)

    1995-06-01

    . 0030-1-941-1181, Fax 0030-1-941-7372 Ireland: Dr I. Elliot, Dunsink Observatory (Dublin Institute for Advanced Studies), Castleknock, Dublin 15, Tel. 00353-1- 838-7911/7959, Fax 00353-1-8387090, E-mail ie@dunsink.dias.ie Italy: Prof. F. Pacini, Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Tel. 0039-55-2752246, Fax 0039-55-220039, E-mail pacini@arcetri.astro.it Luxemburg: Dr. F. Wagner, Laboratoire de Physique, Lycee de Garcons d'Esch, BP 195, L-4002 Esch/Alzette, Tel. 00352-556285, Fax 00352-570994 The Netherlands: Dr. H. Lamers, Rijksuniversiteit Utrecht, Princetonplein 5, Postbus 80.000, NL-3508 TA Utrecht, Tel. 0031-30-535200, Fax 0031-30531601, email hennyl@sron.ruu.nl Portugal: Dr. T. Lago, Centro de Astrofisico, Universidade do Porto, Rua do Campo Alegre 823, P-4150 Porto, Tel. 00351-2-6007081, Fax 00351-2-6007982, E-mail mtlago@ncc.up.pt Spain: Dr. Asuncion Sanchez/Dr Telmo Fernandez, Planetario de Madrid, Parque Tierno Galvan, E-28045 Madrid, Tel. 0034-1-4673578, Fax 0034-1-4681154, E-mail tfc@vilspa.esa.es Sweden: Dr. Kerstin Loden, Stockholms Observatorium, S-133 36 Saltsjoebaden, Tel. 0046-8-164454, Fax 0046-8-7174719, e-mail lodenk@astro.su.se Switzerland: Mr. M. Wieland, Schweizer Jugend Forscht/La Science Appelle les Jeunes, Technoramastrasse 1, CH-8404 Winterthur, Tel. 0041-52-2424440, Fax 0041-52-2422967 United Kingdom: Dr A. M. Cohen, Dane Valley High School, Jackson Road, Congleton, Cheshire CW12 1NT, England, United Kingdom, Tel. +44-260-273000, Fax +44-260-297352 (until July 1, 1995). The National Committee for the United Kingdom, c/o The Association for Astronomy Education, 9 Hurst Lane, Bollington, Macclesfield, Cheshire SK10 5LN, England (after July 1, 1995). [1] See ESO Press Releases 08/93 of 5 November 1993 and 17/94 of 2 December 1994. ESO Press Information is made available on the World-Wide Web (URL: http://www.hq.eso.org/) and on CompuServe (space science and astronomy area, GO SPACE).

  19. a Passage to the Universe

    Science.gov (United States)

    1995-11-01

    Brussel, Campus Ofenplein, Pleinlaan 2, B-1050 Brussels, Tel. 0032-2-6293469, Fax 0032-9-3623976, E-mail csterken@is1.vub.ac.be Denmark: Mr. B. F. Joergensen, Tycho Brahe Planetariet, Gl. Kongevej 10, DK-1610 Copenhagen V, Tel. 0045-33-144888, Fax 0045-33-142888, E-mail tycho@inet.uni-c.dk Finland: Mr. M. Hotakainen, Taehtitieteellinen Yhdistys Ursa, Laivanvarustajankatu 9C 54, FIN-00140 Helsinki, Tel. 00358-0-174048, Fax 00358-0-657728 France: Mr. B. Pellequer, Geospace d'Aniane, Boite Postale 22, F-34150 Aniane, Tel. 0033-6-7034949, Fax 0033-6-7752864 Germany: Dr. K.-H. Lotze, Friedrich-Schiller-Universitaet, Max-Wien-Platz 1, D-07743 Jena, Germany, Tel. +49-3641-635904/636654, Fax +49-3641-636728 Greece: Dr. D. Simopoulos, Eugenides Foundation, Astronomy Department, 387 Sygrou Avenue, Palaio Faliro, GR-175 64 Athens, Tel. 0030-1-941-1181, Fax 0030-1-941-7372 Ireland: Dr. I. Elliot, Dunsink Observatory (Dublin Institute for Advanced Studies), Castleknock, Dublin 15, Tel. 00353-1- 838-7911/7959, Fax 00353-1-8387090, E-mail ie@dunsink.dias.ie Italy: Dr. B. Monsignori Fossi, Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Tel. 0039-55-2752246, Fax 0039-55-220039, E-mail bmonsignori@arcetri.astro.it The Netherlands: Dr. M. Drummen, Stichting `De Koepel', Zonnenburg 2, NL-3512 NL Utrecht, Tel. 0031-30-311360, Fax 0031-30-342852, E-mail dekoepel@knoware.nl Spain: Dr. A. Sanchez/Dr. T. Fernandez, Planetario de Madrid, Parque Tierno Galvan, E-28045 Madrid, Tel. 0034-1-4673578, Fax 0034-1-4681154, E-mail tfc@vilspa.esa.es Sweden: Dr. K. Loden, Stockholms Observatorium, S-133 36 Saltsjoebaden, Tel. 0046-8-164454, Fax 0046-8-7174719, E-mail lodenk@astro.su.se United Kingdom: Dr. A. M. Cohen, c/o The Association for Astronomy Education, 9 Hurst Lane, Bollington, Macclesfield, Cheshire SK10 5LN, England Notes: [1] See ESO Press Releases 08/93 of 5 November 1993 and 17/94

  20. Galactic Building Blocks Seen Swarming Around Andromeda

    Science.gov (United States)

    2004-02-01

    Green Bank, WV - A team of astronomers using the National Science Foundation's Robert C. Byrd Green Bank Telescope (GBT) has made the first conclusive detection of what appear to be the leftover building blocks of galaxy formation -- neutral hydrogen clouds -- swarming around the Andromeda Galaxy, the nearest large spiral galaxy to the Milky Way. This discovery may help scientists understand the structure and evolution of the Milky Way and all spiral galaxies. It also may help explain why certain young stars in mature galaxies are surprisingly bereft of the heavy elements that their contemporaries contain. Andromeda Galaxy This image depicts several long-sought galactic "building blocks" in orbit of the Andromeda Galaxy (M31). The newfound hydrogen clouds are depicted in a shade of orange (GBT), while gas that comprises the massive hydrogen disk of Andromeda is shown at high-resolution in blue (Westerbork Sythesis Radio Telescope). CREDIT: NRAO/AUI/NSF, WSRT (Click on Image for Larger Version) "Giant galaxies, like Andromeda and our own Milky Way, are thought to form through repeated mergers with smaller galaxies and through the accretion of vast numbers of even lower mass 'clouds' -- dark objects that lack stars and even are too small to call galaxies," said David A. Thilker of the Johns Hopkins University in Baltimore, Maryland. "Theoretical studies predict that this process of galactic growth continues today, but astronomers have been unable to detect the expected low mass 'building blocks' falling into nearby galaxies, until now." Thilker's research is published in the Astrophysical Journal Letters. Other contributors include: Robert Braun of the Netherlands Foundation for Research in Astronomy; Rene A.M. Walterbos of New Mexico State University; Edvige Corbelli of the Osservatorio Astrofisico di Arcetri in Italy; Felix J. Lockman and Ronald Maddalena of the National Radio Astronomy Observatory (NRAO) in Green Bank, West Virginia; and Edward Murphy of the

  1. Optical Counterparts of Undetermined Type -Ray Active Galactic ...

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... ... David Salvetti2 Marco Berton1 Valentina Cracco1 Fermi-LAT collaboration. Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, Vicolo dell'Osservatorio 3, 35122 Padova, Italy. IASF Milano – Istituto di Astrofisica Spaziale e Fisica Cosmica, Via E. Bassini 15, 20133 Milano, Italy.

  2. High Energy Phenomena in Eta Carinae Roberto F. Viotti , Lucio ...

    Indian Academy of Sciences (India)

    R. Narasimhan (Krishtel eMaging) 1461 1996 Oct 15 13:05:22

    e-mail: uvspace@ias.rm.cnr.it. 2Osservatorio Astronomico di Roma, 00040 Monte Porzio, Italy. 3ASI Science Data Centre, ESA-ESRIN, 00044 Frascati, Italy. 4Dipartimento di Fisica, Universit`a La Sapienza, 00185 Roma, Italy. .... In this regard, we recall that the most recent CHANDRA observations have also suggested that ...

  3. L'universo senza fine breve storia del Tutto : passato e futuro del cosmo

    CERN Document Server

    Regge, Tullio

    1999-01-01

    Che aspetto avrà l'universo tra miliardi di anni? E quale sarà il destino del pianeta terra? Un bilancio scientifico delle scoperte cosmologiche più avanzate e straordinarie, tracciato dal più celebre astrofisico italiano. Regge fa piazza pulita di teorie millenariste, come quella di un futuro collasso dell'universo e spiega perché questo è destinato invece a espandersi progressivamente. Nella forma di un saggio accessibile al grande pubblico, Regge propone un'esplorazione rigorosa e affascinante sul futuro dell'universo e degli esseri viventi che lo abitano.

  4. A decline and fall in the future of Italian Astronomy?

    OpenAIRE

    Antonelli, Angelo; Antonuccio-Delogu, Vincenzo; Baruffolo, Andrea; Benetti, Stefano; Bianchi, Simone; Biviano, Andrea; Bonafede, Annalisa; Bondi, Marco; Borgani, Stefano; Bragaglia, Angela; Brescia, Massimo; Brucato, John Robert; Brunetti, Gianfranco; Brunino, Riccardo; Cantiello, Michele

    2010-01-01

    On May 27th 2010, the Italian astronomical community learned with concern that the National Institute for Astrophysics (INAF) was going to be suppressed, and that its employees were going to be transferred to the National Research Council (CNR). It was not clear if this applied to all employees (i.e. also to researchers hired on short-term contracts), and how this was going to happen in practice. In this letter, we give a brief historical overview of INAF and present a short chronicle of the ...

  5. Giant Galaxy Messier 87 finally sized up

    Science.gov (United States)

    2009-05-01

    population in general. As they are relatively short-lived (a few tens of thousands of years -- a mere blip on astronomical timescales), astronomers can estimate that one star in about 8000 million of Sun-like stars is visible as a planetary nebula at any given moment. Thus planetary nebulae can provide a unique handle on the number, types of stars and their motions in faint outer galaxy regions that may harbour a substantial amount of mass. These motions contain the fossil record of the history of galaxy interaction and the formation of the galaxy cluster. This research is presented in a paper to appear in Astronomy and Astrophysics: "The Edge of the M87 Halo and the Kinematics of the Diffuse Light in the Virgo Cluster Core," by Michelle Doherty et al. The team is composed of Michelle Doherty and Magda Arnaboldi (ESO), Payel Das and Ortwin Gerhard (Max-Planck-Institute for Extraterrestrial Physics, Garching, Germany), J. Alfonso L. Aguerri (IAC, Tenerife, Spain), Robin Ciardullo (Pennsylvania State University, USA), John J. Feldmeier (Youngstown State University, USA), Kenneth C. Freeman (Mount Stromlo Observatory, Australia), George H. Jacoby (WIYN Observatory, Tucson, AZ, USA), and Giuseppe Murante (INAF, Osservatorio Astronomico di Pino Torinese, Italy). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in the Atacama Desert region of Chile: La Silla, Paranal and Chajnantor.

  6. Exoplanets Clue to Sun's Curious Chemistry

    Science.gov (United States)

    2009-11-01

    . "Like our Sun, these stars have been very efficient at destroying the lithium they inherited at birth," says team member Nuno Santos. "Using our unique, large sample, we can also prove that the reason for this lithium reduction is not related to any other property of the star, such as its age." Unlike most other elements lighter than iron, the light nuclei of lithium, beryllium and boron are not produced in significant amounts in stars. Instead, it is thought that lithium, composed of just three protons and four neutrons, was mainly produced just after the Big Bang, 13.7 billion years ago. Most stars will thus have the same amount of lithium, unless this element has been destroyed inside the star. This result also provides the astronomers with a new, cost-effective way to search for planetary systems: by checking the amount of lithium present in a star astronomers can decide which stars are worthy of further significant observing efforts. Now that a link between the presence of planets and curiously low levels of lithium has been established, the physical mechanism behind it has to be investigated. "There are several ways in which a planet can disturb the internal motions of matter in its host star, thereby rearrange the distribution of the various chemical elements and possibly cause the destruction of lithium. It is now up to the theoreticians to figure out which one is the most likely to happen," concludes Mayor. More information This research was presented in a paper that appears in the 12 November 2009 issue of Nature (Enhanced lithium depletion in Sun-like stars with orbiting planets, by G. Israelian et al.). The team is composed of Garik Israelian, Elisa Delgado Mena, Carolina Domínguez Cerdeña, and Rafael Rebolo (Instituto de Astrofisíca de Canarias, La Laguna, Tenerife, Spain), Nuno Santos and Sergio Sousa (Centro de Astrofisica, Universidade de Porto, Portugal), Michel Mayor and Stéphane Udry (Observatoire de Genève, Switzerland), and Sofia Randich (INAF

  7. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester M13 9PL, United Kingdom. INAF - Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy. Institute for Studies in Theoretical Physics and Mathematics, Tehran, Iran.

  8. Journal of Astrophysics and Astronomy | Indian Academy of Sciences

    Indian Academy of Sciences (India)

    2016-01-27

    Jan 27, 2016 ... Moscow Engineering Physics Institute, Kashirskoe Shosse 31, 115409 Moscow, Russia. Astronomical Institute, Czech Academy of Sciences, Fricova 298, 251 65 Ondrejov, Czech Republic. INAF/Observatorio Astronomico di Palermo and University of Palermo, Palazzo dei Normanni, I-90134 Palermo, Italy.

  9. Exploration of Professional Social Networks and Opinions about Scholarly Communication Tools among Italian Astrophysicists

    OpenAIRE

    M. Marra

    2015-01-01

    The poster conveys the first results of a survey conducted among astrophysicists working at INAF. Just under 120 respondents made it possible to investigate their behaviour and opinions with regard to use of some major professional social networks and preferences about some aspects of scholarly communication and evaluation.

  10. The GAMMA Ray Sky as Seen by Fermi: Opening a New Window on the High Energy Space Environment

    Science.gov (United States)

    2009-01-01

    de Physique des Particules (IN2P3) in France; the Agenzia Spaziale Italiana (ASI), the Instituto Nazionale di Fisica Nucle- are (INFN), and the...Instituto Nazionale di Astrofisicia (INAF) in Italy; the Ministry of Education , Culture, Sports, Science and Technology (MEXT), the High Energy

  11. Template for letter of approval by Research Supervisor

    International Development Research Centre (IDRC) Digital Library (Canada)

    Liliane Castets-Poupart

    a) As research supervisor of J. Smith, I confirm that I approve and support the research proposal submitted by the candidate. b) J. Smith has successfully completed the following course(s):. STAT 890: Statistics, Survey Design and Analysis INAF 540: International Affairs Dynamics. ECON 700: Qualitative Research Data.

  12. Template for letter of approval by Research Supervisor

    International Development Research Centre (IDRC) Digital Library (Canada)

    Liliane Castets-Poupart

    a) As research supervisor of Mr. John Smith, I confirm that I approve and support the research proposal submitted by the candidate. b) Mr. Smith has successfully completed the following course(s):. STAT 890: Statistics, Survey Design and Analysis. INAF 540: International Affairs Dynamics. ECON 700: Qualitative Research ...

  13. INTEGRAL/JEM-X detection of 1RXS J194211.9+255552

    DEFF Research Database (Denmark)

    Chenevez, Jérôme; Fiocchi, M.; Bazzano, A.

    2011-01-01

    The INTEGRAL satellite has resumed Galactic Plane Scanning observations (PI: A. Bazzano) since November 27^th , 2011. Results are made publicly available at: http://gpsiasf.iasf-roma.inaf.it/ The transient ROSAT source 1RXS J194211.9+255552 is detected by INTEGRAL/JEM-X during the Galactic Plane ...

  14. Climate Change and Future World

    Science.gov (United States)

    2013-03-01

    2013. 4 Centro Studi di Politica Internazionale, Cambiamenti Climatici e Governance della Sicurezza: la Rilevanza Politica della Nuova Agenda...Internazionale, (Osservatorio di Politica Internazionale, n. 16 – maggio 2010), 1. (Center for the Studies of International Politics, Climate Change and...CMMDiscussionPaper1ClimateChangeAdaptationa ndConflict.pdf), accessed 3/06/2013. 38 Ibid. 39 Ibid, 10. 40 Centro Studi di Politica Internazionale, Cambiamenti Climatici e

  15. Lo sport nelle scienze sociali: da chimera a realtà

    Directory of Open Access Journals (Sweden)

    Marco Pasini

    2013-04-01

    Full Text Available Lo sport per la sua trama profonda, le implicazioni che cristallizza, le emozioni che condensa, è fonte di interpretazione e osservatorio straordinariamente ricco per la ricerca sociale. L'obiettivo di questo numero della rivista, grazie ai contributi qualificati, trasversali, multidisciplinari ed empirici, è proprio quello di affrontare le questioni fondamentali sopra indicate attraverso differenti percorsi di senso e approcci teorico-metodologici specifici.

  16. On Solar Granulations, Limb Darkening, and Sunspots: Brief Insights in Remembrance of Father Angelo Secchi

    OpenAIRE

    Robitaille P.-M.

    2011-01-01

    Father Angelo Secchi used the existence of solar granulation as a central line of rea- soning when he advanced that the Sun was a gaseous body with a photosphere contain- ing incandescent particulate matter (Secchi A. Sulla Struttura della Fotosfera Solare. Bullettino Meteorologico dell’Osservatorio del Collegio Romano , 30 November 1864, v.3(11), 1–3). Secchi saw the granules as condensed matter emitting the photospheric spectrum, while the darkened intergranular lanes conv...

  17. Spatial and temporal distribution of vertical ground movements at Mt. Vesuvius in the period 1973-2009

    Directory of Open Access Journals (Sweden)

    Folco Pingue

    2013-11-01

    Full Text Available Since the early ’70s vertical ground movements at Mount Vesuvius area have been investigated and monitored by the Osservatorio Vesuviano (Isti-tuto Nazionale di Geofisica Vulcanologia - Osservatorio Vesuviano since 2001. This monitoring began with the installation of a high-precision leveling line in the region at medium-high elevations on the volcano. The deformation pattern and expected strain field assessment methods in the volcanic structure induced by inner sources has demanded in subsequent years the expansion of the leveling network up to cover the whole volcanic area, enclosing part of leveling lines of other institutions. As a result of this expansion, the Mt. Vesuvius Area Leveling Network (VALN has today reached a length of about 270 km and consists of 359 benchmarks. It is configured in 21 circuits and is connected, westward, to the Campi Flegrei leveling network and, northward, to the Campania Plain leveling network. The data collected have been carefully re-analyzed for random and systematic errors and for error propagation along the leveling lines to identify the areas affected by significant ground movements. For each survey, the data were rigorously adjusted and vertical ground movements were evaluated by differentiating the heights calculated by the various measurements conducted by the Osservatorio Vesuviano from 1973 to 2009.

  18. Most Efficient Spectrograph to Shoot the Southern Skies

    Science.gov (United States)

    2009-05-01

    CNRS; in Italy the Osservatorio di Brera, Trieste, Palermo and Catania; and in the Netherlands, the University of Amsterdam, the University of Nijmegen and ASTRON. Beside the participating institutes and ESO, the project was supported by the National Agencies of Italy (INAF), the Italian Ministry for Education, University and Research (MIUR), the Netherlands (NOVA and NWO) and by the Carlsberg Foundation in Denmark. The project was also supported in Denmark and the Netherlands with funds from the EU Descartes prize, the highest European prize for science, awarded in 2002 to the European collaboration on gamma-ray burst research headed by Professor Ed van den Heuvel. ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in the Atacama Desert region of Chile: La Silla, Paranal and Chajnantor.

  19. Cosmic "Dig" Reveals Vestiges of the Milky Way's Building Blocks

    Science.gov (United States)

    2009-11-01

    means of a computer-controlled deformable mirror that counteracts the image distortion introduced by atmospheric turbulence. It is based on real-time optical corrections computed at very high speed (many hundreds of times each second) from image data obtained by a wavefront sensor (a special camera) that monitors light from a reference star, Present AO systems can only correct the effect of atmospheric turbulence in a very small region of the sky - typically 15 arcseconds or less - the correction degrading very quickly when moving away from the reference star. Engineers have therefore developed new techniques to overcome this limitation, one of which is multi-conjugate adaptive optics. MAD uses up to three guide stars instead of one as references to remove the blur caused by atmospheric turbulence over a field of view thirty times larger than existing techniques (eso0719). More information This research was presented in a paper that appears in the 26 November 2009 issue of Nature , "The cluster Terzan 5 as a remnant of a primordial building block of the Galactic bulge", by F. R. Ferraro et al.. The team is composed of Francesco Ferraro, Emanuele Dalessandro, Alessio Mucciarelli and Barbara Lanzoni (Department of Astronomy, University of Bologna, Italy), Giacomo Beccari (ESA, Space Science Department, Noordwijk, Netherlands), Mike Rich (Department of Physics and Astronomy, UCLA, Los Angeles, USA), Livia Origlia, Michele Bellazzini and Gabriele Cocozza (INAF - Osservatorio Astronomico di Bologna, Italy), Robert T. Rood (Astronomy Department, University of Virginia, Charlottesville, USA), Elena Valenti (ESO and Pontificia Universidad Catolica de Chile, Departamento de Astronomia, Santiago, Chile) and Scott Ransom (National Radio Astronomy Observatory, Charlottesville, USA). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 14 countries

  20. Fisica del Plasma Fondamenti e applicazioni astrofisiche

    CERN Document Server

    Chiuderi, Claudio

    2012-01-01

    L'opera si propone di introdurre i principi fondamentali della Fisica del Plasma, disciplina che trova applicazione sia nel campo del'energetica (Fusione Termonucleare Controllata), sia dell'Astrofisica (oltre il 90% della materia dell'Universo è sotto forma di plasma). Dopo un capitolo introduttivo, vengono discussi i possibili schemi di descrizione teorica dei plasmi. La parte centrale è dedicata alla discussione della magnetoidrodinamica, con particolare riguardo alla teoria delle onde e delle instabilità. Vengono infine trattati i problemi della riconnessione magnetica e delle onde d'urto nei plasmi. Per ogni argomento trattato vengono illustrate delle applicazioni di carattere astrofisico. I calcoli vengono sempre svolti esplicitamente in modo da permettere allo studente una piena comprensione delle relative tecniche. Una serie di esercizi permette inoltre la verifica delle competenze acquisite. Il libro è destinato agli studenti dei corsi di Laurea Magistrale e di Dottorato .

  1. I sei numeri dell'universo le forze profonde che spiegano il cosmo

    CERN Document Server

    Rees, Martin

    2002-01-01

    È possibile che sei semplici numeri, sei costanti universali, diano conto dell'infinita varietà e della stupefacente complessità del cosmo? L'astrofisico Martin Rees ci mostra che non soltano ciò è possibile, ma in quei sei numeri sono scritti la storia, la struttura e il futuro dell'universo, e che perfino la comparsa della vita sulla terra, e dunque la nostra stessa esistenza, non sarebbe concepibile se uno solo di quei valori numerici, definiti nell'istante che segnò la nascita del mondo, fosse differente. I sei numeri dell'universo ci introducono così ad alcune delle questioni più profonde su cui si interroga oggi la scienza.

  2. Medicina-Noto VLBI observation of SN2013ej

    Science.gov (United States)

    Sokolovsky, K.; Giroletti, M.; Stagni, M.; Nanni, M.; Mahabal, A.

    2013-08-01

    We used the 32m radio telescopes of Istituto di Radioastronomia (INAF-IRA) in Medicina and Noto as a two-element very long baseline interferometer to search for a possible radio counterpart of SN2013ej, a type IIP supernova (CBET #3606, ATel #5228, #5229, #5230, #5237, #5243) in M74. The observations were conducted at 6.7 GHz on 2013 July 31.3 UT, 6 days after the first optical detection reported in CBET #3609.

  3. Os efeitos do alfabetismo funcional sobre a empregabilidade dos trabalhadores brasileiros

    Directory of Open Access Journals (Sweden)

    Cristiano Machado Costa

    2014-06-01

    Full Text Available Este trabalho utiliza a pesquisa Indicador de Alfabetismo Funcional (Inaf, realizada entre 2001 e 2007, para investigar os efeitos do alfabetismo funcional sobre a empregabilidade dos trabalhadores brasileiros, ressaltando as diferenças entre sexos e setores econômicos. Utilizando modelos probit e controlando para características observáveis dos indivíduos, os resultados apontam para uma maior importância das habilidades funcionais entre as mulheres. O efeito do aumento em um desvio-padrão na nota do Inaf resulta em crescimento de 6,10 p.p. na probabilidade de a mulher estar empregada. O indicador não se mostra significativo com relação à empregabilidade dos homens brasileiros, exceto no setor comercial, em que o aumento de um desvio-padrão no score Inaf eleva a probabilidade de um indivíduo estar empregado em 4 p.p. O setor comercial caracteriza-se pela maior interação entre os profissionais e os clientes, demandando habilidades funcionais que, muitas vezes, não são capturadas por meio das estatísticas usuais de escolaridade (nível e/ou anos de estudo.

  4. The many facets of extragalactic radio surveys: towards new scientific challenges

    Science.gov (United States)

    2015-10-01

    Radio continuum surveys are a powerful tool to detect large number of objects over a wide range of redshifts and obtain information on the intensity, polarization and distribution properties of radio sources across the sky. They are essential to answer to fundamental questions of modern astrophysics. Radio astronomy is in the midst of a transformation. Developments in high-speed digital signal processing and broad-band optical fibre links between antennas have enabled significant upgrades of the existing radio facilities (e-MERLIN, JVLA, ATCA-CABB, eEVN, APERTIF), and are leading to next-generation radio telescopes (LOFAR, MWA, ASKAP, MeerKAT). All these efforts will ultimately lead to the realization of the Square Kilometre Array (SKA), which, owing to advances in sensitivity, field-of-view, frequency range and spectral resolution, will yield transformational science in many astrophysical research fields. The purpose of this meeting is to explore new scientific perspectives offered by modern radio surveys, focusing on synergies allowed by multi-frequency, multi-resolution observations. We will bring together researchers working on wide aspects of the physics and evolution of extra-galactic radio sources, from star-forming galaxies to AGNs and clusters of galaxies, including their role as cosmological probes. The organization of this conference has been inspired by the recent celebration of the 50th anniversary of the Northern Cross Radio Telescope in Medicina (BO), whose pioneering B2 and B3 surveys provided a significant contribution to radio astronomical studies for many decades afterwards. The conference was organized by the Istituto di Radioastronomia (INAF), and was held at the CNR Research Area in Bologna, on 20-23 October 2015. This Conference has received support from the following bodies and funding agencies: National Institute for Astrophysics (INAF), ASTRON, RadioNet3 (through the European Union’s Seventh Framework Programme for research

  5. Pulsating Star Mystery Solved

    Science.gov (United States)

    2010-11-01

    ] The name OGLE-LMC-CEP0227 arises because the star was first discovered to be a variable during the OGLE search for gravitational microlensing. More details about OGLE are available at: http://ogle.astrouw.edu.pl/. More information This research was presented in a paper to appear in the journal Nature on 25 November 2010. The team is composed of G. Pietrzyński (Universidad de Concepción, Chile, Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Poland), I. B. Thompson (Carnegie Observatories, USA), W. Gieren (Universidad de Concepción, Chile), D. Graczyk (Universidad de Concepción, Chile), G. Bono (INAF-Osservatorio Astronomico di Roma, Universita' di Roma, Italy), A. Udalski (Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Poland), I. Soszyński (Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Poland), D. Minniti (Pontificia Universidad Católica de Chile) and B. Pilecki (Universidad de Concepción, Chile, Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Poland). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world's most advanced visible-light astronomical observatory and VISTA, the world's largest survey telescope. ESO is the European partner of a revolutionary astronomical telescope ALMA, the

  6. UDI STOP Femminicidio

    Directory of Open Access Journals (Sweden)

    Giovanna Crivelli

    2014-04-01

    Full Text Available L'UDI, Unione Donne in Italia, ha collaborato con l'Osservatorio dei Processi Comunicativi a un numero monografico della rivista scientifica M@gm@ dal titolo "Violenza maschile e femminicidio". Il numero monografico vuole mettere a disposizione le analisi, l’esperienza e la storia nostra e delle nostre interlocutrici, come contributo al nostro comune lavoro di sensibilizzazione, contrasto alla violenza maschile sulle donne – femminicidio. “UDI STOP femminicidio” è da anni la nostra campagna contro la violenza di genere, la collaborazione con l’Osservatorio dei Processi Comunicativi è parte integrante di questo sforzo. Il primo e dichiarato dei nostri progetti politici è il contrasto alla cultura e al potere ideologico che consente il femminicidio, la subordinazione culturale e sociale, la percezione della donna come oggetto di dominio, la riduzione in schiavitù di tante donne, comprese molte donne prostitute... Sappiamo di non voler tradire una “responsabilità di genere” che deve necessariamente concretizzarsi in tanti “gesti responsabili”, nella lunga pazienza quotidiana che consente la sedimentazione di un cambiamento radicale nelle coscienze. Vogliamo continuare ad essere l’associazione che coniuga insieme la soggettività personale e l'assunzione diretta di responsabilità, della progettualità a lungo termine che non trova “contraddittorio” misurarsi con la solidarietà concreta e quotidiana con le altre donne, nel tentativo di far nascere le nuove maniere di pensare.

  7. Time Trends of High Blood Pressure Prevalence, Awareness and Control in the Italian General Population : Surveys of the National Institute of Health.

    Science.gov (United States)

    Di Lonardo, Anna; Donfrancesco, Chiara; Palmieri, Luigi; Vanuzzo, Diego; Giampaoli, Simona

    2017-06-01

    High blood pressure (BP) is a major risk factor for cardiovascular disease. The urgency of the problem was underlined by the World Health Organization (WHO) Global Action Plan for the prevention and control of noncommunicable diseases, which recommends a 25% relative reduction in the prevalence of raised BP by 2020. A surveillance system represents a useful tool to monitor BP in the general population. Since 1980s, the National Institute of Health has conducted several surveys of the adult general population, measuring cardiovascular risk factors by standardized procedures and methods. To describe mean BP levels and high BP prevalence from 1978 to 2012 by sex and quinquennia of age. Data were derived from the following three studies: (i) Risk Factors and Life Expectancy (RIFLE), conducted between 1978 and 2002 in 13 Italian regions (>70,000 persons); (ii) Osservatorio Epidemiologico Cardiovascolare (OEC), conducted between 1998-2002 in the general population from all Italian regions (>9000 persons); and (iii) Osservatorio Epidemiologico Cardiovascolare/Health Examination Survey (OEC/HES), conducted between 2008-2012 in the general population from all Italian regions (>9000 persons). A significant decrease in mean systolic and diastolic BP levels and prevalence of high BP from 1978 to 2012 was observed both in men and women. BP and high BP increased by age classes in all considered periods. BP awareness and control also improved. Our data suggest that BP control could be achieved by 2020, as recommended by WHO.

  8. Ionic channel mechanisms mediating the intrinsic excitability of Kenyon cells in the mushroom body of the cricket brain.

    Science.gov (United States)

    Inoue, Shigeki; Murata, Kaoru; Tanaka, Aiko; Kakuta, Eri; Tanemura, Saori; Hatakeyama, Shiori; Nakamura, Atsunao; Yamamoto, Chihiro; Hasebe, Masaharu; Kosakai, Kumiko; Yoshino, Masami

    2014-09-01

    Intrinsic neurons within the mushroom body of the insect brain, called Kenyon cells, play an important role in olfactory associative learning. In this study, we examined the ionic mechanisms mediating the intrinsic excitability of Kenyon cells in the cricket Gryllus bimaculatus. A perforated whole-cell clamp study using β-escin indicated the existence of several inward and outward currents. Three types of inward currents (INaf, INaP, and ICa) were identified. The transient sodium current (INaf) activated at -40 mV, peaked at -26 mV, and half-inactivated at -46.7 mV. The persistent sodium current (INaP) activated at -51 mV, peaked at -23 mV, and half-inactivated at -30.7 mV. Tetrodotoxin (TTX; 1 μM) completely blocked both INaf and INaP, but 10nM TTX blocked INaf more potently than INaP. Cd(2+) (50 μM) potently blocked INaP with little effect on INaf. Riluzole (>20 μM) nonselectively blocked both INaP and INaf. The voltage-dependent calcium current (ICa) activated at -30 mV, peaked at -11.3 mV, and half-inactivated at -34 mV. The Ca(2+) channel blocker verapamil (100 μM) blocked ICa in a use-dependent manner. Cell-attached patch-clamp recordings showed the presence of a large-conductance Ca(2+)-activated K(+) (BK) channel, and the activity of this channel was decreased by removing the extracellular Ca(2+) or adding verapamil or nifedipine, and increased by adding the Ca(2+) agonist Bay K8644, indicating that Ca(2+) entry via the L-type Ca(2+) channel regulates BK channel activity. Under the current-clamp condition, membrane depolarization generated membrane oscillations in the presence of 10nM TTX or 100 μM riluzole in the bath solution. These membrane oscillations disappeared with 1 μM TTX, 50 μM Cd(2+), replacement of external Na(+) with choline, and blockage of Na(+)-activated K(+) current (IKNa) with 50 μM quinidine, indicating that membrane oscillations are primarily mediated by INaP in cooperation with IKNa. The plateau potentials observed either in

  9. LOW LITERACY AND NEW DIGITAL MEDIA: THE EXPERIENCE OF LOW-LITERACY INDIVIDUALS IN SOCIAL MEDIA AND INSTANT MESSENGERS

    OpenAIRE

    LORENNA SILVA EUNAPIO DA CONCEIÇÃO

    2016-01-01

    Dados do Ibope e do Indicador de Analfabetismo Funcional (Inaf) de 2012 revelam que, no Brasil, existem aproximadamente 14 milhões de analfabetos absolutos e um pouco mais de 35 milhões de analfabetos funcionais. Segundo estatísticas, o Brasil é o terceiro país do mundo em tempo gasto na internet, sendo mais da metade em mídias sociais. Nesse contexto, as atividades diárias se direcionam a comunicações baseadas em texto, e a falta de capacidade de leitura e escrita torna-se ...

  10. The Tenth International Workshop on MULTIFREQUENCY BEHAVIOUR OF HIGH ENERGY COSMIC SOURCES Palermo, Italy, 2013

    Directory of Open Access Journals (Sweden)

    Editorial, Foreword

    2014-12-01

    Full Text Available Organizing Institutions:Istituto di Astrofisica e Planetologia Spaziali IAPS-INAF, Roma, ItalyDpt de Cargas Utiles y Ciencias del Espacio, DCUCE-INTA Madrid, SpainE.O. Hulburt Center for Space Research, HCA-NRL, Washington D.C., USAMax-Planck Institut fr Extraterrestrische Physik, MPE, Garching, GermanySt. John’s College, SJC, Annapolis MD, USAInstitute für Astronomie und Astrophysik, Karls Eberhard, Universität SAND 1, Tübingen, GermanyASCR - Astronomical Institute, Ondřejov, Czech RepublicCTU - Czech Technical University, Prague, Czech Republic

  11. Young and Waltzing Binary Stars

    Science.gov (United States)

    2001-10-01

    stars heat up enough to start nuclear burning. When infant stars in RXJ 0529.4+0041 eventually reach middle-age, their sizes will most likely also be quite similar to that of the Sun. The significance of RXJ 0529.4+0041 Few systems are known for which such precise determinations of the stellar parameters have ever been possible - and this binary system represents the first case where both the components are such young stars . A detailed comparison of the derived stellar parameters with current models for the evolution of young stars shows fairly good agreement for the primary component. However, there are certain discrepancies in the case of the secondary component, showing that the current models for the early stages of lower-mass stars must still be refined. More information Part of the results described in this press release are described in more detail in a scientific article ( "RXJ 0529.4+0041: a low-mass pre-main sequence eclipsing-spectroscopic binary" by E. Covino et al.) that has been published in the European research journal Astronomy & Astrophysics (Vol. 361, p. 49). Notes [1] The team consists of Elvira Covino (Principal Investigator), Juan M. Alcalá , Rosita Paladino (all Osservatorio Astronomico di Capodimonte, Napoli, Italy), Antonio Frasca , Santo Catalano , Ettore Marilli (all Osservatorio Astrofisico di Catania, Italy) and Michael Sterzik (ESO-Chile). [2] One solar mass corresponds to 1.99 10 30 kg, or about 330,000 times the mass of the Earth. The Sun is about 4500 million years old and its total lifetime is of the order of 12-13,000 million years. It is an interesting thought that if the Sun would have been somewhat heavier, its total lifetime might have been too short for living organisms to develop on the Earth. In fact, the biological evolution that ultimately lead to the emergence of human beings apparently lasted about 4 billion years; this corresponds to the total lifetime of a star that is only about 20 % heavier than the Sun. Note also the

  12. Buchi neri nel mio bagno di schiuma l’enigma di Einstein

    CERN Document Server

    Vishveshwara, C V

    2008-01-01

    "Le bolle stavano turbinando tutto intorno a me e massaggiavano il mio corpo ... Mentre me la godevo in questo fantastico bagno di bolle, i miei occhi si fecero pesanti e mi lasciaii trasportare in un dormiveglia sublimamente estatico". Così inizia l’incontro di Alfie con una vasca da bagno eccezionale e rivelatrice, acquistata da un vicino misterioso di nome Al. L’Enigma di Einstein, ovvero buchi neri nel mio bagno di schiuma, racconta la storia della teoria della gravitazione, dai suoi primordi fino agli ultimi sviluppi in astrofisica, focalizzandosi sulla teoria della relatività generale di Albert Einstein e sulla fisica dei buchi neri. Tramite conversazioni avvincenti e diagrammi scarabocchiati su tovaglioli di carta, si susseguono a ruota i rudimenti della relatività, dello spazio-tempo e di molti aspetti della fisica moderna. In scenette narrate con abilità pedagogica e notevole talento letterario, il lettore s’imbatterà nelle lezioni informali che un astrofisico cosmopolita tiene al suo amic...

  13. OAJ 2.6m survey telescope: optical alignment and on-sky evaluation of IQ performances

    Science.gov (United States)

    Lousberg, Gregory P.; Bastin, Christian; Moreau, Vincent; Pirnay, Olivier; Flebus, Carlo; Chueca, Sergio; Iñiguez, César; Ederoclite, Alessandro; Ramió, Héctor V.; Cenarro, A. Javier

    2016-08-01

    AMOS has recently completed the alignment campaign of the 2.6m telescope for the Observatorio Astrofisico de Javalambre (OAJ). AMOS developed an innovative alignment technique for wide field-of-view telescopes that has been successfully implemented on the OAJ 2.6m telescope with the active support of the team of CEFCA (Centro de Estudios de Física del Cosmos de Aragón). The alignment relies on two fundamental techniques: (1) the wavefront-curvature sensing (WCS) for the evaluation of the telescope aberrations at arbitrary locations in the focal plane, and (2) the comafree point method for the adjustment of the position of the secondary mirror (M2) and of the focal plane (FP). The alignment campaign unfolds in three steps: (a) analysis of the repeatability of the WCS measurements, (b) assessment of the sensitivity of telescope wavefront error to M2 and FP position adjustments, and (c) optical alignment of the telescope. At the end of the campaign, seeing-limited performances are demonstrated in the complete focal plane. With the help of CEFCA team, the image quality of the telescope are investigated with a lucky-imaging method. Image sizes of less than 0.3 arcsec FWHM are obtained, and this excellent image quality is observed over the complete focal plane.

  14. The High-Level Interface Definitions in the ASTRI/CTA Mini Array Software System (MASS)

    Science.gov (United States)

    Conforti, V.; Tosti, G.; Schwarz, J.; Bruno, P.; Cefal‘A, M.; Paola, A. D.; Gianotti, F.; Grillo, A.; Russo, F.; Tanci, C.; Testa, V.; Antonelli, L. A.; Canestrari, R.; Catalano, O.; Fiorini, M.; Gallozzi, S.; Giro, E.; Palombara, N. L.; Leto, G.; Maccarone, M. C.; Pareschi, G.; Stringhetti, L.; Trifoglio, M.; Vercellone, S.; Astri Collaboration; Cta Consortium

    2015-09-01

    ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana) is a Flagship Project funded by the Italian Ministry of Education, University and Research, and led by INAF, the Italian National Institute of Astrophysics. Within this framework, INAF is currently developing an end-to-end prototype, named ASTRI SST-2M, of a Small Size Dual-Mirror Telescope for the Cherenkov Telescope Array, CTA. A second goal of the project is the realization of the ASTRI/CTA mini-array, which will be composed of seven SST-2M telescopes placed at the CTA Southern Site. The ASTRI Mini Array Software System (MASS) is designed to support the ASTRI/CTA mini-array operations. MASS is being built on top of the ALMA Common Software (ACS) framework, which provides support for the implementation of distributed data acquisition and control systems, and functionality for log and alarm management, message driven communication and hardware devices management. The first version of the MASS system, which will comply with the CTA requirements and guidelines, will be tested on the ASTRI SST-2M prototype. In this contribution we present the interface definitions of the MASS high level components in charge of the ASTRI SST-2M observation scheduling, telescope control and monitoring, and data taking. Particular emphasis is given to their potential reuse for the ASTRI/CTA mini-array.

  15. The ICT monitoring system of the ASTRI SST-2M prototype proposed for the Cherenkov Telescope Array

    Science.gov (United States)

    Gianotti, F.; Bruno, P.; Tacchini, A.; Conforti, V.; Fioretti, V.; Tanci, C.; Grillo, A.; Leto, G.; Malaguti, G.; Trifoglio, M.

    2016-08-01

    In the framework of the international Cherenkov Telescope Array (CTA) observatory, the Italian National Institute for Astrophysics (INAF) has developed a dual mirror, small sized, telescope prototype (ASTRI SST-2M), installed in Italy at the INAF observing station located at Serra La Nave, Mt. Etna. The ASTRI SST-2M prototype is the basis of the ASTRI telescopes that will form the mini-array proposed to be installed at the CTA southern site during its preproduction phase. This contribution presents the solutions implemented to realize the monitoring system for the Information and Communication Technology (ICT) infrastructure of the ASTRI SST-2M prototype. The ASTRI ICT monitoring system has been implemented by integrating traditional tools used in computer centers, with specific custom tools which interface via Open Platform Communication Unified Architecture (OPC UA) to the Alma Common Software (ACS) that is used to operate the ASTRI SST-2M prototype. The traditional monitoring tools are based on Simple Network Management Protocol (SNMP) and commercial solutions and features embedded in the devices themselves. They generate alerts by email and SMS. The specific custom tools convert the SNMP protocol into the OPC UA protocol and implement an OPC UA server. The server interacts with an OPC UA client implemented in an ACS component that, through the ACS Notification Channel, sends monitor data and alerts to the central console of the ASTRI SST-2M prototype. The same approach has been proposed also for the monitoring of the CTA onsite ICT infrastructures.

  16. The Solar Tower at Monte Mario: a New Didactic Laboratory for Astronomy

    Science.gov (United States)

    D'Alessio, F.; Faccini, M.; Leoni, R.; Giobbi, G.

    The year 2009 witnessed the restoration of the Solar Tower of Astronomical Observatory of Rome, in the INAF main office of Villa Mellini, Monte Mario. This structure underwent a patient restructuring of optics, mechanics and control equipment. Moreover, some areas have been converted into welcome centre for the visitors, so as to transform a scientific instrument - which was active up to a few years ago - into a didactic structure, mainly suitable for school groups. The Solar Tower of Monte Mario, which has been open to the public since January 2010, allows visitors to directly observe the Sun, as well as the spectrum of its light. The Tower therefore becomes an effective didactic instrument in order to teach and talk about a wide range of scientific topics - from Solar Physics to Sun-Earth interactions, to Stellar Evolution. Here we describe the work done by the DivA group of INAF-OAR for putting back into service the Solar Tower, from the technical and didactic viewpoints. We shall also take stock of the activities organized in the first few months of activity.

  17. All Sky Camera, LIDAR and Electric Field Meter: Auxiliary instruments for the ASTRI SST-2M prototype

    Directory of Open Access Journals (Sweden)

    Leto Giuseppe

    2015-01-01

    Full Text Available ASTRI SST-2M is the end-to-end prototype telescope of the Italian National Institute of Astrophysics, INAF, designed to investigate the 10–100 TeV band in the framework of the Cherenkov Telescope Array, CTA. The ASTRI SST-2M telescope has been installed in Italy in September 2014, at the INAF observing station located at Serra La Nave on Mount Etna. The telescope is foreseen to be completed and fully operative in spring 2015 including auxiliary instrumentation needed to support both operations and data analysis. In this contribution we present the current status of a sub-set of the auxiliary instruments that are being used at the Serra La Nave site, namely an All Sky Camera, an Electric Field Meter and a Raman Lidar devoted, together with further instrumentation, to the monitoring of the atmospheric and environmental conditions. The data analysis techniques under development for these instruments could be applied at the CTA sites, where similar auxiliary instrumentation will be installed.

  18. Global positioning system survey data for active seismic and volcanic areas of eastern Sicily, 1994 to 2013.

    Science.gov (United States)

    Bonforte, Alessandro; Fagone, Sonia; Giardina, Carmelo; Genovese, Simone; Aiesi, Gianpiero; Calvagna, Francesco; Cantarero, Massimo; Consoli, Orazio; Consoli, Salvatore; Guglielmino, Francesco; Puglisi, Biagio; Puglisi, Giuseppe; Saraceno, Benedetto

    2016-08-01

    This work presents and describes a 20-year long database of GPS data collected by geodetic surveys over the seismically and volcanically active eastern Sicily, for a total of more than 6300 measurements. Raw data were initially collected from the various archives at the Istituto Nazionale di Geofisica e Vulcanologia, Sezione di Catania-Osservatorio Etneo and organized in a single repository. Here, quality and completeness checks were performed, while all necessary supplementary information were searched, collected, validated and organized together with the relevant data. Once all data and information collections were completed, raw binary data were converted into the universal ASCII RINEX format; all data are provided in this format with the necessary information for precise processing. In order to make the data archive readily consultable, we developed software allowing the user to easily search and obtain the needed data by simple alphanumeric and geographic queries.

  19. Multiscreening and Social TV: The Changing Landscape of TV Consumption in Italy

    Directory of Open Access Journals (Sweden)

    Alberto Marinelli

    2014-12-01

    Full Text Available The explosive growth of handheld screen devices has fostered the emergence of new TV consumption practices: "always connected while watching TV" is the expression that best summarizes this transformation.  On the one hand we observe multiscreening practices engendered by the availability of second screen devices, which people use both simultaneously and sequentially while watching. On the other hand  these handeld device are strengthening the social dimension of the TV-watching experience (Social TV. This paper aims to analyze the diffusion of social and connected television in the Italian market,  relying on data from the “Osservatorio Social TV 2013-2014” (Sapienza University, Rome.

  20. Global positioning system survey data for active seismic and volcanic areas of eastern Sicily, 1994 to 2013

    Science.gov (United States)

    Bonforte, Alessandro; Fagone, Sonia; Giardina, Carmelo; Genovese, Simone; Aiesi, Gianpiero; Calvagna, Francesco; Cantarero, Massimo; Consoli, Orazio; Consoli, Salvatore; Guglielmino, Francesco; Puglisi, Biagio; Puglisi, Giuseppe; Saraceno, Benedetto

    2016-08-01

    This work presents and describes a 20-year long database of GPS data collected by geodetic surveys over the seismically and volcanically active eastern Sicily, for a total of more than 6300 measurements. Raw data were initially collected from the various archives at the Istituto Nazionale di Geofisica e Vulcanologia, Sezione di Catania—Osservatorio Etneo and organized in a single repository. Here, quality and completeness checks were performed, while all necessary supplementary information were searched, collected, validated and organized together with the relevant data. Once all data and information collections were completed, raw binary data were converted into the universal ASCII RINEX format; all data are provided in this format with the necessary information for precise processing. In order to make the data archive readily consultable, we developed software allowing the user to easily search and obtain the needed data by simple alphanumeric and geographic queries.

  1. Research and Project Activities in Astrophysics

    Science.gov (United States)

    Harnden, F. Rick, Jr.

    2002-02-01

    In collaboration with G Micela, S. Sciortino, and others at the Osservatorio Astronomico di Palermo G. S. Valens, we conducted studies of X-ray emission from normal stars, primarily via observations of several open star clusters and star forming regions (viz. the Pleiades, NBC 2516, NBC 2264, and the Orion Nebula Cluster). Our work was based on combined data from several X-ray observatories, Einstein, ROSAT, XMM-Newton and Chandra, as well as ground-based optical and radio data. Preliminary results were presented at several meetings: HEAD/AAS, November, 1997 a 195th AAS Meeting, January 2000 a Three Islands Conference, April 2000 a X-ray Astronomy 2000, September 2000 a 197th AAS Meeting, January 2001 Two Years of Science with Chandra, September 2001

  2. A Tale of Two Populations

    Science.gov (United States)

    2005-03-01

    FLAMES instrument on the Very Large Telescope at Paranal. They used the MEDUSA mode, allowing to obtain no less than 130 spectra simultaneously. Twelve one-hour spectra were obtained for 17 stars of the blue population and the same number stars from the red one. These stars have magnitudes between 20 and 21, i.e., they are between 500,000 and 1 million times fainter than what can be seen with the unaided eye. The individual spectra of stars from each population were then co-added. This produced a "mean" spectrum of a blue-population star and another of a red-population. Each of these spectra represents a total of no less than 204 hours of exposure time and accordingly provides information in unrivalled detail about these stars, especially in terms of their chemical composition. The scientific outcome matches the technical achievement! From a careful study of the combined spectra, the astronomers were able to establish that - contrary to all prior expectations - the bluer stars are more "metal-rich" (by a factor two) than the redder ones. "The latter were found to have an abundance of elements more massive than helium corresponding to about 1/40 the solar abundance [2] ", explains Raffaele Gratton of INAF-Osservatorio Astronomico di Padova in Italy. "This is indeed very puzzling as current models of stars predict that the more metal-rich a star is, the redder it ought to be". Giampaolo Piotto (University of Padova, Italy), leader of the team, thinks that there is a solution to this celestial puzzle: "The only way we can explain this discrepancy is by assuming that the two populations of stars have a different abundance of helium. We find that while the red stars have a normal helium abundance, the bluer stars must be enriched in helium by more than 50% with respect to the other population!" These stars are thus the most helium-rich stars ever found, and not by just a few percent! It took some 8 billion years for the Milky Way Galaxy to increase its helium abundance from

  3. Software use cases to elicit the software requirements analysis within the ASTRI project

    Science.gov (United States)

    Conforti, Vito; Antolini, Elisa; Bonnoli, Giacomo; Bruno, Pietro; Bulgarelli, Andrea; Capalbi, Milvia; Fioretti, Valentina; Fugazza, Dino; Gardiol, Daniele; Grillo, Alessandro; Leto, Giuseppe; Lombardi, Saverio; Lucarelli, Fabrizio; Maccarone, Maria Concetta; Malaguti, Giuseppe; Pareschi, Giovanni; Russo, Federico; Sangiorgi, Pierluca; Schwarz, Joseph; Scuderi, Salvatore; Tanci, Claudio; Tosti, Gino; Trifoglio, Massimo; Vercellone, Stefano; Zanmar Sanchez, Ricardo

    2016-07-01

    The Italian National Institute for Astrophysics (INAF) is leading the Astrofisica con Specchi a Tecnologia Replicante Italiana (ASTRI) project whose main purpose is the realization of small size telescopes (SST) for the Cherenkov Telescope Array (CTA). The first goal of the ASTRI project has been the development and operation of an innovative end-to-end telescope prototype using a dual-mirror optical configuration (SST-2M) equipped with a camera based on silicon photo-multipliers and very fast read-out electronics. The ASTRI SST-2M prototype has been installed in Italy at the INAF "M.G. Fracastoro" Astronomical Station located at Serra La Nave, on Mount Etna, Sicily. This prototype will be used to test several mechanical, optical, control hardware and software solutions which will be used in the ASTRI mini-array, comprising nine telescopes proposed to be placed at the CTA southern site. The ASTRI mini-array is a collaborative and international effort led by INAF and carried out by Italy, Brazil and South-Africa. We present here the use cases, through UML (Unified Modeling Language) diagrams and text details, that describe the functional requirements of the software that will manage the ASTRI SST-2M prototype, and the lessons learned thanks to these activities. We intend to adopt the same approach for the Mini Array Software System that will manage the ASTRI miniarray operations. Use cases are of importance for the whole software life cycle; in particular they provide valuable support to the validation and verification activities. Following the iterative development approach, which breaks down the software development into smaller chunks, we have analysed the requirements, developed, and then tested the code in repeated cycles. The use case technique allowed us to formalize the problem through user stories that describe how the user procedurally interacts with the software system. Through the use cases we improved the communication among team members, fostered

  4. The upgrade of an educational observatory control system with a PLC-based architecture

    Science.gov (United States)

    Baldini, V.; Cirami, R.; Coretti, I.; Di Marcantonio, P.; Galeotta, S.; Iafrate, G.; Mannetta, M.; Santin, P.

    2014-07-01

    A Celestron C14 telescope equipped with a robotic Paramount ME equatorial mount is being used for public outreach at the Basovizza site of the INAF-Astronomical Observatory of Trieste. Although the telescope could be fully remotely controlled, the control of the instrumentations and the movement of the main motor of the dome requires the physical presence of an operator. To overcome this limitation the existing control system has been upgraded using a Beckhoff PLC to allow the remote control of the whole instrumentation, including the management of the newly installed weather sensor and the access to the telescope area. Exploiting the decentralization features typical of a PLC based solution, the PLC modules are placed in two different racks, according to the function to be controlled. A web interface is used for the communication between the user and the instrumentation. The architecture of this control system will be presented in detail in this paper.

  5. Developments of FPGA-based digital back-ends for low frequency antenna arrays at Medicina radio telescopes

    Science.gov (United States)

    Naldi, G.; Bartolini, M.; Mattana, A.; Pupillo, G.; Hickish, J.; Foster, G.; Bianchi, G.; Lingua, A.; Monari, J.; Montebugnoli, S.; Perini, F.; Rusticelli, S.; Schiaffino, M.; Virone, G.; Zarb Adami, K.

    In radio astronomy Field Programmable Gate Array (FPGA) technology is largely used for the implementation of digital signal processing techniques applied to antenna arrays. This is mainly due to the good trade-off among computing resources, power consumption and cost offered by FPGA chip compared to other technologies like ASIC, GPU and CPU. In the last years several digital backend systems based on such devices have been developed at the Medicina radio astronomical station (INAF-IRA, Bologna, Italy). Instruments like FX correlator, direct imager, beamformer, multi-beam system have been successfully designed and realized on CASPER (Collaboration for Astronomy Signal Processing and Electronics Research, https://casper.berkeley.edu) processing boards. In this paper we present the gained experience in this kind of applications.

  6. INTEGRAL detection of the multi-peaked emission from the Be/X-ray binary pulsar GRO J1008-57

    DEFF Research Database (Denmark)

    Fiocchi, M.; Sguera, A.; Chenevez, Jérôme

    2014-01-01

    /4 of the outbursts in Be/XRBs (e.g. Kretschmar et al., 2013, arXiv.1302.3434). We will continue to monitor the source activity with INTEGRAL through the GPS programme until December 20th. Light curves and images can be found on the GPS webpages: http://gpsiasf.iasf-roma.inaf.it/......Recent observations from the on-going INTEGRAL Galactic Plane Scanning programme (PI: A. Bazzano) have detected increasing X-ray flux from the Be/X-ray binary pulsar GRO J1008-57, confirming the re-brightening detected by MAXI/GSC (ATel #6819). The source was in the field of view of the IBIS...

  7. LITERATURA INFANTOJUVENIL, POLÍTICAS PÚBLICAS DE LEITURA E FORMAÇÃO DE LEITORES

    Directory of Open Access Journals (Sweden)

    Flávia Ferreira de Paula

    2014-01-01

    Full Text Available This paper aims to discuss the children and youth literature, Brazilian reading public policies and their relations with readers’ formation. Firstly, approaches, the concepts of reading, from the concepts of beginning literacy and literacy, and some data on reading in Brazil, based on INAF 2009 and PISA 2009. Reading at school environment and the role of children and youth literature in the formation of new readers are also subjects addressed here. Furthermore, raises information on public policies and programs which aim to encourage reading in Brazil in the last few years. Lastly, we go further on Programa Nacional Biblioteca da Escola [School Library National Program] (PNBE and some reviews on the program.

  8. Division XII / Commission 41 / Working Group Historical Instruments

    Science.gov (United States)

    Pigatto, Luisa; Il-Seong, Nha; Hamel, Jürgen; Johnson, Kevin; Kochhar, Rajesh K.; Nakamura, Tsuko; Orchiston, Wayne; Pettersen, Bjørn R.; Schechner, Sara J.; Yunli, Shi

    The Historical Instruments Working Group (WG-HI) and Commission 41 started planning an interdisciplinary conference titled Astronomy and its instruments before and after Galileo since January 2007. This conference, as an IYA2009 initiative, aims “to highlight mankind's path toward an improved knowledge of the sky using mathematical and mechanical tools as well as monuments and buildings, giving rise, in doing so, to scientific astronomy”. Commission 46 and Commission 55 also support this conference, to be held on the Isle of San Servolo, Venice (Italy), 27 September 3 October 2009. As a fact of history, it was in Venice that Galileo was advised and got material (glass) to make his telescope, and in Venice he presented an working instrument to Venetian Doge in August 1609. The conference is co-sponsored by IAU as a Joint Symposium with the INAF Astronomical Observatory of Padova, Italy.

  9. Celestial-themed Cartoons Captivate Children

    Science.gov (United States)

    Cappelli, V.; di Benedetto, C.

    2010-12-01

    Attivamente: Big discoveries with Galileo and Phineas & Ferb, an educational entertainment project for children, was a collaboration between Disney Television Italy and the Education and Public Outreach office of the INAF Astronomical Observatory of Padua, Italy. The project started during the International Year of Astronomy 2009 and came to an end in June 2010. It consisted of a cartoon series, several articles in a Disney magazine and an educational kit focused on Galileo Galilei and the Moon. The kit, called the First Astronomical Kit, was distributed to 30 000 children in Italy, and included a board game about the Moon, an observation diary and a lunar fact card. The aim of the kit was to give children some basic astronomical knowledge and to demonstrate the essential role that observation plays in understanding the heavens. This article discusses how a research institute and a major entertainment company -- each with very different working practices -- were able to work together to form a successful partnership.

  10. IXPE - The Imaging X-Ray Polarimetry Explorer

    Science.gov (United States)

    Ramsey, Brian

    2014-01-01

    The Imaging X-ray Polarimetry Explorer (IXPE) is a Small Explorer Mission that will be proposed in response to NASA's upcoming Announcement of Opportunity. IXPE will transform our understanding of the most energetic and exotic astrophysical objects, especially neutron stars and black holes, by measuring the linear polarization of astronomical objects as a function of energy, time and, where relevant, position. As the first dedicated polarimetry observatory IXPE will add a new dimension to the study of cosmic sources, enlarging the observational phase space and providing answers to fundamental questions. IXPE will feature x-ray optics fabricated at NASA/MSFC and gas pixel focal plane detectors provided by team members in Italy (INAF and INFN). This presentation will give an overview of the proposed IXPE mission, detailing the payload configuration, the expected sensitivity, and a typical observing program.

  11. The VIMOS Public Extragalactic Redshift Survey (VIPERS). The decline of cosmic star formation: quenching, mass, and environment connections

    Science.gov (United States)

    Cucciati, O.; Davidzon, I.; Bolzonella, M.; Granett, B. R.; De Lucia, G.; Branchini, E.; Zamorani, G.; Iovino, A.; Garilli, B.; Guzzo, L.; Scodeggio, M.; de la Torre, S.; Abbas, U.; Adami, C.; Arnouts, S.; Bottini, D.; Cappi, A.; Franzetti, P.; Fritz, A.; Krywult, J.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marulli, F.; Moutard, T.; Polletta, M.; Pollo, A.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Bel, J.; Blaizot, J.; Coupon, J.; Hawken, A.; Ilbert, O.; Moscardini, L.; Peacock, J. A.; Gargiulo, A.

    2017-06-01

    We use the final data of the VIMOS Public Extragalactic Redshift Survey (VIPERS) to investigate the effect of the environment on the evolution of galaxies between z = 0.5 and z = 0.9. We characterise local environment in terms of the density contrast smoothed over a cylindrical kernel, the scale of which is defined by the distance to the fifth nearest neighbour. This is performed by using a volume-limited sub-sample of galaxies complete up to z = 0.9, but allows us to attach a value of local density to all galaxies in the full VIPERS magnitude-limited sample to I web site is http://www.vipers.inaf.it/

  12. Atmospheres in a Test Tube

    Science.gov (United States)

    Claudi, R.; Erculiani, M. S.; Giro, E.; D'Alessandro, M.; Galletta, G.

    2013-09-01

    The "Atmosphere in a Test Tube" project is a laboratory experiment that will be able to reproduce condition of extreme environments by means of a simulator. These conditions span from those existing inside some parts of the human body to combinations of temperatures, pressures, irradiation and atmospheric gases present on other planets. In this latter case the experiments to be performed will be useful as preliminary tests for both simulation of atmosphere of exoplanets and Solar System planets and Astrobiology experiments that should be performed by planetary landers or by instruments to be launched in the next years. In particular at INAF Astronomical Observatory of Padova Laboratory we are approaching the characterization of extrasolar planet atmospheres taking advantage by innovative laboratory experiments with a particular focus on low mass Neptunes and Super earths and low mass M dwarfs primaries.

  13. INTEGRAL high-energy monitoring of the X-ray burster KS 1741-293

    Science.gov (United States)

    De Cesare, G.; Bazzano, A.; Martínez Núñez, S.; Stratta, G.; Tarana, A.; Del Santo, M.; Ubertini, P.

    2007-09-01

    KS 1741-293, discovered in 1989 by the X-ray camera TTM on the Kvant module of the Mir space station and identified as an X-ray burster, had not been detected in the hard X-ray band until the advent of the INTEGRAL observatory. Moreover, this source has recently been the object of scientific discussion, being also associated with a nearby extended radio source that in principle could be the supernova remnant produced by the accretion-induced collapse in the binary system. Our long-term monitoring with INTEGRAL, covering the period from 2003 February to 2005 May, confirms that KS 1741-293 is transient in the soft and hard X-ray bands. When the source is active, from a simultaneous JEM-X and IBIS data analysis, we provide a wide-band spectrum from 5 to 100 keV, which can be fitted by a two-component model: a multiple blackbody for the soft emission and a Comptonized or a cut-off power-law model for the hard component. Finally, by the detection of two X-ray bursters with JEM-X, we confirm the bursting nature of KS 1741-293, including this source in the class of hard-tailed X-ray bursters. Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), the Czech Republic and Poland, and with the participation of Russia and the USA. E-mail: giovanni.decesare@iasf-roma.inaf.it ‡ INAF personnel resident at ASDC.

  14. Functional coupling between sodium-activated potassium channels and voltage-dependent persistent sodium currents in cricket Kenyon cells.

    Science.gov (United States)

    Takahashi, Izumi; Yoshino, Masami

    2015-10-01

    In this study, we examined the functional coupling between Na(+)-activated potassium (KNa) channels and Na(+) influx through voltage-dependent Na(+) channels in Kenyon cells isolated from the mushroom body of the cricket Gryllus bimaculatus. Single-channel activity of KNa channels was recorded with the cell-attached patch configuration. The open probability (Po) of KNa channels increased with increasing Na(+) concentration in a bath solution, whereas it decreased by the substitution of Na(+) with an equimolar concentration of Li(+). The Po of KNa channels was also found to be reduced by bath application of a high concentration of TTX (1 μM) and riluzole (100 μM), which inhibits both fast (INaf) and persistent (INaP) Na(+) currents, whereas it was unaffected by a low concentration of TTX (10 nM), which selectively blocks INaf. Bath application of Cd(2+) at a low concentration (50 μM), as an inhibitor of INaP, also decreased the Po of KNa channels. Conversely, bath application of the inorganic Ca(2+)-channel blockers Co(2+) and Ni(2+) at high concentrations (500 μM) had little effect on the Po of KNa channels, although Cd(2+) (500 μM) reduced the Po of KNa channels. Perforated whole cell clamp analysis further indicated the presence of sustained outward currents for which amplitude was dependent on the amount of Na(+) influx. Taken together, these results indicate that KNa channels could be activated by Na(+) influx passing through voltage-dependent persistent Na(+) channels. The functional significance of this coupling mechanism was discussed in relation to the membrane excitability of Kenyon cells and its possible role in the formation of long-term memory. Copyright © 2015 the American Physiological Society.

  15. The VIMOS Public Extragalactic Redshift Survey (VIPERS). Full spectroscopic data and auxiliary information release (PDR-2)

    Science.gov (United States)

    Scodeggio, M.; Guzzo, L.; Garilli, B.; Granett, B. R.; Bolzonella, M.; de la Torre, S.; Abbas, U.; Adami, C.; Arnouts, S.; Bottini, D.; Cappi, A.; Coupon, J.; Cucciati, O.; Davidzon, I.; Franzetti, P.; Fritz, A.; Iovino, A.; Krywult, J.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marchetti, A.; Marulli, F.; Polletta, M.; Pollo, A.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Bel, J.; Branchini, E.; De Lucia, G.; Ilbert, O.; McCracken, H. J.; Moutard, T.; Peacock, J. A.; Zamorani, G.; Burden, A.; Fumana, M.; Jullo, E.; Marinoni, C.; Mellier, Y.; Moscardini, L.; Percival, W. J.

    2018-01-01

    We present the full public data release (PDR-2) of the VIMOS Public Extragalactic Redshift Survey (VIPERS), performed at the ESO VLT. We release redshifts, spectra, CFHTLS magnitudes and ancillary information (as masks and weights) for a complete sample of 86 775 galaxies (plus 4732 other objects, including stars and serendipitous galaxies); we also include their full photometrically-selected parent catalogue. The sample is magnitude limited to iAB ≤ 22.5, with an additional colour-colour pre-selection devised as to exclude galaxies at z performed through a fully automated pipeline; all redshift determinations were then visually validated and assigned a quality flag. Measurements with a quality flag ≥ 2 are shown to have a confidence level of 96% or larger and make up 88% of all measured galaxy redshifts (76 552 out of 86 775), constituting the VIPERS prime catalogue for statistical investigations. For this sample the rms redshift error, estimated using repeated measurements of about 3000 galaxies, is found to be σz = 0.00054(1 + z). All data are available at http://vipers.inaf.it and on the ESO Archive. Based on observations collected at the European Southern Observatory, Cerro Paranal, Chile, using the Very Large Telescope under programmes 182.A-0886 and partly 070.A-9007. Also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS web site is http://www.vipers.inaf.it/

  16. Coma dust environment observed by GIADA during the Perihelion of 67P/Churyumov-Gerasimenko.

    Science.gov (United States)

    Rotundi, A.; Della Corte, V.; Fulle, M.; Ferrari, M.; Ivanovski, S. L.; Sordini, R.; Mazzotta Epifani, E.; Palumbo, P.; Colangeli, L.; Lopez-Moreno, J. J.; Rodriguez, J.; Zakharov, V.; Bussoletti, E.; Crifo, J. F.; Esposito, F.; Green, S.; Gruen, E.; Lamy, P. L.; McDonnell, T.; Mennella, V.; Molina, A.; Moreno, F.; Ortiz, J. L.; Palomba, E.; Perrin, J. M.; Rodrigo, R.; Weissman, P. R.; Zarnecki, J.; Cosi, M.; Giovane, F.; Gustafson, B.; Herranz, M.; Jeronimo, J. M.; Leese, M.; Lopez-Jimenez, A.; Morales, R.

    2015-12-01

    GIADA (Grain Impact Analyzer and Dust Accumulator) is an in-situ instrument mounted onboard Rosetta monitoring the dust environment of comet 67P/Churyumov-Gerasimenko. GIADA is composed of 3 sub-systems: 1) the Grain Detection System, based on particle detection through light scattering; 2) the Impact Sensor, giving momentum measurement; 3) the Micro-Balances System, constituted of 5 quartz crystal microbalances, giving cumulative deposited dust. The combination of the measurements performed by these 3 subsystems provides: the number, the mass, the momentum and the speed distribution of dust particles emitted from the comet nucleus. We will present the coma dust environment as observed by GIADA during the perihelion phase of the Rosetta space mission. Despite the large distance from the nucleus, more than 200 km, GIADA was able to detect temporal and spatial variation of dust density distribution. Specific high dust spatial density sectors of the coma have been identified and their evolution during the perihelion phase was studied. Acknowledgements. GIADA was built by a consortium led by the Univ. Napoli "Parthenope" & INAF- Oss. Astr. Capodimonte, IT, in collaboration with the Inst. de Astrofisica de Andalucia, ES, Selex-ES s.p.a. and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with a support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developped from a PI proposal supported by the University of Kent; sci. & tech. contribution given by CISAS, IT, Lab. d'Astr. Spat., FR, and Institutions from UK, IT, FR, DE and USA. We thank the RSGS/ESAC, RMOC/ESOC & Rosetta Project/ESTEC for their outstanding work. Science support provided by NASA through the US Rosetta Project managed by JPL/California Institute of Technology. GIADA calibrated data will be available through the ESA's PSA web site.

  17. Windrum: a program for monitoring seismic signals in real time

    Science.gov (United States)

    Giudicepietro, Flora

    2017-04-01

    Windrum is a program devote to monitor seismic signals arriving from remote stations in real time. Since 2000, the Osservatorio Vesuviano (INGV) uses the first version of Windrum to monitor the seismic activity of Mt. Vesuvius, Campi Flegrei, Ischia and Stromboli volcano. The program has been also used at the Observatory of Bukittinggi (Indonesia), at the offices of the Italian National Civil Protection, at the COA in Stromboli and at the Civil Protection Center of the municipality of Pozzuoli (Napoli, Italy). In addition, the Osservatorio Vesuviano regularly uses Windrum in educational events such as the Festival of Science in Genova (Italy), FuturoRemoto and other events organized by Città della Scienza in Naples (Italy). The program displays the seismic trace of one station on a monitor, using short packet of data (typically 1 or 2 seconds) received through UTC Internet protocol. The data packets are in Trace_buffer format, a native protocol of Earthworm seismic system that is widely used for the data transmission on Internet. Windrum allows the user to visualize 24 hours of signals, to zoom selected windows of data, in order to estimate the duration Magnitude (Md) of an earthquake, in an intercative way, and to generate graphic images for the web. Moreover, Windrum can exchange Internet messages with other copies of the same program to synchronize actions, such as to zoom the same window of data or mark the beginning of an earthquake on all active monitors simultaneously. Originally, in 2000, Windrum was developed in VB6. I have now developed a new version in VB.net, which goes beyond the obsolescence problems that were appearing. The new version supports the decoding of binary packets received by soket in a more flexible way, allowing the generation of graphic images in different formats. In addition, the new version allows a more flexible layout configuration, suitable for use on large screens with high resolution. Over the past 17 years the use of Windrum

  18. Usefulness of syncope guidelines in risk stratification of syncope in emergency department.

    Science.gov (United States)

    Sruamsiri, Kamphee; Chenthanakij, Boriboon; Tantiwut, Aphinant; Wittayachamnankul, Borwon

    2014-02-01

    Management of patients with syncope in the Emergency Department now focuses on identifying patients who will be at future risk of serious morbidity. Among the risk stratification scoring systems being used were the San Francisco Syncope Rule (SFSR) and Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) score. To assess the accuracy of SFSR and OESIL score at predicting short-term serious outcome in Maharaj Nakorn Chiang Mai Hospital. In a prospective descriptive analysis study, adult patients presenting with syncope or near syncope between October 1, 2009 and April 24, 2010 were enrolled. All patients were followed-up at 7-day and 1-month. Statistical analysis included accuracy, sensitivity, specificity, predictive values, and likelihood ratios. One hundred seventy eight patients were enrolled in the present study. Fifty-three patients had a short-term serious outcome on follow-up. SFSR had 74.7% accuracy, 90.6% sensitivity, 68% specificity, 54.5% PPV 94.4% NPV likelihood ratio positive (LR+) of 2.8, and likelihood ratio negative (LR-) of 0.1, whereas OESIL score had 80.9% accuracy, 79.4% sensitivity, 81.6% specificity, 64.6% PPV 90.3% NPV, LR+ of 4.3, and LR- of 0.2. Both scores have good accuracy and sensitivity, but they should not be used as the only device in patient disposition. However, both scores showed a low false negative rate. Therefore, they may help in helping physician discharge low-risk patients.

  19. Syncope in the emergency department of a large northern Italian hospital: incidence, efficacy of a short-stay observation ward and validation of the OESIL risk score.

    Science.gov (United States)

    Numeroso, Filippo; Mossini, Gianluigi; Spaggiari, Eleonora; Cervellin, Gianfranco

    2010-09-01

    Syncope causes 1-3% of all emergency department (ED) visits, a high percentage of hospitalisations and prolonged hospital stay; nevertheless, many cases remain unexplained. This study analysed the incidence of syncope at the ED of the University Hospital of Parma in the first half of 2008; then a sample of 200 patients admitted later for syncope into the ED ward was studied, in order to evaluate the efficacy of a brief observation unit and to validate the Osservatorio Epidemiologico della Sincope nel Lazio (OESIL) risk score as a tool to identify cardiogenic syncopes. As reported in the literature, syncope accounts for 2.3% of ED consultations and for 4.2% of total hospital admissions. A brief observation ward in the ED seems to have the necessary characteristics for managing most cases of syncope quickly (3.5 days). The final diagnosis was certain in 60%, suspected in 33% and unexplained in 7% of patients. The commonest forms of syncope were non-cardiogenic. Factors associated with cardiogenic syncope were previous syncopal events, lack of prodromal symptoms and a high OESIL risk score.

  20. Collapse query cause: the management of adult syncope in the emergency department.

    Science.gov (United States)

    Reed, M J; Gray, A

    2006-08-01

    Syncope is a commonly encountered problem in the emergency department (ED). Its causes are many and varied, some of which are potentially life threatening. A review was carried out of relevant papers in the available literature, and this article attempts to assimilate current evidence relating to ED management. While the cause of syncope can be identified in many patients, and life threatening conditions subsequently treated, a risk stratification approach should be taken for those in whom a cause is not identified in the ED. Aspects of the history and examination that may help identify high risk patients are explored and the role of investigations to aid this stratification is discussed. Identifying a cardiac cause for syncope is a poor prognostic indicator. Patients with unexplained syncope who have significant cardiac disease should therefore be investigated thoroughly to determine the nature of the underlying heart disease and the cause of syncope, although presently there is little evidence that this improves their dismal prognosis. This risk stratification approach has led to the development of several clinical decision rules, which are discussed along with current international guidelines on syncope management. This review suggests that presently the American College of Emergency Physicians guidelines are the most useful aids specific to the management of syncope in the ED; however, the Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) score may also be a useful ED risk stratification tool.

  1. Association of corrected QT interval with long-term mortality in patients with syncope.

    Science.gov (United States)

    Balasubramaniyam, Nivas; Palaniswamy, Chandrasekar; Aronow, Wilbert S; Khera, Sahil; Balasubramanian, Gokulakrishnan; Harikrishnan, Prakash; Doshi, Jay V; Nabors, Christopher; Peterson, Stephen J; Sule, Sachin

    2013-12-30

    The electrocardiographic parameters QRS duration, QRS-T angle and QTc can predict mortality in patients with cardiovascular disease. The prgnostic value of these parameters in hospitalized patients with syncope needs investigation. We retrospectively studied 590 consecutive patients hospitalized with syncope. After excluding patients with baseline abnormal rhythm, QT- prolonging medications, and missing data, 459 patients were analyzed. Baseline demographic characteristics, co-morbidities, medication use, San Francisco Syncope Rule (SFSR) and Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) score and data on mortality were collected. The categorical variables and continuous variables of the 2 groups of patients with prolonged QTc and normal QTc interval were analyzed by Fischer's exact test and Mann-Whitney Test. A stepwise Cox regression model was used for time to death analysis. Of 459 patients, prolonged QTc interval was observed in 122 (27%). Mean follow-up was 41 months. Patients with prolonged QTc interval had higher prevalence of cardiovascular disease, OESIL score, high risk SFSR, hypertension, dyslipidemia, coronary artery disease, congestive heart failure, and increased mortality. Stepwise Cox regression analysis showed that significant independent prognostic factors for time to death were prolonged QTc interval (p = 0.005), age (p = 0.001), diabetes mellitus (p = 0.001) and history of malignancy (p = 0.006). QRS duration and QRS-T angle were not independent predictors of mortality. A prolonged QTc interval is an independent predictor of long-term mortality in hospitalized patients with syncope.

  2. Use of QT intervals for a more accurate diagnose of syncope and evaluation of syncope severity.

    Science.gov (United States)

    Buttà, C; Tuttolomondo, A; Casuccio, A; Di Raimondo, D; Giarrusso, L; Miceli, G; Lo Vecchio, S; Canino, B; Licata, G; Pinto, A

    2014-07-01

    This study aimed to evaluate the use of QT intervals, their diagnostic predictive value in patients with syncope and their relationship with syncope severity. One hundred and forty nine patients with a diagnosis of syncope were admitted to Internal Medicine departments at the University of Palermo, Italy, between 2006 and 2012, and 140 control subjects hospitalised for other causes were enrolled. QT maximum, QT minimum, QTpeak, QT corrected, QT dispersion and Tpeak-to-Tend interval were compared between two groups. The paper medical records were used for scoring with San Francisco Syncope Rule (SFSR), Evaluation of Guidelines in SYncope Study (EGSYS) score and Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) risk score. Mean QTc (p 424.8 ms (sensibility: 81.88 - specificity: 57.86) showed the greatest predictive value for diagnosis of syncope. On the EGSYS score and on the OESIL score, QTc was significantly prolonged in high-risk patients compared with low-risk patients. On the San Francisco Syncope Rule, QTc and QTdisp were significantly prolonged in high-risk patients compared with low-risk patients. Mean QTc, mean QTdisp, mean TpTe, mean QTmax and mean QTpeak were significantly longer in patients with syncope compared with control subjects. Furthermore, prolonged QTc and QTdisp were associated with major severe syncope according to San Francisco Syncope Rule, EGSYS and OESIL risk scores. © 2014 John Wiley & Sons Ltd.

  3. On the Theory of Sunspots Proposed by Signor Kirchoff

    Directory of Open Access Journals (Sweden)

    Secchi A.

    2011-07-01

    Full Text Available Eileen Reeves (Department of Comparative Literature, Princeton University, Princeton, New Jersey, 08544 and Mary Posani (Department of French and Italian, The Ohio State University, Columbus, Ohio, 43221 provide a translation of Father Pietro Angelo Secchi’s classic work “ Secchi A. Sulla Teoria Delle Macchie Solari: Proposta dal sig. Kirchoff” as it appeared in Bullettino Meteorologico dell’ Osservatorio del Collegio Romano , 31 January 1864, v.3(4, 1–4. This was the first treatise to propose a partic- ulate photosphere floating on the gaseous body of the Sun. The idea would dominate astrophysical thought for the next 50 years. Secchi appears to have drafted the article, as a response to Gustav Kirchhoff’s proposal, echoing early Galilean ideas, that sunspots represented clouds which floated above the photosphere. Other than presenting a new solar model, noteworthy aspects of this work include Secchi’s appropriate insistence that materials do not emit the same light at the same temperature and his gentle rebuke of Kirchhoff relative to commenting on questions of astronomy.

  4. A Note on the Constitution of the Sun

    Directory of Open Access Journals (Sweden)

    Magnus H. G.

    2011-07-01

    Full Text Available Patrice Robitaille (TAV College, Montreal, Canada provides a translation of Heinrich Gustav Magnus’ classic work Notiz ̈uber die Beschaffenheit der Sonne , as it appeared in March 1864 within Poggendorff’s Annalen der Physik und Chemie ,1864, v.131, 510– 512. The article had previously been translated into French: Notice sur la constitution du soleil. Archives des science physique et naturelles (Gen`eve , 1864, v.20, 171–175. This work formed the basis of the present translation. Heinrich Gustav Magnus (May 2, 1802 – April 4, 1870 was a professor at the University of Berlin and had studied in Paris under Joseph Louis Gay-Lussac. He would count amongst his students Wil- helm Beetz, Hermann Helmholtz, Gustav Wiedemann, John Tyndall, Rudolph Weber, and Adolph W ̈ ullner (Heinrich Gustav Magnus, Platinum Metals Review , 1976, v.20(1, 21–24. In his Notiz , Magnus demonstrated that the addition of sodium hydroxide to the gaseous flame resulted in a tremendous increase in luminosity. Magnus’ work would inspire Father Secchi to propose that the Sun was a gaseous globe whose photosphere contained condensed particulate matter (Secchi A. Sulla Struttura della Fotosfera So- lare. Bulletino Meteorologico dell’ Osservatorio del Collegio Romano , 1864, v.3(11, 1–3; English translation in Progr. Phys. , 2011, v.3, 30–32. Magnus’ report on the constitution of the Sun would continue to impact solar physics for two generations.

  5. [Waiting time between acute event and rehabilitation: continuity of nursing care and rehabilitation. Analysis and suggestions for a Service of Protected Discharge].

    Science.gov (United States)

    D'Ilio, Ilaria; Raimondi, Anna Maria; Radice, Laura; Di Mauro, Stefania

    2014-01-01

    In recent years, in Italy, population lengthening of life leads to an higher number of individuals with chronic diseases (Osservatorio, 2010). The hospital which deals with the acute phase of diseases needs to be integrated with primary care. This connection is particularly important for the treatment, care and rehabilitation of patient, as well as a general need for more health and social care integrated tools. At the San Gerardo Hospital in Monza, in the context of the patient's post-acute rehabilitation, we analyze the phase between discharge from hospital and the expected date of hospitalization in facilities providing rehabilitation. The aim of this observational descriptive study is to determine the distribution of days of waiting. Furthermore, several different approach are analysed (i.e. Integrated Home Care) in order to reduce unnecessary days hospitalization and a more intelligent and cost effective use of resources The research question are the follow, to quantify waiting time between discharge and hospitalization in the rehabilitation facility and to ascertain if patients are sent to the correct facility. 1083 individuals were taken into account, of those 55% (N=652) were discharged from the hospital later. This leads to a 4505 days of inappropriate hospitalization. Although the use of home care could be beneficial to the hospital, this can be used only for tiny part of the patients and it is not cost effective. A possible solution can be set up a number of low cost bed entirely managed by nurses due to the low level of intensity care.

  6. Il cielo sopra Roma I luoghi dell’astronomia

    CERN Document Server

    Buonanno, Roberto

    2008-01-01

    L’astronomia a Roma c’è sempre stata, ma un po’ nascosta: era nei palazzi, nelle chiese o, meglio, sopra le chiese, specole disseminate lungo un percorso che oramai conoscono in pochi. I romani hanno assistito, incuriositi ed impauriti, al rogo di Giordano Bruno in un angolo di Campo de' Fiori a loro familiare, ma probabilmente non capirono bene di quale colpa fosse accusato. Non pensarono certo che si trattasse di un filosofo e di uno scienziato che aveva cercato di immaginare in che modo era fatto il mondo. Chi era questo Galileo, di cui si celebrava il processo a S. Maria sopra Minerva? Era un uomo che voleva cambiare la prospettiva del mondo e che, per questo, era stato ammonito da Roberto Bellarmino. E chi era questo gesuita, Secchi, che nel 1870 costringeva gli Italiani a privare Roma del suo Osservatorio Astronomico, visto che il Direttore non riconosceva lo Stato Italiano? Come è possibile che dopo la visita di Hitler a Mussolini alla vigilia della Guerra, la Germania decise di regalare all’...

  7. Development of iridium coated x-ray mirrors for astronomical applications

    Science.gov (United States)

    Döhring, Thorsten; Probst, Anne-Catherine; Emmerich, Florian; Stollenwerk, Manfred; Stehlíková, Veronika; Friedrich, Peter; Damm, Christine

    2017-08-01

    Future space-based X-ray observatories need to be very lightweight for launcher mass constraints. Therefore they will use a reduced mirror thickness, which results in the additional requirement of low coating stress to avoid deformation of the initial precisely shaped mirror substrates. Due to their excellent reflection properties iridium coatings are sometimes applied for grazing incidence mirrors in astronomical X-ray telescopes. At Aschaffenburg University of Applied Sciences the coating of thin iridium films by an RF-magnetron sputtering technique is under development. The work is embedded in collaborations with the Max-Planck-Institute for Extraterrestrial Physics in Germany, the Czech Technical University in Prague, the Osservatorio Astronomico di Brera in Italy, the German Leibniz Institute for Solid State and Materials Research in Dresden, and the French Institute Fresnel. Sputtering with different parameters leads to iridium films with different properties. The current work is focused on the microstructure of the iridium coatings to study the influence of the substrate and of the argon gas pressure on the thin film growing process. Correlations between coating density, surface micro-roughness, the crystalline structure of the iridium layers, and the expected reflectivity of the X-ray mirror as well as coating stress effects are presented and discussed. The final goal of the project is to integrate the produced prototype mirrors into an X-ray telescope module. On a longer timescale measurements of the mirror modules optical performance are planned at the X-ray test facility PANTER.

  8. Clinical trials and gender medicine.

    Science.gov (United States)

    Cassese, Mariarita; Zuber, Veronica

    2011-01-01

    Women use more medicines than men because they fall ill more often and suffer more from chronic diseases, but also because women pay more attention to their health and have more consciousness and care about themselves. Although medicines can have different effects on women and men, women still represent a small percentage in the first phases of trials (22%) which are essential to verify drugs dosage, side effects, and safety. Even though women are more present in trials, studies results are not presented with a gender approach. This situation is due to educational, social, ethical and economical factors. The scientific research must increase feminine presence in clinical trials in order to be equal and correct, and all the key stakeholder should be involved in this process. We still have a long way to cover and it doesn't concern only women but also children and old people. The aim is to have a medicine not only illness-focused but patient-focused: a medicine able to take into consideration all the patient characteristics and so to produce a really personalized therapy. What above described is part of the reasons why in 2005 was founded the National Observatory for Women's Health (Osservatorio Nazionale sulla Salute della Donna, ONDa) which promotes a gender health awareness and culture in Italy, at all the levels of the civil and scientific society.

  9. Clinical trials and gender medicine

    Directory of Open Access Journals (Sweden)

    Mariarita Cassese

    2011-01-01

    Full Text Available Women use more medicines than men because they fall ill more often and suffer more from chronic diseases, but also because women pay more attention to their health and have more consciousness and care about themselves. Although medicines can have different effects on women and men, women still represent a small percentage in the first phases of trials (22% which are essential to verify drugs dosage, side effects, and safety. Even though women are more present in trials, studies results are not presented with a gender approach. This situation is due to educational, social, ethical and economical factors. The scientific research must increase feminine presence in clinical trials in order to be equal and correct, and all the key stakeholder should be involved in this process. We still have a long way to cover and it doesn't concern only women but also children and old people. The aim is to have a medicine not only illness-focused but patient-focused: a medicine able to take into consideration all the patient characteristics and so to produce a really personalized therapy. What above described is part of the reasons why in 2005 was founded the National Observatory for Women's Health (Osservatorio Nazionale sulla Salute della Donna, ONDa which promotes a gender health awareness and culture in Italy, at all the levels of the civil and scientific society.

  10. Geophysical monitoring of a complex geologic framework: the multi-disciplinary sensor networks in Sicily (Italy)

    Science.gov (United States)

    Cantarero, M.; Di Prima, S.; Mattia, M.; Patanè, D.; Rossi, M.

    2012-04-01

    Since 2004 the Osservatorio Etneo INGV has begun a new approach to the geophysical monitoring of volcanic and seismic areas of Sicily (Italy) where the core is a new type of remote infrastructure able to efficiently accommodate different kinds of sensor. In particular our multi-parametric network is mainly focused on the monitoring of different geophysical parameters (seismic ground velocity and acceleration, infrasound and ground deformation GPS).The whole seismic network consists of 66 broad band digital stations, 19 analog stations, 13 accelerometric stations and 12 infrasonic stations, for a total of 110 stations while the Continuous GPS network consist of 80 stations. Every station is equipped with solar panels in order to satisfy the power requirements of the instruments and with satellite-based communication systems. In this work we show both the technical solutions of this integrated network and its main advantages, if compared with older kinds of remote stations. Moreover we show some examples of the more interesting scientific results achieved thank to this technologically advanced network.

  11. Raccontare, Ascoltare, Comprendere: metodologia e ambiti di applicazione delle narrazioni nelle scienze sociali

    Directory of Open Access Journals (Sweden)

    Barbara Poggio

    2012-04-01

    Full Text Available Il convegno "Raccontare, Ascoltare, Comprendere: Metodologia e ambiti di applicazione delle narrazioni nelle scienze sociali", organizzato dal Dipartimento di Sociologia e Ricerca Sociale dell'Università di Trento il 22-23 settembre 2011, realizzato con il patrocinio dell'Associazione Italiana di Sociologia e dell'Osservatorio dei Processi Comunicativi, ha proposto di stimolare un confronto tra studiose e studiosi delle scienze sociali che all'interno di diverse aree tematiche utilizzano le narrazioni come principale strumento di ricerca e di analisi, nell'intento di valorizzare la capacità euristica offerta dall'approccio narrativo e biografico nel leggere ed interpretare la società. Presentiamo all'interno di questo numero monografico, in collaborazione con la rivista internazionale di scienze umane e sociali "M@gm@", una selezione delle relazioni discusse al convegno che documentano la preziosa occasione, di scambio di riflessioni metodologiche e di esperienze di ricerca empirica, rappresentata da queste due intense giornate di lavori.

  12. Development of Constellation-X optics technologies at MSFC

    Science.gov (United States)

    O'Dell, Stephen L.; Jones, William D.; Ramsey, Brian D.; Engelhaupt, Darell E.; Smith, Winfred S.; Cohen, Lester M.; Van Speybroeck, Leon P.

    2000-07-01

    The Constellation X-ray Mission is the next major x-ray- astronomy mission in the NASA Space Science road map. As a follow-on to the Chandra X-ray Observatory--nee, the Advanced X-ray Astrophysics Facility--Constellation X will provide high-throughput, high-resolution spectroscopy to probe the gravitational field, kinematics, temperature, density, composition and ionization state of cosmic sources. The Constellation-X observatory system comprises four separate satellites, each with one large Spectroscopy X-ray Telescope (SXT, with a pixelated microcalorimeter and a reflection-grating-CCD spectrometer) and three smaller Hard X-ray Telescopes (HXTs, with pixelated hard-x-ray detectors). Essential to the success of Constellation X is the development of large (1.6-m-diameter), lightweight optics for the SXT mirror assembly. With the Smithsonian Astrophysical Observatory, teams led by NASA's Marshall Space Flight Center, by NASA's Goddard Space Flight Center, and by Italy's Osservatorio Astronomico di Brera are currently developing competing mirror techniques for lightweight SXT optics, toward achieving the required system-level half-power diameter--better than 15 arcsec.

  13. Marine geophysical methods for archaeological investigation of volcanic and bradyseismic areas

    Directory of Open Access Journals (Sweden)

    F. Giordano

    1995-06-01

    Full Text Available The aim of this work was to test several geophysical methods for the identification and study of submerged prehistorical coastlines and archaeological sites. This research program was carried out in collaboration with the <<Osservatorio Vesuviano>> in the Gulf of Pozzuoli and dealt in particular with the bathymetric strips extending from - 5 m to - 50 m Within these strips we identified the coastline dating from the Rornan period. former beach boundaries associated with the vertical movements of the earth's surface caused by seismic-volcanic activity, and the variations in sea level following the climactic changes throughout the last 15000 years. The UNIBOOM system was used for this part of the programme, perinittiilg the identification of several coastlines and submerged beaches lying at different levels. The use of a modern Side Scan Sonar - for the morphological invesdgation of the sea bed - in a zone which had been the object of numerous archaeological surveys in the past, permitted previously unknown structures near the Lacuus Baianus to be identified. Other features worth pointing out include the operating speed of the system (15000 m'lfirst minute approx and its observation capacity in cloudy waters compared to visible radiation, as well as its ability to penetrate thin layers of mud which generally impede direct underwater observation.

  14. Instrumental seismic catalogue of Mt. Etna earthquakes (Sicily, Italy: ten years (2000-2010 of instrumental recordings

    Directory of Open Access Journals (Sweden)

    Salvatore Alparone

    2015-10-01

    Full Text Available Instrumental seismic catalogues are an essential tool for the zonation of the territory and the production of seismic hazard maps. They are also a valuable instrument for detailed seismological studies regarding active volcanoes and, above all, for interpreting the magma dynamics and the evolution of eruptive phenomena. In this paper, we show the first instrumental earthquake catalogue of Mt. Etna, for the period 2000-2010, with the purpose of producing a homogeneous dataset of 10 years of seismological observations. During this period, 16,845 earthquakes have been recorded by the seismic network run by the Istituto Nazionale di Geofisica and Vulcanologia, Osservatorio Etneo, in Catania. A total of 6,330 events, corresponding to approximately 40% of all earthquakes recorded, were located by using a one-dimensional VP velocity model. The magnitude completeness of the catalogue is equal to about 1.5 for the whole period, except for some short periods in 2001 and 2002-2003 and at the end of 2009. The reliability of the data collected is supported by the good values of the main hypocentral parameters through the time. The spatial distribution of seismicity allowed the highlighting of several seismogenetic areas characterized by different seismic rates and focal depths. This seismic catalogue represents a fundamental tool for several research aiming to a better understanding of the behavior of an active volcano such as Mt. Etna. 

  15. Seismic and volcanic activity during 2014 in the region involved by TOMO-ETNA seismic active experiment

    Directory of Open Access Journals (Sweden)

    Graziella Barberi

    2016-09-01

    Full Text Available This paper presents an overview of the seismic and volcanic activity occurred during 2014 in the region involved by the TOMO-ETNA seismic active experiment (Mt. Etna, Aeolian Islands and Peloritani-Messina Strait areas. To better characterize the seismicity over the year, three-dimensional hypocenter locations and focal mechanism solutions of a dataset of 678 selected small-to-moderate magnitude earthquakes (0.5 ≤ ML ≤ 4.3 were analyzed. In the framework of the TOMO-ETNA experiment, a temporary seismic network was installed on-land from June to November 2014, both to acquire seismic signals produced by shots and to record the local seismicity. Data collected by the temporary network were used to integrate those deriving from the permanent seismic network operated by the Istituto Nazionale di Geofisica e Vulcanologia (INGV-Osservatorio Etneo (Etna Observatory, thus obtaining a numerically more robust dataset. In agreement with previous analysis and studies, the distribution of the hypocentral locations is well representative of the seismicity that typically characterizes this area. The selected well-constrained 42 fault plane solutions evidence two domains characterized by different motions and style of deformation. In particular, an extensional domain in the northeastern Sicily and a strike-slip regime in the northernmost part of the studied region have been observed.

  16. Shaded relief magnetic anomaly map of Italy and surrounding marine areas

    International Nuclear Information System (INIS)

    Chiappini, M.; Meloni, A.; Boschi, E.; Faggioni, O.; Beverini, N.; Carmisciano, C.; Marson, I.

    2000-01-01

    Magnetic observations made onshore the Italian Peninsula, and across the adjacent seas, have been compiled in a new digital database that provides the first complete regional scale view of the crustal scale magnetic anomalies of the regional at sea level. The offshore data were acquired between 1965-1972 by the Osservatorio Geofisico Sperimentale (OGS) while the ground measurements were performed within the framework of the Progetto Finalizzato Geodinamica of the Calling's Nazionale delle Ricerche (PFG-CNR) between 1977 and 1981. The new shaded relief magnetic anomaly map of total intensity of the Earth's magnetic field for Italy and the surrounding seas has been produced at sea level, for the geomagnetic epoch 1979.0. The most remarkable result of this new map, with respect to the previous compilations and to the aero magnetic map of Italy, is an unprecedented view of the magnetic signature of the major tectonic elements in their regional setting. There is good correlation between known structural geology and the magnetic anomalies, and now that the longer wavelength signatures have been corrected, deeper interpretations are possible

  17. Shaded relief magnetic anomaly map of Italy and surrounding marine areas

    Directory of Open Access Journals (Sweden)

    C. Carmisciano

    2000-06-01

    Full Text Available Magnetic observations made onshore the Italian Peninsula, and across the adjacent seas, have been compiled in a new digital database that provides the first complete regional scale view of the crustal scale magnetic anomalies of the region at sea level. The offshore data were acquired between 1965-1972 by the Osservatorio Geofisico Sperimentale (OGS while the ground measurements were performed within the framework of the Progetto Finalizzato Geodinamica of the Consiglio Nazionale delle Ricerche (PFG-CNR between 1977 and 1981. The new shaded relief magnetic anomaly map of total intensity of the Earth's magnetic field for Italy and the surrounding seas has been produced at sea level, for the geomagnetic epoch 1979.0. The most remarkable result of this new map, with respect to the previous compilations and to the aeromagnetic map of Italy, is an unprecedented view of the magnetic signature of the major tectonic elements in their regional setting. There is good correlation between known structural geology and the magnetic anomalies, and now that the longer wavelength signatures have been corrected, deeper interpretations are possible.

  18. FUTURO REMOTO 2015: researchers meet people.

    Science.gov (United States)

    De Lucia, Maddalena; Fedele, Alessandro; Esposito, Roberta; Torello, Vincenzo; Nave, Rosella; Pino, Nicola Alessandro; Russo, Massimo; Alessio, Giuliana; Gaudiosi, Germana; Nappi, Rosa; Belviso, Pasquale; Carandente, Antonio; De Cesare, Walter; Sansivero, Fabio; Siniscalchi, Valeria; Borgstrom, Sven; Milano, Girolamo; Pasquale Ricciardi, Giovanni; De Natale, Giuseppe

    2016-04-01

    As participant of the 29th Edition of the cultural initiative "Futuro Remoto 2015", the INGV section of Naples Osservatorio Vesuviano has realized a temporary exhibition aimed to build bridges between the scientific community and the public. The event, a festival of art, culture, science and technology, has taken place on October 15th - 19th 2015, in Naples, Italy, in the city center, and was organized by "Città della Scienza", the science center of the city of Naples, belonging to the ECSITE netwok.. The total number of visitors was about 130.000 people. It was a free and open access event, funded by public institutions. Sharing their scientific expertise with the public, in the "Terra" ("Earth") stand the INGV-OV researchers have shown, with interactive labs, how progress in technology and research develope and allow a better understanding of the dynamic processes and of the evolution of our planet. Popularizing science, when widely accessible to the people, make the knowledge not remaining confined to an elite, being efficiently spread in society, with deep implications in the social role of researchers. Practical activities and labs, dialogues and interaction with researchers of INGV-OV have allowed young and adult public, schools, students, experts or simply curious people to deepen burning issues in an area exposed to high seismic and volcanic risk.

  19. GIADA onboard Rosetta characterising comet 67/PChuryumov-Gerasimenko dust environment inbound to and outbound from perihelion.

    Science.gov (United States)

    Della Corte, Vincenzo; Rotundi, Alessandra; Fulle, Marco

    2016-07-01

    GIADA (Grain Impact Analyzer and Dust Accumulator) is an in-situ instrument onboard Rosetta monitoring the dust environment of comet 67P/Churyumov-Gerasimenko. GIADA is composed of 3 sub-systems: 1) the Grain Detection System, based on particle detection through light scattering; 2) the Impact Sensor, measuring particle momentum; 3) the Micro-Balances System, constituted of 5 quartz crystal microbalances, providing cumulated dust from different directions. From the combination of the measurements performed by the three subsystems we retrieve: the number, the mass, the momentum, the speed of individual dust particles and the cumulative dust flux emitted from the comet nucleus. We will present the coma dust environment as observed by GIADA during the pre-landing and escort phases of the Rosetta space mission. GIADA was able to detect temporal and spatial variation of dust density distribution and to disentangle different types of impacting dust particles. Specific high dust spatial density sectors of the coma have been identified and their evolution with respect to the heliocentric distance was studied. From August 2014 to December 2015, i.e. inbound, at and outbound perihelion, Rosetta performed different trajectories around the nucleus and flybys with different close approach distances, different coordinates of the sub-spacecraft point and different observing geometry (phase angle), allowed GIADA to characterize the dust environment within the 67P/C-G coma and its temporal variation. Acknowledgements. GIADA was built by a consortium led by the Univ. Napoli "Parthenope" & INAF- Oss. Astr. Capodimonte, IT, in collaboration with the Inst. de Astrofisica de Andalucia, ES, Selex-ES s.p.a. and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with a support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developed from a PI proposal

  20. Giada improved calibration of measurement subsystems

    Science.gov (United States)

    Della Corte, V.; Rotundi, A.; Sordini, R.; Accolla, M.; Ferrari, M.; Ivanovski, S.; Lucarelli, F.; Mazzotta Epifani, E.; Palumbo, P.

    2014-12-01

    GIADA (Grain Impact Analyzer and Dust Accumulator) is an in-situ instrument devoted to measure the dynamical properties of the dust grains emitted by the comet. An Extended Calibration activity using the GIADA Flight Spare Model has been carried out taking into account the knowledge gained through the analyses of IDPs and cometary samples returned from comet 81P/Wild 2. GIADA consists of three measurement subsystems: Grain Detection System, an optical device measuring the optical cross-section for individual dust; Impact Sensor an aluminum plate connected to 5 piezo-sensors measuring the momentum of impacting single dust grains; Micro Balance System measuring the cumulative deposition in time of dust grains smaller than 10 μm. The results of the analyses on data acquired with the GIADA PFM and the comparison with calibration data acquired during the pre-launch campaign allowed us to improve GIADA performances and capabilities. We will report the results of the following main activities: a) definition of a correlation between the 2 GIADA Models (PFM housed in laboratory and In-Flight Model on-board ROSETTA); b) characterization of the sub-systems performances (signal elaboration, sensitivities, space environment effects); c) new calibration measurements and related curves by means of the PFM model using realistic cometary dust analogues. Acknowledgements: GIADA was built by a consortium led by the Univ. Napoli "Parthenope" & INAF-Oss. Astr. Capodimonte, IT, in collaboration with the Inst. de Astrofisica de Andalucia, ES, Selex-ES s.p.a. and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with a support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developed from a University of Kent, UK, PI proposal; sci. & tech. contribution given by CISAS, IT, Lab. d'Astr. Spat., FR, and Institutions from UK, IT, FR, DE and USA. We thank

  1. GIADA On-Board Rosetta: Early Dust Grain Detections and Dust Coma Characterization of Comet 67P/C-G

    Science.gov (United States)

    Rotundi, A.; Della Corte, V.; Accolla, M.; Ferrari, M.; Ivanovski, S.; Lucarelli, F.; Mazzotta Epifani, E.; Sordini, R.; Palumbo, P.; Colangeli, L.; Lopez-Moreno, J. J.; Rodriguez, J.; Fulle, M.; Bussoletti, E.; Crifo, J. F.; Esposito, F.; Green, S.; Grün, E.; Lamy, P. L.; McDonnell, T.; Mennella, V.; Molina, A.; Moreno, F.; Ortiz, J. L.; Palomba, E.; Perrin, J. M.; Rodrigo, R.; Weissman, P. R.; Zakharov, V.; Zarnecki, J.

    2014-12-01

    GIADA (Grain Impact Analyzer and Dust Accumulator) flying on-board Rosetta is devoted to study the cometary dust environment of 67P/Churiumov-Gerasimenko. GIADA is composed of 3 sub-systems: the GDS (Grain Detection System), based on grain detection through light scattering; an IS (Impact Sensor), giving momentum measurement detecting the impact on a sensed plate connected with 5 piezoelectric sensors; the MBS (MicroBalances System), constituted of 5 Quartz Crystal Microbalances (QCMs), giving cumulative deposited dust mass by measuring the variations of the sensors' frequency. The combination of the measurements performed by these 3 subsystems provides: the number, the mass, the momentum and the velocity distribution of dust grains emitted from the cometary nucleus.No prior in situ dust dynamical measurements at these close distances from the nucleus and starting from such large heliocentric distances are available up to date. We present here the first results obtained from the beginning of the Rosetta scientific phase. We will report dust grains early detection at about 800 km from the nucleus in August 2014 and the following measurements that allowed us characterizing the 67P/C-G dust environment at distances less than 100 km from the nucleus and single grains dynamical properties. Acknowledgements. GIADA was built by a consortium led by the Univ. Napoli "Parthenope" & INAF-Oss. Astr. Capodimonte, IT, in collaboration with the Inst. de Astrofisica de Andalucia, ES, Selex-ES s.p.a. and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with a support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developped from a PI proposal supported by the University of Kent; sci. & tech. contribution given by CISAS, IT, Lab. d'Astr. Spat., FR, and Institutions from UK, IT, FR, DE and USA. We thank the RSGS/ESAC, RMOC/ESOC & Rosetta Project

  2. Monitoring Comet 67P/C-G Micrometer Dust Flux: GIADA onboard Rosetta.

    Science.gov (United States)

    Della Corte, Vincenzo; Rotundi, Alessandra; Ivanovski, Stavro; Accolla, Mario; Ferrari, Marco; Sordini, Roberto; Lucarelli, Francesca; Zakharov, Vladimir; Fulle, Marco; Mazzotta Epifani, Elena; López-Moreno, José J.; Rodríguez, Julio; Colangeli, Luigi; Palumbo, Pasquale; Bussoletti, Ezio; Crifo, Jean-Francois; Esposito, Francesca; Green, Simon F.; Grün, Eberhard; Lamy, Philippe L.

    2015-04-01

    (21)ESA-ESAC, Camino Bajo del Castillo, s/n., Urb. Villafranca del Castillo, 28692 Villanueva de la Cañada, Madrid, Spagna The MicroBalance System (MBS) is one of the three measurement subsystems of GIADA, the Grain Impact Analyzer and Dust Accumulator on board the Rosetta/ESA spacecraft (S/C). It consists of five Quartz Crystal Microbalances (QCMs) in roughly orthogonal directions providing the cumulative dust flux of grains smaller than 10 microns. The MBS is continuously monitoring comet 67P/CG since the beginning of May 2014. During the first 4 months of measurements, before the insertion of the S/C in the bound orbit phase, there were no evidences of dust accumulation on the QCMs. Starting from the beginning of October, three out of five QCMs measured an increase of the deposited dust. The measured fluxes show, as expected, a strong anisotropy. In particular, the dust flux appears to be much higher from the Sun direction with respect to the comet direction. Acknowledgment: GIADA was built by a consortum led by the Univ. Napoli "Parthenope" & INAF- Oss. Astr. Capodimonte, in collaboration with the Inst. de Astrofisica de Andalucia, Selex-ES, FI and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with the support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developed from a PI proposal from the University of Kent; sci. & tech. contribution were provided by CISAS, IT, Lab. d'Astr. Spat., FR, and Institutions from UK, IT, FR, DE and USA. We thank the RSGS/ESAC, RMOC/ESOC & Rosetta Project/ESTEC for their out-standing work. Science support provided was by NASA through the US Rosetta Project managed by the Jet Propulsion Laboratory/ California Institute of Technology. GIADA calibrated data will be available through ESA's PSA web site (www.rssd.esa.int/index.php? project=PSA&page=in dex). We would like to thank Angioletta

  3. Reflective and antireflective coatings for the optical chain of the ASTRI SST-2M prototype

    Science.gov (United States)

    Bonnoli, Giacomo; Canestrari, Rodolfo; Catalano, Osvaldo; Pareschi, Giovanni; Perri, Luca; Stringhetti, Luca

    2013-09-01

    ASTRI is a Flagship Project of the Italian Ministry of Education, University and Research, led by the Italian National Institute of Astrophysics, INAF. One of the main aims of the ASTRI Project is the design, construction and on-field verification of a dual mirror (2M) end-to-end prototype for the Small Size Telescope (SST) envisaged to become part of the Cherenkov Telescope Array. The ASTRI SST-2M prototype is designed according to the Schwarzschild-Couder optical scheme, and adopts a camera based on Silicon Photo Multipliers (SiPM); it will be assembled at the INAF astronomical site of Serra La Nave on mount Etna (Catania, Italy) in the second half of 2014, and will start scientific validation phase soon after. With its 4m wide primary dish, the telescope will be sensitive to multi-TeV Very High Energy (VHE) gamma rays up to 100 TeV and above, with a point spread function of ~2 arcminutes and a wide (semiaperture 4.8°) corrected field of view. The peculiarities of the optical design and of the SiPM bandpass pushed towards specifically optimized choices in terms of reflective coatings for both the primary and the secondary mirror. Fully dielectric multi-layer coatings have been developed and tested as an option for the primary mirror, aiming to filter out the large Night Sky Background contamination at wavelengths λ>~700 nm. On the other hand, for the large monolithic secondary mirror a simpler design with quartz-overcoated aluminium has been optimized for incidences far from normality. The conformation of the ASTRI camera in turn pushed towards the design of a reimaging system based on thin pyramidal light guides, that could be optionally integrated in the focal surface, aiming to increase the fill factor. An anti-reflective coating optimized for a wide range of incident angles faraway from normality was specifically developed to enhance the UV-optical transparency of these elements. The issues, strategy, simulations and experimental results are thoroughly

  4. Nbody Simulations and Weak Gravitational Lensing using new HPC-Grid resources: the PI2S2 project

    Science.gov (United States)

    Becciani, U.; Antonuccio-Delogu, V.; Costa, A.; Comparato, M.

    2008-08-01

    We present the main project of the new grid infrastructure and the researches, that have been already started in Sicily and will be completed by next year. The PI2S2 project of the COMETA consortium is funded by the Italian Ministry of University and Research and will be completed in 2009. Funds are from the European Union Structural Funds for Objective 1 regions. The project, together with a similar project called Trinacria GRID Virtual Laboratory (Trigrid VL), aims to create in Sicily a computational grid for e-science and e-commerce applications with the main goal of increasing the technological innovation of local enterprises and their competition on the global market. PI2S2 project aims to build and develop an e-Infrastructure in Sicily, based on the grid paradigm, mainly for research activity using the grid environment and High Performance Computer systems. As an example we present the first results of a new grid version of FLY a tree Nbody code developed by INAF Astrophysical Observatory of Catania, already published in the CPC program Library, that will be used in the Weak Gravitational Lensing field.

  5. INTRIGOSS: A new Library of High Resolution Synthetic Spectra

    Science.gov (United States)

    Franchini, Mariagrazia; Morossi, Carlo; Di Marcancantonio, Paolo; Chavez, Miguel; GES-Builders

    2018-01-01

    INTRIGOSS (INaf Trieste Grid Of Synthetic Spectra) is a new High Resolution (HiRes) synthetic spectral library designed for studying F, G, and K stars. The library is based on atmosphere models computed with specified individual element abundances via ATLAS12 code. Normalized SPectra (NSP) and surface Flux SPectra (FSP), in the 4800-5400 Å wavelength range, were computed by means of the SPECTRUM code. The synthetic spectra are computed with an atomic and bi-atomic molecular line list including "bona fide" Predicted Lines (PLs) built by tuning loggf to reproduce very high SNR Solar spectrum and the UVES-U580 spectra of five cool giants extracted from the Gaia-ESO survey (GES). The astrophysical gf-values were then assessed by using more than 2000 stars with homogenous and accurate atmosphere parameters and detailed chemical composition from GES. The validity and greater accuracy of INTRIGOSS NSPs and FSPs with respect to other available spectral libraries is discussed. INTRIGOSS will be available on the web and will be a valuable tool for both stellar atmospheric parameters and stellar population studies.

  6. A European Roadmap for Research in Astrobiology - The AstRoMap Roadmap

    Science.gov (United States)

    Gómez, F.; Walter, N.; Horneck, G.; Muller, C.; Rettberg, P.; Capria, M.; Palomba, E.

    2015-10-01

    AstRoMap (Astrobiology Road Mapping activity-www.astromap-eu.org) is a collaborative project which will provide the European Planetary Science Community with a road map in astrobiology. The goals of the project have been: (i) to pose big questions related to astrobiology; and (ii) the identification of experiments, new technology and/or those space missions to be developed in future programs and which could answer those big questions. This collaborative infrastructure includes the organization of expert panels and international workshops in order to discuss about those big questions and the science objectives by the community to be addressed. The main deliverable will be a Roadmap document. The project is steered by a consortium of six European and national research institutes and associations: -­- Centro de Astrobiologica (INTACSIC), Spain -­- European Science Foundation, France -­- Association pour un Réseau Européen d'Exo/Astrobiology (EANA), France -­- B-USOC, Belgium -­- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Germany -­- National Institute for Astrophysics (INAF), ItalyOrigin and evolution of planetary systems -­- Origin of organic compounds in space -­- Rock-water-carbon interactions, organic synthesis, and steps to life -­- Life and habitability on Earth and in Space -­- -­- Biosignatures as facilitating life detection The key topics will focus on a limited number of strategic scientific objectives to be addressed in the next 20 years by European astrobiologists, and suggest research activities for future development.

  7. The VIMOS Public Extragalactic Redshift Survey (VIPERS):. A quiescent formation of massive red-sequence galaxies over the past 9 Gyr

    Science.gov (United States)

    Fritz, A.; Scodeggio, M.; Ilbert, O.; Bolzonella, M.; Davidzon, I.; Coupon, J.; Garilli, B.; Guzzo, L.; Zamorani, G.; Abbas, U.; Adami, C.; Arnouts, S.; Bel, J.; Bottini, D.; Branchini, E.; Cappi, A.; Cucciati, O.; De Lucia, G.; de la Torre, S.; Franzetti, P.; Fumana, M.; Granett, B. R.; Iovino, A.; Krywult, J.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marulli, F.; McCracken, H. J.; Paioro, L.; Polletta, M.; Pollo, A.; Schlagenhaufer, H.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Burden, A.; Di Porto, C.; Marchetti, A.; Marinoni, C.; Mellier, Y.; Moscardini, L.; Nichol, R. C.; Peacock, J. A.; Percival, W. J.; Phleps, S.; Wolk, M.

    2014-03-01

    We explore the evolution of the colour-magnitude relation (CMR) and luminosity function (LF) at 0.4 contamination varies for the different methods and with redshift, but regardless of the method we measure a consistent evolution of the red-sequence (RS). Between 0.4 1011 M⊙) and expeditious RS formation over a short period of ~1.5 Gyr starting before z = 1. This is supported by the detection of ongoing SF in early-type galaxies at 0.9 Chile, using the Very Large Telescope under programs 182.A-0886 and partly 070.A-9007. Also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS website is http://www.vipers.inaf.it/.Appendices are available in electronic form at http://www.aanda.org

  8. A COMPUTER CLUSTER SYSTEM FOR PSEUDO-PARALLEL EXECUTION OF GEANT4 SERIAL APPLICATION

    Directory of Open Access Journals (Sweden)

    Memmo Federici

    2013-12-01

    Full Text Available Simulation of the interactions between particles and matter in studies for developing X-rays detectors generally requires very long calculation times (up to several days or weeks. These times are often a serious limitation for the success of the simulations and for the accuracy of the simulated models. One of the tools used by the scientific community to perform these simulations is Geant4 (Geometry And Tracking [2, 3]. On the best of experience in the design of the AVES cluster computing system, Federici et al. [1], the IAPS (Istituto di Astrofisica e Planetologia Spaziali INAF laboratories were able to develop a cluster computer system dedicated to Geant 4. The Cluster is easy to use and easily expandable, and thanks to the design criteria adopted it achieves an excellent compromise between performance and cost. The management software developed for the Cluster splits the single instance of simulation on the cores available, allowing the use of software written for serial computation to reach a computing speed similar to that obtainable from a native parallel software. The simulations carried out on the Cluster showed an increase in execution time by a factor of 20 to 60 compared to the times obtained with the use of a single PC of medium quality.

  9. Optimization of detectors positioning with respect to flying dynamics for future formation flight missions

    Science.gov (United States)

    Civitani, Marta; Djalal, Sophie; Chipaux, Remi

    2009-08-01

    In a X-ray telescope in formation flight configuration, the optics and the focal-plane detectors reside in two different spacecraft. The dynamics of the detector spacecraft (DSC) with respect to the mirror spacecraft (MSC, carrying the mirrors of the telescope) changes continuously the arrival positions of the photons on the detectors. In this paper we analyze this issue for the case of the SIMBOL-X hard X-ray mission, extensively studied by CNES and ASI until 2009 spring. Due to the existing gaps between pixels and between detector modules, the dynamics of the system may produce a relevant photometric effect. The aim of this work is to present the optimization study of the control-law algorithm with respect to the detector's geometry. As the photometric effect may vary depending upon position of the source image on the detector, the analysis-carried out using the simuLOS (INAF, CNES, CEA) simulation tool-is extended over the entire SIMBOL-X field of view.

  10. Geneva University: Particle Acceleration in supernova remnants and its implications for the origin of galactic cosmic rays

    CERN Multimedia

    Université de Genève

    2012-01-01

    GENEVA UNIVERSITY École de physique Département de physique nucléaire et corspusculaire 24, quai Ernest-Ansermet 1211 Genève 4 Tél.: (022) 379 62 73 Fax: (022) 379 69 92 Wednesday 28 March 2012 SEMINAIRE DE PHYSIQUE CORPUSCULAIRE 11h15 - Science III, Auditoire 1S081 Particle Acceleration in supernova remnants and its implications for the origin of galactic cosmic rays Prof. Pasquale BLASI INAF, Arcetri Observatory, Firenze The process of cosmic ray energization in supernova remnant shocks is described by the theory of non linear diffusive shock acceleration (NLDSA). Such theory is able to describe the acceleration itself, the dynamical reaction of accelerated particles on the shock, and the crucial phenomenon of the magnetic field amplification, the very key to generate high energy cosmic rays. I will illustrate the basic aspects of this theoretical framework, as well as its successes and problems. I will then discuss the observations, in X-rays an...

  11. The HARPS-N archive through a Cassandra, NoSQL database suite?

    Science.gov (United States)

    Molinari, Emilio; Guerra, Jose; Harutyunyan, Avet; Lodi, Marcello; Martin, Adrian

    2016-07-01

    The TNG-INAF is developing the science archive for the WEAVE instrument. The underlying architecture of the archive is based on a non relational database, more precisely, on Apache Cassandra cluster, which uses a NoSQL technology. In order to test and validate the use of this architecture, we created a local archive which we populated with all the HARPSN spectra collected at the TNG since the instrument's start of operations in mid-2012, as well as developed tools for the analysis of this data set. The HARPS-N data set is two orders of magnitude smaller than WEAVE, but we want to demonstrate the ability to walk through a complete data set and produce scientific output, as valuable as that produced by an ordinary pipeline, though without accessing directly the FITS files. The analytics is done by Apache Solr and Spark and on a relational PostgreSQL database. As an example, we produce observables like metallicity indexes for the targets in the archive and compare the results with the ones coming from the HARPS-N regular data reduction software. The aim of this experiment is to explore the viability of a high availability cluster and distributed NoSQL database as a platform for complex scientific analytics on a large data set, which will then be ported to the WEAVE Archive System (WAS) which we are developing for the WEAVE multi object, fiber spectrograph.

  12. AGILE Highlights after Six Years in Orbit

    Directory of Open Access Journals (Sweden)

    Carlotta Pittori

    2014-12-01

    Full Text Available AGILE is an ASI space mission in collaboration with INAF, INFN and CIFS, dedicated to the observation of the gamma-ray Universe in the 30 MeV - 50 GeV energy range, with simultaneous X-ray imaging capability in the 18-60 keV band. The AGILE satellite was launched on April 23rd, 2007, and produced several important scientic results, among which the unexpected discovery of strong ares from the Crab Nebula. This discovery won to the AGILE PI and the AGILE Team the Bruno Rossi Prize for 2012 by the High Energy Astrophysics division of the American Astronomical Society. Thanks to its sky monitoring capability and fast ground segment alert system, AGILE detected many Galactic and extragalactic sources: among other results AGILE discovered gamma-ray emission from the microquasar Cygnus X-3, detected many bright blazars, discovered several new gamma-ray pulsars, and discovered emission up to 100 MeV from Terrestrial Gamma-Ray Flashes. We present an overview of the main AGILE Data Center activities and the AGILE scientic highlights after 6 years of operations.

  13. Our world is everyone’s!

    CERN Multimedia

    2013-01-01

    At the end of this month, CERN will embark on its most ambitious open day weekend to date, stretching the definition of the weekend to embrace four days from Friday to Monday.   The first to benefit will be our industrial partners, who have a dedicated day to themselves on Friday to discover CERN’s amazing world of technology, and the opportunities that await companies joining us on our adventure to explore the Universe. This transitions nicely into the European Researchers Night, an EU initiative that CERN has participated in for several years. This year, we’re partnering with the Italian National Institute for Astrophysics (INAF), and teaming up with ESA, ESO, UNESCO and the Italian National Institute for Nuclear Physics (INFN) to present a multi-centred night of our Origins to celebrate the sciences of the infinitesimally small and the infinitely large. There will be webcast talks from a celestial range of speakers and opportunities for participants to speed-date a scien...

  14. The EXTraS project: Exploring the X-ray Transient and variable Sky

    Science.gov (United States)

    Kreikenbohm, A.; Oertel, M.; Wilms, J.; DeLuca, A.; Haberl, F.; Greiner, J.; Delvaux, C.; Carpano, S.; Law-Green, D.; Rosen, S.

    2015-07-01

    Modern X-ray observatories can yield unique insights into time domain astrophysics. Indeed, a huge amount of information is already stored - and largely unexploited - in data archives. The EXTraS project harvests the hitherto unexplored temporal domain information buried in the serendipitous data collected by the European Photon Imaging Camera (EPIC) instrument onboard the ESA XMM-Newton mission since its launch. This includes a search for fast transients, missed by standard image analysis, and a search and characterization of variability (both periodic and aperiodic) in hundreds of thousands of sources spanning more than nine orders of magnitude in time scale (from less than 1 s to 10 yr) and six orders of magnitude in flux (from 10(-9) to more than 10(-15) erg cm(-2) s(-1) in 0.2-12 keV). X-ray results are to be complemented by multiwavelength characterization of new discoveries. Phenomenological classification of variable sources will also be performed. Our final catalogue and results will be made available to the community, together with new analysis tools, at the end of the project (late 2016). EXTraS is funded within the EU/FP7-Cooperation Space framework and is carried out by a collaboration including INAF (Italy), IUSS (Italy), CNR/IMATI (Italy), University of Leicester (UK), MPE (Germany) and ECAP (Germany).

  15. Screening and validation of EXTraS data products

    Science.gov (United States)

    Carpano, Stefania; Haberl, F.; De Luca, A.; Tiengo, A.: Israel, G.; Rodriguez, G.; Belfiore, A.; Rosen, S.; Read, A.; Wilms, J.; Kreikenbohm, A.; Law-Green, D.

    2015-09-01

    The EXTraS project (Exploring the X-ray Transient and variable Sky) is aimed at fullyexploring the serendipitous content of the XMM-Newton EPIC database in the timedomain. The project is funded within the EU/FP7-Cooperation Space framework and is carried out by a collaboration including INAF (Italy), IUSS (Italy), CNR/IMATI (Italy), University of Leicester (UK), MPE (Germany) and ECAP (Germany). The several tasks consist in characterise aperiodicvariability for all 3XMM sources, search for short-term periodic variability on hundreds of thousands sources, detect new transient sources that are missed by standard source detection and hence not belonging to the 3XMM catalogue, search for long term variability by measuring fluxes or upper limits for both pointed and slew observations, and finally perform multiwavelength characterisation andclassification. Screening and validation of the different products is essentially in order to reject flawed results, generated by the automatic pipelines. We present here the screening tool we developed in the form of a Graphical User Interface and our plans for a systematic screening of the different catalogues.

  16. The spectral imaging facility: Setup characterization

    Energy Technology Data Exchange (ETDEWEB)

    De Angelis, Simone, E-mail: simone.deangelis@iaps.inaf.it; De Sanctis, Maria Cristina; Manzari, Paola Olga [Institute for Space Astrophysics and Planetology, INAF-IAPS, Via Fosso del Cavaliere, 100, 00133 Rome (Italy); Ammannito, Eleonora [Institute for Space Astrophysics and Planetology, INAF-IAPS, Via Fosso del Cavaliere, 100, 00133 Rome (Italy); Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, Los Angeles, California 90095-1567 (United States); Di Iorio, Tatiana [ENEA, UTMEA-TER, Rome (Italy); Liberati, Fabrizio [Opto Service SrL, Campagnano di Roma (RM) (Italy); Tarchi, Fabio; Dami, Michele; Olivieri, Monica; Pompei, Carlo [Selex ES, Campi Bisenzio (Italy); Mugnuolo, Raffaele [Italian Space Agency, ASI, Spatial Geodesy Center, Matera (Italy)

    2015-09-15

    The SPectral IMager (SPIM) facility is a laboratory visible infrared spectrometer developed to support space borne observations of rocky bodies of the solar system. Currently, this laboratory setup is used to support the DAWN mission, which is in its journey towards the asteroid 1-Ceres, and to support the 2018 Exo-Mars mission in the spectral investigation of the Martian subsurface. The main part of this setup is an imaging spectrometer that is a spare of the DAWN visible infrared spectrometer. The spectrometer has been assembled and calibrated at Selex ES and then installed in the facility developed at the INAF-IAPS laboratory in Rome. The goal of SPIM is to collect data to build spectral libraries for the interpretation of the space borne and in situ hyperspectral measurements of planetary materials. Given its very high spatial resolution combined with the imaging capability, this instrument can also help in the detailed study of minerals and rocks. In this paper, the instrument setup is first described, and then a series of test measurements, aimed to the characterization of the main subsystems, are reported. In particular, laboratory tests have been performed concerning (i) the radiation sources, (ii) the reference targets, and (iii) linearity of detector response; the instrumental imaging artifacts have also been investigated.

  17. EXTraS: Exploring the X-ray Transient and variable Sky

    Science.gov (United States)

    De Luca, A.; Salvaterra, R.; Tiengo, A.; D'Agostino, D.; Watson, M.; Haberl, F.; Wilms, J.

    2017-10-01

    The EXTraS project extracted all temporal domain information buried in the whole database collected by the EPIC cameras onboard the XMM-Newton mission. This included a search and characterisation of variability, both periodic and aperiodic, in hundreds of thousands of sources spanning more than eight orders of magnitude in time scale and six orders of magnitude in flux, as well as a search for fast transients, missed by standard image analysis. Phenomenological classification of variable sources, based on X-ray and multiwavelength information, has also been performed. All results and products of EXTraS are made available to the scientific community through a web public data archive. A dedicated science gateway will allow scientists to apply EXTraS pipelines on new observations. EXTraS is the most comprehensive analysis of variability, on the largest ever sample of soft X-ray sources. The resulting archive and tools disclose an enormous scientific discovery space to the community, with applications ranging from the search for rare events to population studies, with impact on the study of virtually all astrophysical source classes. EXTraS, funded within the EU/FP7 framework, is carried out by a collaboration including INAF (Italy), IUSS (Italy), CNR/IMATI (Italy), University of Leicester (UK), MPE (Germany) and ECAP (Germany).

  18. 27 September 2013: Fast forward and rewind to our Origins

    CERN Multimedia

    Antonella Del Rosso

    2013-01-01

    Origins is the EU co-funded project that will celebrate the 2013 Researchers Night on 27 September. For the first time, a webcast produced at CERN, UNESCO in Paris and the National Institute for Astrophysics (INAF) in Bologna, Italy will bring cosmologists and particle physicists to the stage. They will take us on a journey both back to the origins of our Universe and forward to the future scientific achievements that we expect to unveil its mysteries.   “The two infinities have never been so close” reads the motto of Origins, the international project led by the CERN Communication Group and selected by the European Union to receive funds under the seventh Framework Programme. “With the discovery of the Higgs boson at CERN in 2012 and the results on the Cosmic Microwave Background radiation recently published by the Planck collaboration, researchers have made progress towards solving some of the most profound mysteries of the Universe we live in. With Origins we wa...

  19. The software upgrade of NICS

    Science.gov (United States)

    Rossetti, Emanuel; Guido, Vincenzo; Oliva, Ernesto

    2008-08-01

    NICS (the Near Infrared Camera Spectrometer) is a cooled near-infrared camera-spectrometer that has been developed in the late 90's at the INAF-Arcetri Astrophysical Observatory for the Ø3.5 m "Telescopio Nazionale Galileo" (TNG) at the La Palma Observatory. The instrument has been operating for regular scientific observations since the beginning of 2001. During the 2001-2007 period it has been used in about 410 nights yielding data which contributed to the production of 60 refereed papers which collected a total of more than 800 citations. At the age of 8 years, NICS is still among the most efficient and versatile infrared instruments existing worldwide. To improve its observational efficiency, we have designed and we are currently developing new control software and GUI interfaces. The former has been devised to optimize the low level tasks (in particular the motors controls), the latter to simplify the communications between the observer and the instrument. We give here a short description of NICS software upgrade.

  20. Planets in a Room

    Science.gov (United States)

    Giacomini, l.; Aloisi, F.; De Angelis, I.

    2017-09-01

    Teaching planetary science using a spherical projector to show the planets' surfaces is a very effective but usually very expensive idea. Whatsmore, it usually assumes the availability of a dedicated space and a trained user. "Planets in a room" is a prototypal low cost version of a small, spherical projector that teachers, museum, planetary scientists and other individuals can easily build and use on their own, to show and teach the planets The project of "Planets in a Room" was made by the italian non-profit association Speak Science with the collaboration of INAF-IAPS of Rome and the Roma Tre University (Dipartimento di Matematica e Fisica). This proposal was funded by the Europlanet Outreach Funding Scheme in 2016. "Planets in a room" will be presented during EPSC 2017 to give birth to the second phase of the project, when the outreach and research community will be involved and schools from all over Europe will be invited to participate with the aim of bringing planetary science to a larger audience.

  1. The Imaging X-Ray Polarimetry Explorer (IXPE): Overview

    Science.gov (United States)

    O'Dell, Steve; Weisskopf, M.; Soffitta, P.; Baldini, L.; Bellazzini, R.; Costa, E.; Elsner, R.; Kaspi, V.; Kolodziejczak, J.; Latronico, L.; hide

    2017-01-01

    Mission background: Imaging x-ray polarimetry in 2–8 kiloelectronvolt band; NASA Astrophysics Small Explorer (SMEX) selected in 2017 January. Orbit: Pegasus-XL (airborne) launch in 2021, from Kwajalein; Equatorial circular orbit at greater than or approximately equal to 540 kilometers (620 kilometers, goal) altitude. Flight system: Spacecraft, payload structure, and integration by Ball Aerospace - Deployable payload boom from Orbital-ATK, under contract to Ball; X-ray Mirror Module Assemblies by NASA/MSFC; X-ray (polarization-sensitive) Instruments by IAPS/INAF (Istituto di Astrofisica e Planetologia Spaziali / Istituto Nazionale di Astrofisica) and INFN (Istituto Nazionale di Fisica Nucleare). Ground system: ASI (Agenzia Spaziale Italiana) Malindi ground station, with Singapore backup; Mission Operations Center at LASP (Laboratory for Atmospheric and Space Physics, University of Colorado); Science Operations Center at NASA/MSFC; Data archive at HEASARC (High Energy Astrophysics Science Archive Research Center), (NASA/GSFC), mirror at ASI Data Center. Science: Active galactic nuclei; Microquasars; Radio pulsars and pulsar wind nebulae; Supernova remnants; Magnetars; Accreting x-ray pulsars.

  2. EVALSO: enabling virtual access to Latin American southern observatories

    Science.gov (United States)

    Cirami, R.; Coretti, I.; Di Marcantonio, P.; Pucillo, M.; Santin, P.

    2008-08-01

    In the field of observational astrophysics, the remoteness of the facilities and the ever increasing data volumes and detectors poses new technological challenges. As an example, the VISTA and VST wide field telescopes, which are being constructed at the ESO's Cerro Paranal Observatory and will be ready in the next few years, have cameras which will produce after just one year of operation a volume of data that will exceed all the data collected by the VLT since the start of operations in 1999. This sets serious limitations if such large quantities of data must be transferred and accessed in a short time by the participating European Institutions. The EVALSO project, approved by the European Community, addresses these targets in two major ways. It will create a physical infrastructure to efficiently connect these facilities to Europe. This infrastructure will be complementary to the international infrastructure already created in the last years with the EC support (RedCLARA, ALICE, GEANT). Besides this, it will provide the astronomers with Virtual Presence (VP), i.e. the tools to perform and control an astronomical observation from the user's site. The main role of INAF - Astronomical Observatory of Trieste (OAT) within the project will be the definition of the architecture, the development of VP system and the integration of a prototype to be used as a demonstrator. This paper will focus on the description of the Virtual Presence system.

  3. VizieR Online Data Catalog: Lupus YSOs X-shooter spectroscopy (Alcala+, 2017)

    Science.gov (United States)

    Alcala, J. M.; Manara, C. F.; Natta, A.; Frasca, A.; Testi, L.; Nisini, B.; Stelzer, B.; Williams, J. P.; Antoniucci, S.; Biazzo, K.; Covino, E.; Esposito, M.; Getman, F.; Rigliaco, E.

    2017-07-01

    All the data used in this paper were acquired with the X-shooter spectrograph at the VLT. The capabilities of X-shooter in terms of wide spectral coverage (310-2500nm), resolution and limiting magnitudes allow us to assess simultaneously the mass accretion and outflow, and disc diagnostics, from the UV and optical to the near IR. The sample studied in this paper consists mainly of two sets of low-mass class II YSOs in the aforementioned Lupus clouds. The first one comprises the 36 objects published in Alcala et al, (2014, Cat. J/A+A/561/A2), observed within the context of the X-shooter INAF/GTO (Alcala et al. 2011AN....332..242A) project; for simplicity we will refer to it as the "GTO sample" throughout the paper. One additional source namely Sz105, was investigated with X-shooter during the GTO, but rejected as a legitimate YSO (see below). The second sample consists of 49 objects observed during ESO periods 95 and 97 (1 April-30 September 2015 and 1 April-30 September 2016, respectively). In addition, we include here six objects observed with X-shooter in other programmes taken from the ESO archive. In total, 55 objects were newly analysed here and we will refer to them as the "new sample". (12 data files).

  4. Integrating the IA2 Astronomical Archive in the VO: The VO-Dance Engine

    Science.gov (United States)

    Molinaro, M.; Laurino, O.; Smareglia, R.

    2012-09-01

    Virtual Observatory (VO) protocols and standards are getting mature and the astronomical community asks for astrophysical data to be easily reachable. This means data centers have to intensify their efforts to provide the data they manage not only through proprietary portals and services but also through interoperable resources developed on the basis of the IVOA (International Virtual Observatory Alliance) recommendations. Here we present the work and ideas developed at the IA2 (Italian Astronomical Archive) data center hosted by the INAF-OATs (Italian Institute for Astrophysics - Trieste Astronomical Observatory) to reach this goal. The core point is the development of an application that from existing DB and archive structures can translate their content to VO compliant resources: VO-Dance (written in Java). This application, in turn, relies on a database (potentially DBMS independent) to store the translation layer information of each resource and auxiliary content (UCDs, field names, authorizations, policies, etc.). The last token is an administrative interface (currently developed using the Django python framework) to allow the data center administrators to set up and maintain resources. This deployment, platform independent, with database and administrative interface highly customizable, means the package, when stable and easily distributable, can be also used by single astronomers or groups to set up their own resources from their public datasets.

  5. AGILE DATA CENTER AT ASDC AND AGILE HIGHLIGHTS

    Directory of Open Access Journals (Sweden)

    Carlotta Pittori

    2013-12-01

    Full Text Available We present an overview of the main AGILE Data Center activities and the AGILE scientific highlights during the first 5 years of operations. AGILE is an ASI space mission in joint collaboration with INAF, INFN and CIFS, dedicated to the observation of the gamma-ray Universe. The AGILE satellite was launched on April 23rd, 2007, and is devoted to gamma-ray astrophysics in the 30MeV ÷ 50 GeV energy range, with simultaneous X-ray imaging capability in the 18 ÷ 60 keV band. Despite the small size and budget, AGILE has produced several important scientific results, including the unexpected discovery of strong and rapid gamma-ray flares from the Crab Nebula over daily timescales. This discovery won AGILE PI and the AGILE Team the prestigious Bruno Rossi Prize for 2012, an international award in the field of high energy astrophysics. Thanks to its sky monitoring capability and fast ground segment alert system, AGILE is substantially improving our knowledge of the gamma-ray sky, also making a crucial contribution to the study of the terrestrial gamma-ray flashes (TGFs detected in the Earth atmosphere. The AGILE Data Center, part of the ASI Science Data Center (ASDC located in Frascati, Italy, is in charge of all the science oriented activities related to the analysis, archiving and distribution of AGILE data.

  6. Comparison of different risk stratification systems in predicting short-term serious outcome of syncope patients

    Directory of Open Access Journals (Sweden)

    Saeed Safari

    2016-01-01

    Full Text Available Background: Determining etiologic causes and prognosis can significantly improve management of syncope patients. The present study aimed to compare the values of San Francisco, Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL, Boston, and Risk Stratification of Syncope in the Emergency Department (ROSE score clinical decision rules in predicting the short-term serious outcome of syncope patients. Materials and Methods: The present diagnostic accuracy study with 1-week follow-up was designed to evaluate the predictive values of the four mentioned clinical decision rules. Screening performance characteristics of each model in predicting mortality, myocardial infarction (MI, and cerebrovascular accidents (CVAs were calculated and compared. To evaluate the value of each aforementioned model in predicting the outcome, sensitivity, specificity, positive likelihood ratio, and negative likelihood ratio were calculated and receiver-operating curve (ROC curve analysis was done. Results: A total of 187 patients (mean age: 64.2 ΁ 17.2 years were enrolled in the study. Mortality, MI, and CVA were seen in 19 (10.2%, 12 (6.4%, and 36 (19.2% patients, respectively. Area under the ROC curve for OESIL, San Francisco, Boston, and ROSE models in prediction the risk of 1-week mortality, MI, and CVA was in the 30-70% range, with no significant difference among models (P > 0.05. The pooled model did not show higher accuracy in prediction of mortality, MI, and CVA compared to others (P > 0.05. Conclusion: This study revealed the weakness of all four evaluated models in predicting short-term serious outcome of syncope patients referred to the emergency department without any significant advantage for one among others.

  7. Comparison of different risk stratification systems in predicting short-term serious outcome of syncope patients.

    Science.gov (United States)

    Safari, Saeed; Baratloo, Alireza; Hashemi, Behrooz; Rahmati, Farhad; Forouzanfar, Mohammad Mehdi; Motamedi, Maryam; Mirmohseni, Ladan

    2016-01-01

    Determining etiologic causes and prognosis can significantly improve management of syncope patients. The present study aimed to compare the values of San Francisco, Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL), Boston, and Risk Stratification of Syncope in the Emergency Department (ROSE) score clinical decision rules in predicting the short-term serious outcome of syncope patients. The present diagnostic accuracy study with 1-week follow-up was designed to evaluate the predictive values of the four mentioned clinical decision rules. Screening performance characteristics of each model in predicting mortality, myocardial infarction (MI), and cerebrovascular accidents (CVAs) were calculated and compared. To evaluate the value of each aforementioned model in predicting the outcome, sensitivity, specificity, positive likelihood ratio, and negative likelihood ratio were calculated and receiver-operating curve (ROC) curve analysis was done. A total of 187 patients (mean age: 64.2 ± 17.2 years) were enrolled in the study. Mortality, MI, and CVA were seen in 19 (10.2%), 12 (6.4%), and 36 (19.2%) patients, respectively. Area under the ROC curve for OESIL, San Francisco, Boston, and ROSE models in prediction the risk of 1-week mortality, MI, and CVA was in the 30-70% range, with no significant difference among models ( P > 0.05). The pooled model did not show higher accuracy in prediction of mortality, MI, and CVA compared to others ( P > 0.05). This study revealed the weakness of all four evaluated models in predicting short-term serious outcome of syncope patients referred to the emergency department without any significant advantage for one among others.

  8. Syncope risk stratification tools vs clinical judgment: an individual patient data meta-analysis.

    Science.gov (United States)

    Costantino, Giorgio; Casazza, Giovanni; Reed, Matthew; Bossi, Ilaria; Sun, Benjamin; Del Rosso, Attilio; Ungar, Andrea; Grossman, Shamai; D'Ascenzo, Fabrizio; Quinn, James; McDermott, Daniel; Sheldon, Robert; Furlan, Raffaello

    2014-11-01

    There have been several attempts to derive syncope prediction tools to guide clinician decision-making. However, they have not been largely adopted, possibly because of their lack of sensitivity and specificity. We sought to externally validate the existing tools and to compare them with clinical judgment, using an individual patient data meta-analysis approach. Electronic databases, bibliographies, and experts in the field were screened to find all prospective studies enrolling consecutive subjects presenting with syncope to the emergency department. Prediction tools and clinical judgment were applied to all patients in each dataset. Serious outcomes and death were considered separately during emergency department stay and at 10 and 30 days after presenting syncope. Pooled sensitivities, specificities, likelihood ratios, and diagnostic odds ratios, with 95% confidence intervals, were calculated. Thirteen potentially relevant papers were retrieved (11 authors). Six authors agreed to share individual patient data. In total, 3681 patients were included. Three prediction tools (Osservatorio Epidemiologico sulla Sincope del Lazio [OESIL], San Francisco Syncope Rule [SFSR], Evaluation of Guidelines in Syncope Study [EGSYS]) could be assessed by the available datasets. None of the evaluated prediction tools performed better than clinical judgment in identifying serious outcomes during emergency department stay, and at 10 and 30 days after syncope. Despite the use of an individual patient data approach to reduce heterogeneity among studies, a large variability was still present. Current prediction tools did not show better sensitivity, specificity, or prognostic yield compared with clinical judgment in predicting short-term serious outcome after syncope. Our systematic review strengthens the evidence that current prediction tools should not be strictly used in clinical practice. Copyright © 2014 Elsevier Inc. All rights reserved.

  9. Relative utility of serum troponin and the OESIL score in syncope.

    Science.gov (United States)

    Hing, Rosslyn; Harris, Roger

    2005-02-01

    To investigate the utility of both a random troponin T level taken greater than 4 h after a syncopal event and the Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) score in predicting outcome post syncope. We prospectively enrolled 113 adult patients who presented to our ED after a syncopal event. Each patient had a troponin T level taken at least 4 h after the event. The relevant history of the syncope, background medical history and ECG were collected at presentation. Patients were followed up via telephone after 3-6 months and medical records were also examined. The OESIL risk score was calculated for each patient and the predictive value of both the troponin T and OESIL score were analysed for their utility post syncope. Data were analysed for 100 patients. Twenty percent were believed to have a cardiac cause for their syncope. An elevated troponin T level was found to be highly specific (0.99, 95% confidence interval [CI] 0.96-1.0) for adverse cardiac outcome, but with a very low sensitivity (0.13, 95% CI 0-0.3). The OESIL risk score was found to be predictive of an adverse cardiac outcome (receiver-operating characteristic [ROC] 0.73, 95% CI 0.63-0.84) and return to normal function (ROC 0.74, 95% CI 0.63-0.86). A normal serum troponin T has a poor negative predictive value for adverse cardiac outcomes following syncope. A simple risk stratification system, such as the OESIL score, can predict those patients most at risk after a syncopal episode.

  10. Development and prospective validation of a risk stratification system for patients with syncope in the emergency department: the OESIL risk score.

    Science.gov (United States)

    Colivicchi, Furio; Ammirati, Fabrizio; Melina, Domenico; Guido, Vincenzo; Imperoli, Giuseppe; Santini, Massimo

    2003-05-01

    Aim of the present study was the development and the subsequent validation of a simple risk classification system for patients presenting with syncope to the emergency departments. A group of 270 consecutive patients (145 females, mean age 59.5 years) presenting with syncope to the emergency departments of six community hospitals of the Lazio region of Italy was used as a derivation cohort for the development of the risk classification system. Data from the baseline clinical history, physical examination and electrocardiogram were used to identify independent predictors of total mortality within the first 12 months after the initial evaluation. Multivariate analysis allowed the recognition of the following predictors of mortality: (1) age >65 years; (2) cardiovascular disease in clinical history; (3) syncope without prodromes; and (4) abnormal electrocardiogram. The OESIL (Osservatorio Epidemiologico sulla Sincope nel Lazio) score was calculated by the simple arithmetic sum of the number of predictors present in every single patient. Mortality increased significantly as the score increased in the derivation cohort (0% for a score of 0, 0.8% for 1 point; 19.6% for 2 points; 34.7% for 3 points; 57.1% for 4 points; p<0,0001 for trend). A similar pattern of increasing mortality with increasing score was prospectively confirmed in a second validation cohort of 328 consecutive patients (178 females; mean age, 57.5 years). Clinical and electrocardiographic data available at presentation to the emergency department can be used for the risk stratification of patients with syncope. The OESIL risk score may represent a simple prognostication tool that could be usefully employed for the triage and management of patients with syncope in emergency departments.

  11. Accuracy and quality of clinical decision rules for syncope in the emergency department: a systematic review and meta-analysis.

    Science.gov (United States)

    Serrano, Luis A; Hess, Erik P; Bellolio, M Fernanda; Murad, Mohammed H; Montori, Victor M; Erwin, Patricia J; Decker, Wyatt W

    2010-10-01

    We assess the methodological quality and prognostic accuracy of clinical decision rules in emergency department (ED) syncope patients. We searched 6 electronic databases, reviewed reference lists of included studies, and contacted content experts to identify articles for review. Studies that derived or validated clinical decision rules in ED syncope patients were included. Two reviewers independently screened records for relevance, selected studies for inclusion, assessed study quality, and abstracted data. Random-effects meta-analysis was used to pool diagnostic performance estimates across studies that derived or validated the same clinical decision rule. Between-study heterogeneity was assessed with the I(2) statistic, and subgroup hypotheses were tested with a test of interaction. We identified 18 eligible studies. Deficiencies in outcome (blinding) and interrater reliability assessment were the most common methodological weaknesses. Meta-analysis of the San Francisco Syncope Rule (sensitivity 86% [95% confidence interval {CI} 83% to 89%]; specificity 49% [95% CI 48% to 51%]) and the Osservatorio Epidemiologico sulla Sincope nel Lazio risk score (sensitivity 95% [95% CI 88% to 98%]; specificity 31% [95% CI 29% to 34%]). Subgroup analysis identified study design (prospective, diagnostic odds ratio 8.82 [95% CI 3.5 to 22] versus retrospective, diagnostic odds ratio 2.45 [95% CI 0.96 to 6.21]) and ECG determination (by evaluating physician, diagnostic odds ratio 25.5 [95% CI 4.41 to 148] versus researcher or cardiologist, diagnostic odds ratio 4 [95% CI 2.15 to 7.55]) as potential explanations for the variability in San Francisco Syncope Rule performance. The methodological quality and prognostic accuracy of clinical decision rules for syncope are limited. Differences in study design and ECG interpretation may account for the variable prognostic performance of the San Francisco Syncope Rule when validated in different practice settings. Copyright © 2010 American

  12. On the Structure of the Solar Photosphere

    Directory of Open Access Journals (Sweden)

    Secchi A.

    2011-07-01

    Full Text Available Mary Posani (Department of French and Italian, The Ohio State University, Colum- bus, Ohio, 43221 and Eileen Reeves (Department of Comparative Literature, Prince- ton University, Princeton, New Jersey, 08544 provide a translation of Father Pietro Angelo Secchi’s classic work “ Sulla Struttura della Fotosfera Solare ” as it appeared in Bullettino Meteorologico dell’ Osservatorio del Collegio Romano , 30 November 1864, v.3(11, 1–3. Secchi’s paper was immediately translated into French by l’Abb ́ e Franc ̧ois Moigno appearing on December 22nd, 1864 ( Sur la structure de la photosph`ere du soleil. Les Mondes , 1864, v.6, 703–707. Moigno’s translation prompted significant interest in the nature of the Sun throughout Europe, with rapid claims of simultaneous discovery by Harv ́ e Faye (Faye H. Sur la constitution physique du soleil — premiere parti . Les Mondes, v.7, 293–306 and others. In this article, Secchi reiterated that the photosphere was composed of solid corpuscles floating on the transparent atmosphere of the Sun. Secchi concluded that the body of the Sun was gaseous based on his vi- sualization of solar granules or “ willow leaves ” described by Nasmyth (Nasmyth J. On the Structure of the Luminous Envelope of the Sun — In a letter to Joseph Sidebotham . Memoirs of the Literary and Philosophical Society of Manchester , 1862, 3rd Series, v.I, 407–411. Secchi also referred to Magnus’ work on solid particles in the gaseous flame (Magnus G. Notiz ̈uber die Bescha enheit der Sonne. Poggendorff’s Annalen der Physik und Chemie , 1864, v.121, 510–512; also in French Notice sur la constitution du soleil . Archives des science physique et naturelles (Gen`eve , 1864, v.20, 171–175. The works by Sechhi, Nasmyth, Magnus, and Faye would dominate astrophysical thought for the next 50 years.

  13. 12th European VLBI Network Symposium and Users Meeting

    Science.gov (United States)

    Tarchi, Andrea; Giroletti, Marcello; Feretti, Luigina

    The Istituto di Radioastronomia (IRA) di Bologna and the Osservatorio Astronomico di Cagliari (OAC), on behalf of the European VLBI Consortium, hosted the 12th European VLBI Network (EVN) Symposium and Users Meeting. The Conference was held from 7th to 10th of October at the Hotel Regina Margherita, in the center of Cagliari. The latest scientific results and technical developments from VLBI, and, in particular, e-VLBI and space-VLBI (RadioAstron) outcomes were reported. The timing of this meeting coincided with the first successful observational tests of the Sardinia Radio Telescopes within the EVN, and with a number of results from new and upgraded radio facilities around the globe, such as e-MERLIN, ALMA, and the SKA pathfinders. The symposium was attended by 133 participants from all over the world, with the Asian community represented by more than 20 colleagues. The program of the meeting consisted of 70 oral contributions (including 8 invited speakers) and 50 poster that covered a very wide range of VLBI topics both in galactic and extragalactic astrophysics (e.g., AGN, stellar evolution from birth to death, astrometry, and planetary science) as well as technological developments and future international collaborations. The scientific program also included a visit to the 64-m Sardinia Radio Telescope (SRT) and the EVN Users Meeting, where astronomers have provided useful feedback on various matters regarding EVN operations. The research leading to these results has received funding from the European Commission Seventh Framework Programme (FP/2007-2013) under grant agreement No 283393 (RadioNet3). EDITORIAL BOARD: Andrea Tarchi, Marcello Giroletti, Luigina Feretti

  14. XMM-Newton survey of the low-metallicity open cluster NGC 2516

    Science.gov (United States)

    Sciortino, S.; Micela, G.; Damiani, F.; Flaccomio, E.; Briggs, K.; Denby, M.; Pye, J.; Grosso, N.; Read, A. M.; Gondoin, P.; Jeffries, R. D.

    2001-01-01

    We present the first results of an XMM-Newton EPIC survey of NGC 2516, a southern low-metallicity open cluster with an age close to the Pleiades. The attained limiting sensitivity is of ~ 2.4 10-15 erg s-1 cm-2 in the 0.1-4.0 keV bandpass. This has been achieved by summing the data of the MOS and PN cameras of two distinct observations for a total exposure time of ~ 33 ks and by analyzing the summed data set with the wavelet detection algorithm developed at Osservatorio Astronomico di Palermo (OAPA) that has yielded over 200 X-ray detections. Using data just from a single exposure or from a single camera would have reduced by a factor 2-4 our limiting sensitivity and would have resulted in 25-40% less X-ray detections. To date, 129 detections have as counterparts one or more of the 540 photometrically selected cluster members in the surveyed region, for a total of 147 likely detected members, with unique identification in 112 cases. We derive the X-ray luminosity functions (XLF) of NGC 2516 members of different spectral types and compare them with those of the more metal rich, approximately coeval Pleiades cluster, finding the NGC 2516 photometrically selected dG and dK stars less luminous than the Pleiades. The XLFs of the NGC 2516 and of the Pleiades dM stars are indistinguishable. We compare the XMM-Newton results with those recently obtained with Chandra.

  15. PROLOGUE

    Directory of Open Access Journals (Sweden)

    José Morales

    2016-09-01

    Full Text Available In 1989 the first bases of what is now a strong and consolidated Spanish-Italian scientific relationship in Seismology and in Volcano-Seismology were established. The first stage took place at the University of Catania, in the former Department of Earth Sciences, placed in the old Science Faculty, when a pre-doctoral student from the University of Granada, Cartuja Observatory (now called Andalusian Institute of Geophysics, arrived to complete his formation in seismology. During this stage, in addition to the training process, new contacts with researchers and mainly with pre-doctoral students of the former International Institute of Volcanology of the Italian National Research Council (IIV-CNR were stablished. These contacts have endured, grown and created a strong international scientific network with consolidated and credible research production. In a short time new working groups were integrated such as the Osservatorio Vesuviano in Naples or the Department of Physics of the University of Salerno from the Italian side, and the Department of Applied Physics of the University of Almería or the Volcanology Department of the Spanish Research Council (CSIC in Spain. At the present this non-official (but very active network comprises many Italian Research Centers belonging to the National Institute of Geophysics and Volcanology (INGV such as Catania, Naples, Rome, Palermo, Pisa or Bologna; Italian Universities as Salerno, Naples, L’Aquila or Calabrian, several Spanish Universities such as Granada, Almería, Jaen, Complutense, Cádiz or La Laguna, but also from other countries such as USA, Russia, Ireland, Portugal, México, Argentina, Germany, France, Norway or UK among others. This collaboration includes a continuous pre-doctoral students training protocols in which the exchange of fellows among the different institutions is fluent. [...

  16. Eruptive pattern classification on Mount Etna (Sicily) and Piton de la Fournaise (La Réunion)

    Science.gov (United States)

    Falsaperla, Susanna; Langer, Horst; Ferrazzini, Valérie

    2016-04-01

    In the framework of the European MEDiterrranean Supersite Volcanoes (MED­SUV) project, Mt. Etna (Italy) and Piton de la Fournaise (La Réunion) were chosen as "European Supersite Demonstrator" and test site, respectively, to promote the transfer and implementation of efficient tools for the identification of impending volcanic activity. Both are "open-conduit volcanoes", forming ideal sites for the test and validation of innovative concepts, which can contribute to minimize volcanic hazard. One of the aims of the MED-SUV project was the development of software for machine learning applicable to data processing for early-warning purposes. Near-real time classification of continuous seismic data stream has been carried out in the control room of INGV Osservatorio Etneo since 2010. Subsequently, automatic alert procedures were activated. In the light of the excellent results for the 24/7 surveillance of Etna, we examine the portability of tools developed in the framework of the project when applied to seismic data recorded at Piton de la Fournaise. In the present application to data recorded at Piton de la Fournaise, the classifier aims at highlighting changes in the frequency content of the background seismic signal heralding the activation of the volcanic source and the imminent eruption. We describe the preliminary results of this test on a set of data of nearly two years starting on January 2014. This period follows three years of inactivity and deflation of the volcano and marks a renewal of the volcano activity with inflation, deep seismicity (-7km bsl) and five eruptions with fountains and lava flows that lasted from a few hours to more than two months. We discuss here the necessary tuning for the implementation of the software to the new dataset analyzed. We also propose a comparison with the results of pattern classification regarding recent eruptive activity at Etna.

  17. Science Fiction In Naples In The Middle Of The 19th Century

    Science.gov (United States)

    Capaccioli, Massimo; Cirella, Emilia Olostro; Stendardo, Enrica; Virgilio, Nicla

    Astronomer, intellectual, passionate patriot, and refined humanist, Ernesto Capocci Belmonte (Picinisco, May 31, 1798 - Naples, January 6, 1864) was a prominent figure of the scientific, cultural, and political life in Naples around the middle of the 19th century. He acquired international recognition for his studies on the orbits of comets and, since 1833, he was named director of the newly built Osservatorio Astronomico in Capodimonte: A prestigious position that he lost for political retaliation as a result of his participation in the movement against the Bourbon rulers in 1848, but which he regained in 1860 upon the arrival in Naples of Giuseppe Garibaldi. An intuitive and open-minded scholar, he looked always at the contemporary experiences in Europe and, as a scientist and cultivated human being, he sought to serve the community by enthusiastically devoting himself also to education and public outreach. He developed clear interests in literature and, as a forerunner, he dared to tackle the genre of science fiction. His short novel Relazione del viaggio alla Luna fatto da una donna nell'anno di grazia 2057 (Report of the Trip to the Moon done by a Woman in the Year of our Lord 2057), written in the period of his exile from the Observatory and practically given up as lost until a private copy was found in the library of one of Capocci's descendants, offers an interesting overview of astronomical knowledge and taste for the elegance in writing, and gives an unusual, and often ironic, viewpoint on the situation of sciences in Naples in the middle of the 19th century.

  18. Broad band seismology in the Scotia region. The base Esperanza seismological observatory

    International Nuclear Information System (INIS)

    Russi, M.; Costa, G.; Febrer, J.

    1995-08-01

    The lithospheric study and the identification of relevant lateral heterogeneities in the Antarctic continent and borderlands, is essential to understand the geodynamic evolution both of the continental and oceanic bordering regions. The complexity of the geological evolution and the structural properties of the lithosphere in the Scotia area have been stressed by many authors. The present setting of the area is the result of the mutual interaction among the Antarctic, South American and several minor plants whose geodynamic history and actual boundaries are still partially unknown. The intense seismic activity that characterizes the region encourages the use of the seismological approach to investigate the lithospheric structure of the area. Since January 1992 a broad band three components station is operating at the Antarctic base Esperanza in the NE area of Antarctic Peninsula. The station has been installed with financial support of the Italian Programma Nazionale di Ricerche in Antartide (PNRA) by Osservatorio Geofisico Sperimentale (OGS) and Instituto Antartico Argentino (IAA). Russi et al. (1994) have analyzed selected recordings using the frequency-time analysis (FTAN) method obtaining some relevant information on the large scale structure of the lithosphere in the Scotia region even if data recorded by a single station were available. The extension of our analysis to further events and to horizontal component records is here presented. Within the framework of the international co-operation to the Antarctic Seismographic Network, the OGS and the IAA are upgrading the Esperanza station and installing an additional broad band station near the town of Ushuaia (Tierra del Fuego, Argentina) with the financial support of PNRA. The inversion of the dispersion curves through the FTAN of the signals recorded by an increased number of stations and generated by events with source-station paths spanning the region will allow us to extract the elastic and anelastic

  19. Comet 67P: Thermal Maps and Local Properties as Derived from Rosetta/VIRTIS data

    Science.gov (United States)

    Tosi, Federico; Capria, Maria Teresa; Capaccioni, Fabrizio; Filacchione, Gianrico; Erard, Stéphane; Leyrat, Cédric; Bockelée-Morvan, Dominique; De Sanctis, Maria Cristina; Raponi, Andrea; Ciarniello, Mauro; Schmitt, Bernard; Arnold, Gabriele; Mottola, Stefano; Fonti, Sergio; Palomba, Ernesto; Longobardo, Andrea; Cerroni, Priscilla; Piccioni, Giuseppe; Drossart, Pierre; Kuehrt, Ekkehard

    2015-04-01

    the compositional investigation based on imaging spectroscopy data collected at shorter wavelengths. In the VIRTIS thermal images, a note of great interest is provided by the 'neck' of the comet close to the 'body', where, because of the concave shape, the 'head' casts prominent shadows on some areas when they experience maximum daily insolation. This is a place potentially subjected to considerable thermal stresses. We evaluate both the spatial thermal gradients and the temporal thermal gradients, providing implications for the surface structure. Acknowledgements: The authors would like to thank the following institutions and agencies, which supported this work: Italian Space Agency (ASI - Italy), Centre National d'Etudes Spatiales (CNES- France), Deutsches Zentrum für Luft- und Raumfahrt (DLR-Germany), National Aeronautic and Space Administration (NASA-USA) Rosetta Program, Science and Technology Facilities Council (UK). VIRTIS has been built by a consortium, which includes Italy, France and Germany, under the scientific responsibility of the Istituto di Astrofisica e Planetologia Spaziali of INAF, Italy, which guides also the scientific operations. The VIRTIS instrument development has been funded and managed by ASI, with contributions from Observatoire de Meudon financed by CNES, and from DLR. The computational resources used in this research have been supplied by INAF-IAPS through the DataWell project.

  20. Mulheres, homens e matemática: uma leitura a partir dos dados do Indicador Nacional de Alfabetismo Funcional Women, men, and mathematics: a reading of data from the National Index of Functional Literacy

    Directory of Open Access Journals (Sweden)

    Maria Celeste Reis Fernandes de Souza

    2008-12-01

    Full Text Available Este artigo tem como propósito discutir as diferenças apresentadas por mulheres e homens em práticas matemáticas cotidianas, demandadas pelos apelos ou pelas oportunidades de uma sociedade pautada na dinâmica e nos critérios da cultura escrita. Tomaremos para análise os resultados divulgados na quarta edição da pesquisa Indicador Nacional de Alfabetismo Funcional (INAF, realizada em 2004, que avaliou as condições e a eficiência da população jovem e adulta brasileira na mobilização de habilidades matemáticas na execução de tarefas do cotidiano, e na qual os resultados apresentados pela população masculina foram considerados sensivelmente superiores aos resultados apresentados pela população feminina. Apoiando-nos numa reflexão referenciada numa perspectiva foucaultiana, buscamos compreender esses resultados como articulados a um campo discursivo, marcado pela racionalidade matemática de matriz cartesiana. Analisando, nessa perspectiva, os mecanismos que contribuem para um pior desempenho das mulheres em relação aos homens em avaliações dessa natureza - voltadas para as possibilidades de dar respostas consideradas adequadas na execução de tarefas cotidianas consideradas relevantes -, nossa preocupação se volta para a identificação de mais uma instância de produção de desigualdades entre as mulheres e os homens, representada pela maior valorização (na vida social e nas avaliações de certos modos de conceber e reagir diante das demandas do cotidiano. Como educadoras, interessanos desvendar a produção das desigualdades, de maneira a desconstruir discursos que a favorecem e instaurar outras perspectivas de análise e de ação pedagógica.The purpose of this article is to discuss the differences observed between women and men in some of the daily mathematical practices made necessary by the demand and opportunities of a society based on the dynamics and criteria of written culture. We take for our analysis

  1. The Italian contribution to the CSES satellite

    Science.gov (United States)

    Conti, Livio

    2016-04-01

    We present the Italian contribution to the CSES (China Seismo-Electromagnetic Satellite) mission. The CSES satellite aims at investigating electromagnetic field, plasma and particles in the near-Earth environment in order to study in particular seismic precursors, particles fluxes (from Van Allen belts, cosmic rays, solar wind, etc.), anthropogenic electromagnetic pollution and more in general the atmosphere-ionosphere-magnetosphere coupling mechanisms that can affect the climate changes. The launch of CSES - the first of a series of several satellite missions - is scheduled by the end of 2016. The CSES satellite has been financed by the CNSA (China National Space Agency) and developed by CEA (China Earthquake Administration) together with several Chinese research institutes and private companies such as the DFH (that has developed the CAST2000 satellite platform). Italy participates to the CSES satellite mission with the LIMADOU project funded by ASI (Italian Space Agency) in collaboration with the Universities of Roma Tor Vergata, Uninettuno, Trento, Bologna and Perugia, as well as the INFN (Italian National Institute of Nuclear Physics), INGV (Italian National Institute of Geophysics and Volcanology) and INAF-IAPS (Italian National Institute of Astrophysics and Planetology). Many analyses have shown that satellite observations of electromagnetic fields, plasma parameters and particle fluxes in low Earth orbit may be useful in order to study the existence of electromagnetic emissions associated with the occurrence of earthquakes of medium and high magnitude. Although the earthquakes forecasting is not possible today, it is certainly a major challenge - and perhaps even a duty - for science in the near future. The claims that the reported anomalies (of electromagnetic, plasma and particle parameters) are seismic precursors are still intensely debated and analyses for confirming claimed correlations are still lacking. In fact, ionospheric currents, plasma

  2. MASSIV: Mass Assemby Survey with SINFONI in VVDS. I. Survey description and global properties of the 0.9 < z < 1.8 galaxy sample

    Science.gov (United States)

    Contini, T.; Garilli, B.; Le Fèvre, O.; Kissler-Patig, M.; Amram, P.; Epinat, B.; Moultaka, J.; Paioro, L.; Queyrel, J.; Tasca, L.; Tresse, L.; Vergani, D.; López-Sanjuan, C.; Perez-Montero, E.

    2012-03-01

    ://cosmosdb.lambrate.inaf.it/VVDS-SINFONI">http://cosmosdb.lambrate.inaf.it/VVDS-SINFONI. This work is based mainly on observations collected at the European Southern Observatory (ESO) Very Large Telescope, Paranal, Chile, as part of the Programs 179.A-0823, 177.A-0837, 78.A-0177, 75.A-0318, and 70.A-9007. This work also benefits from data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and the CNRS.Table 5 is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/539/A91

  3. Seasonal effects on the nucleus of comet 67P revealed by Rosetta/VIRTIS

    Science.gov (United States)

    Tosi, Federico; Capaccioni, Fabrizio; Filacchione, Gianrico; Erard, Stéphane; Rouseeau, Batiste; Combe, Jean-Philippe; Capria, Maria Teresa; Leyrat, Cédric; Longobardo, Andrea; Bockelée-Morvan, Dominique; Kappel, David; Arnold, Gabriele; Fonti, Sergio; Mancarella, Francesca; Kuehrt, Ekkehard; Mottola, Stefano

    2016-04-01

    hemisphere. These three regions are chosen so as to be relatively smooth at the spatial resolution that is achieved from a distance of about 100 km (25 m/px for VIRTIS-M, 50×150 m/px for VIRTIS-H), in order to limit the effects of large-scale surface roughness. Acknowledgements: The authors would like to thank the following institutions and agencies, which supported this work: Italian Space Agency (ASI - Italy), Centre National d'Etudes Spatiales (CNES- France), Deutsches Zentrum für Luft- und Raumfahrt (DLR-Germany), National Aeronautic and Space Administration (NASA-USA) Rosetta Program, Science and Technology Facilities Council (UK). VIRTIS has been built by a consortium, which includes Italy, France and Germany, under the scientific responsibility of the Istituto di Astrofisica e Planetologia Spaziali of INAF, Italy, which guides also the scientific operations. The VIRTIS instrument development has been funded and managed by ASI, with contributions from Observatoire de Meudon financed by CNES, and from DLR. The computational resources used in this research have been supplied by INAF-IAPS through the DataWell project.

  4. GIADA on-board Rosetta: comet 67P/C-G dust coma characterization

    Science.gov (United States)

    Rotundi, Alessandra; Della Corte, Vincenzo; Fulle, Marco; Sordini, Roberto; Ivanovski, Stavro; Accolla, Mario; Ferrari, Marco; Lucarelli, Francesca; Zakharov, Vladimir; Mazzotta Epifani, Elena; López-Moreno, José J.; Rodríguez, Julio; Colangeli, Luigi; Palumbo, Pasquale; Bussoletti, Ezio; Crifo, Jean-Francois; Esposito, Francesca; Green, Simon F.; Grün, Eberhard; Lamy, Philippe L.

    2015-04-01

    complete set of dust grain parameters, i.e., mass, speed, and geometrical cross-section. These detections allowed us to constraint the grain density. The GIADA detections type was studied as a function of the observational geometrical configuration. Acknowledgments: GIADA was built by a consortium led by the Univ. Napoli "Parthenope" & INAF- Oss. Astr. Capodimonte, in collaboration with the Inst. de Astrofisica de Andalucia, Selex-ES, FI and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with the support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developed from a PI proposal from the University of Kent; sci. & tech. contribution were provided by CISAS, IT, Lab. d'Astr. Spat., FR, and Institutions from UK, IT, FR, DE and USA. We thank the RSGS/ESAC, RMOC/ESOC & Rosetta Project/ESTEC for their outstanding work. Science support provided was by NASA through the US Rosetta Project managed by the Jet Propulsion Laboratory/California Institute of Technology. GIADA calibrated data will be available through ESA's PSA web site (www.rssd.esa.int/index.php?project=PSA&page=in dex). We would like to thank Angioletta Coradini for her contribution as a GIADA Co-I.

  5. European Virtual Atomic And Molecular Data Center - VAMDC

    Science.gov (United States)

    Dimitrijevic, M. S.; Sahal-Brechot, S.; Kovacevic, A.; Jevremovic, D.; Popovic, L. C.

    2010-07-01

    Reliable atomic and molecular data are of great importance for different applications in astrophysics, atmospheric physics, fusion, environmental sciences, combustion chemistry, and in industrial applications from plasmas and lasers to lighting. Currently, very important resources of such data are highly fragmented, presented in different, nonstandardized ways, available through a variety of highly specialized and often poorly documented interfaces, so that the full exploitation of all their scientific worth is limited, hindering research in many topics like e.g. the characterization of extrasolar planets, understanding the chemistry of our local solar system and of the wider universe, the study of the terrestrial atmosphere and quantification of climate change; the development of the fusion rersearch, etc. The Virtual Atomic and Molecular Data Centre (http://www.vamdc.eu, VAMDC) is an European Union funded FP7 project aiming to build a secure, documented, flexible and interoperable e-science environment-based interface to existing atomic and molecular data. It will also provide a forum for training potential users and dissemination of expertise worldwide. Partners in the Consortium of the Project are: 1) Centre National de Recherche Scientifique - CNRS (Paris, Reims, Grenoble, Bordeaux, Dijon, Toulouse); 2) The Chancellor, Masters and Scholars of the University of Cambridge - CMSUC; 3) University College London - UCL; 4) Open University - OU; (Milton Keynes, England); 5) Universitaet Wien - UNIVIE; 6) Uppsala Universitet - UU; 7) Universitaet zu Koeln - KOLN; 8) Istituto Nazionale di Astrofisica - INAF (Catania, Cagliari); 9) Queen's University Belfast - QUB; 10) Astronomska Opservatorija - AOB (Belgrade, Serbia); 11) Institute of Spectroscopy RAS - ISRAN (Troitsk, Russia); 12) Russian Federal Nuclear Center - All-Russian Institute of Technical Physics - RFNC-VNIITF (Snezhinsk, Chelyabinsk Region, Russia; 13) Institute of Atmospheric Optics - IAO (Tomsk, Russia

  6. The ASTRI Mini-Array Science Case

    Science.gov (United States)

    Vercellone, Stefano; Catalano, O.; Maccarone, M.; Stamerra, A.; Di Pierro, F.; Vallania, P.; Canestrari, R.; Bonnoli, G.; Pareschi, G.; Tosti, G.; Caraveo, P.; ASTRI Collaboration

    2013-04-01

    ASTRI is a flagship project of the Italian Ministry of Education, University and Research. Within this framework, INAF is currently developing an end-to-end prototype of the CTA small-size telescope in a dual-mirror configuration (SST-2M) to be tested under field conditions, and scheduled to start data acquisition in 2014. A remarkable improvement in terms of performance could come from the operation, in 2016, of a SST-2M mini-array, composed by a few SST-2M telescopes and to be placed at final CTA Southern Site. The SST mini-array will be able to study in great detail relatively bright sources (a few x10E-12 erg/cm2/s at 10 TeV) with an angular resolution of a few arcmin and an energy resolution of about 10 - 15%. Moreover, thanks to the array approach, it will be possible to verify the wide FoV performance to detect very high energy showers with the core located at a distance up to 500 m, to compare the mini-array performance with the Monte Carlo expectations by means of deep observations of few selected targets, and to perform the first CTA science, with its first solid detections during the first year of operation. Prominent sources such as extreme blazars (1ES 0229+200), nearby well-known BL Lac objects (MKN 501) and radio-galaxies, galactic pulsar wind nebulae (Crab Nebula, Vela-X), supernovae remnants (Vela-junior, RX J1713.7-3946) and microquasars (LS 5039), as well as the Galactic Center can be observed in a previously unexplored energy range, in order to investigate the electron acceleration and cooling, relativistic and non relativistic shocks, the search for cosmic-ray (CR) Pevatrons, the study of the CR propagation, and the impact of the extragalactic background light on the spectra of the sources.

  7. The VIMOS Public Extragalactic Redshift Survey (VIPERS). An unprecedented view of galaxies and large-scale structure at 0.5 < z < 1.2

    Science.gov (United States)

    Guzzo, L.; Scodeggio, M.; Garilli, B.; Granett, B. R.; Fritz, A.; Abbas, U.; Adami, C.; Arnouts, S.; Bel, J.; Bolzonella, M.; Bottini, D.; Branchini, E.; Cappi, A.; Coupon, J.; Cucciati, O.; Davidzon, I.; De Lucia, G.; de la Torre, S.; Franzetti, P.; Fumana, M.; Hudelot, P.; Ilbert, O.; Iovino, A.; Krywult, J.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marulli, F.; McCracken, H. J.; Paioro, L.; Peacock, J. A.; Polletta, M.; Pollo, A.; Schlagenhaufer, H.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zamorani, G.; Zanichelli, A.; Burden, A.; Di Porto, C.; Marchetti, A.; Marinoni, C.; Mellier, Y.; Moscardini, L.; Nichol, R. C.; Percival, W. J.; Phleps, S.; Wolk, M.

    2014-06-01

    We describe the construction and general features of VIPERS, the VIMOS Public Extragalactic Redshift Survey. This ESO Large Programme is using the Very Large Telescope with the aim of building a spectroscopic sample of ~ 100 000 galaxies with iABcontamination is found to be only 3.2%, endorsing the quality of the star-galaxy separation process and fully confirming the original estimates based on the VVDS data, which also indicate a galaxy incompleteness from this process of only 1.4%. Using a set of 1215 repeated observations, we estimate an rms redshift error σz/ (1 + z) = 4.7 × 10-4 and calibrate the internal spectral quality grading. Benefiting from the combination of size and detailed sampling of this dataset, we conclude by presenting a map showing in unprecedented detail the large-scale distribution of galaxies between 5 and 8 billion years ago. Based on observations collected at the European Southern Observatory, Cerro Paranal, Chile, using the Very Large Telescope under programmes 182.A-0886 and partly 070.A-9007. Also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS website is http://www.vipers.inaf.it/

  8. Insight into the nature and formation of the organic matter observed on Ceres

    Science.gov (United States)

    Ammannito, E.; Vinogradoff, V.; De Sanctis, M. C.; De Angelis, S.; Ferrari, M.; Ciarniello, M.; Raponi, A.; Raymond, C. A.; Russell, C. T.

    2017-12-01

    Observed by the Dawn spacecraft since March 2015, Ceres is a fascinating world [1]. Its surface, covered by phyllosilicates, carbonates, ammoniated-bearing hydrated minerals, water ice, salts and opaque materials indicates a complex chemical environment [1,2,3]. VIR, the Visible and InfraRed mapping spectrometer onboard the Dawn mission, has revealed the presence of aliphatic carbons with the 3.3-3.5 µm bands, near the Ernutet crater [4]. The origin of this OM is likely related to an endogenous source [4] and new issues are raised: what is the origin formation and the true nature of the OM hidden behind these aliphatic signatures? We used the spectral imaging (SPIM) facility in use at the laboratory of IAPS-INAF (spare of the VIR instrument onboard Dawn) to measure organic materials in the range 0.2-5.1 µm. These materials, such as insoluble organic matter (IOM) of chondrites, synthetic polymers, asphaltite, as well as spectra from literature data have been compared to VIR data. The Ceres aliphatic bands might match with an aliphatic branched polymer structure, i.e. with a 1.3 minerals. In either case, the partial differentiation of Ceres, might have driven the volatiles (i.e. the organic matter) near the surface. The second hypothesis, might also explain the high concentration of nitrogen. [1] Russell et al., (2016) Science, 353 (6303) 1008-1010. [2] De Sanctis et al., (2015) Nature 528, 241-244. [3] De Sanctis et al., (2016) Nature 536, 54- 57. [4] De Sanctis et al., (2017) Science, 355, 719-722. [5] Holm et al., (2015), Astrobiology, 15, 587-600.

  9. Second-order spherical optoelectronic detector for 3D multi-particles wave emission and propagation in space time domains

    Science.gov (United States)

    Romano, Francesco; Cimmino, Rosario F.

    2017-09-01

    This paper concerns a feasibility study on a 2nd order spherical, or three-dimensional, angular momentum and linear momentum detector for photonic radiation applications. It has been developed in order to obtain a paraxial approximation of physical events observed under Coulomb gauge condition, which is essential to compute both the longitudinal and transverse rotational components of the observed 3-D vortex field, generally neglected by conventional detection systems under current usage. Since light and laser beams are neither full transversal or rotational phenomena, to measure directly and in the same time both the energy, mainly not-rotational, related to the relevant part of the linear momentum and the potential solenoidal energy (vortex), related to the angular momentum, 2nd order spherical, or 3-D, detector techniques are required. In addition, direct 2nd order measure techniques enable development of TEM + DEM [17] studies, therefore allowing for monochromatic complex wave detection with a paraxial accuracy in the relativistic time-space domain. Light and optic or Electromagnetic 2nd order 3-D AnM energy may usefully be used in tre-dimensional optical TEM, noTEM, DEM vortex or laser communications The paper illustrates an innovative quadratic order 3-D spherical model detector applied to directly measure a light source power spectrum and compares the performances of this innovative technique with those obtained with a traditional 1st order system. Results from a number of test experiments conducted in cooperation with INAF Observatories of ArcetriFlorence and Medicina-Bologna (Italy), and focused on telescopic observations of the inter-stellar electromagnetic radiations, are also summarized. The innovative quadratic-order spherical detector turns out to be optimal for optical and/or radio telescopes application, optical and optoelectronic sensors development and gravitational wave 2nd order detectors implementation. Although the proposed method is very

  10. A PHOTOGRAMMETRIC PIPELINE FOR THE 3D RECONSTRUCTION OF CASSIS IMAGES ON BOARD EXOMARS TGO

    Directory of Open Access Journals (Sweden)

    E. Simioni

    2017-07-01

    Full Text Available CaSSIS (Colour and Stereo Surface Imaging System is the stereo imaging system onboard the European Space Agency and ROSCOSMOS ExoMars Trace Gas Orbiter (TGO that has been launched on 14 March 2016 and entered a Mars elliptical orbit on 19 October 2016. During the first bounded orbits, CaSSIS returned its first multiband images taken on 22 and 26 November 2016. The telescope acquired 11 images, each composed by 30 framelets, of the Martian surface near Hebes Chasma and Noctis Labyrithus regions reaching at closest approach at a distance of 250 km from the surface. Despite of the eccentricity of this first orbit, CaSSIS has provided one stereo pair with a mean ground resolution of 6 m from a mean distance of 520 km. The team at the Astronomical Observatory of Padova (OAPD-INAF is involved into different stereo oriented missions and it is realizing a software for the generation of Digital Terrain Models from the CaSSIS images. The SW will be then adapted also for other projects involving stereo camera systems. To compute accurate 3D models, several sequential methods and tools have been developed. The preliminary pipeline provides: the generation of rectified images from the CaSSIS framelets, a matching core and post-processing methods. The software includes in particular: an automatic tie points detection by the Speeded Up Robust Features (SURF operator, an initial search for the correspondences through Normalize Cross Correlation (NCC algorithm and the Adaptive Least Square Matching (LSM algorithm in a hierarchical approach. This work will show a preliminary DTM generated by the first CaSSIS stereo images.

  11. Imaging X-Ray Polarimetry Explorer (IXPE) Risk Management

    Science.gov (United States)

    Alexander, Cheryl; Deininger, William D.; Baggett, Randy; Primo, Attina; Bowen, Mike; Cowart, Chris; Del Monte, Ettore; Ingram, Lindsey; Kalinowski, William; Kelley, Anthony; hide

    2018-01-01

    The Imaging X-ray Polarimetry Explorer (IXPE) project is an international collaboration to build and fly a polarization sensitive X-ray observatory. The IXPE Observatory consists of the spacecraft and payload. The payload is composed of three X-ray telescopes, each consisting of a mirror module optical assembly and a polarization-sensitive X-ray detector assembly; a deployable boom maintains the focal length between the optical assemblies and the detectors. The goal of the IXPE Mission is to provide new information about the origins of cosmic X-rays and their interactions with matter and gravity as they travel through space. IXPE will do this by exploiting its unique capability to measure the polarization of X-rays emitted by cosmic sources. The collaboration for IXPE involves national and international partners during design, fabrication, assembly, integration, test, and operations. The full collaboration includes NASA Marshall Space Flight Center (MSFC), Ball Aerospace, the Italian Space Agency (ASI), the Italian Institute of Astrophysics and Space Planetology (IAPS)/Italian National Institute of Astrophysics (INAF), the Italian National Institute for Nuclear Physics (INFN), the University of Colorado (CU) Laboratory for Atmospheric and Space Physics (LASP), Stanford University, McGill University, and the Massachusetts Institute of Technology. The goal of this paper is to discuss risk management as it applies to the IXPE project. The full IXPE Team participates in risk management providing both unique challenges and advantages for project risk management. Risk management is being employed in all phases of the IXPE Project, but is particularly important during planning and initial execution-the current phase of the IXPE Project. The discussion will address IXPE risk strategies and responsibilities, along with the IXPE management process which includes risk identification, risk assessment, risk response, and risk monitoring, control, and reporting.

  12. GIARPS@TNG: GIANO-B and HARPS-N together for a wider wavelength range spectroscopy

    Science.gov (United States)

    Claudi, R.; Benatti, S.; Carleo, I.; Ghedina, A.; Guerra, J.; Micela, G.; Molinari, E.; Oliva, E.; Rainer, M.; Tozzi, A.; Baffa, C.; Baruffolo, A.; Buchschacher, N.; Cecconi, M.; Cosentino, R.; Fantinel, D.; Fini, L.; Ghinassi, F.; Giani, E.; Gonzalez, E.; Gonzalez, M.; Gratton, R.; Harutyunyan, A.; Hernandez, N.; Lodi, M.; Malavolta, L.; Maldonado, J.; Origlia, L.; Sanna, N.; Sanjuan, J.; Scuderi, S.; Seemann, U.; Sozzetti, A.; Perez Ventura, H.; Hernandez Diaz, M.; Galli, A.; Gonzalez, C.; Riverol, L.; Riverol, C.

    2017-08-01

    Since 2012, thanks to the installation of the high-resolution echelle spectrograph in the optical range HARPS-N, the Italian telescope TNG (La Palma) became one of the key facilities for the study of the extrasolar planets. In 2014 TNG also offered GIANO to the scientific community, providing a near-infrared (NIR) cross-dispersed echelle spectroscopy covering 0.97-2.45μm at a resolution of 50000. GIANO, although designed for direct light-feed from the telescope at the Nasmyth-B focus, was provisionally mounted on the rotating building and connected via fibers to only available interface at the Nasmyth-A focal plane. The synergy between these two instruments is particularly appealing for a wide range of science cases, especially for the search of exoplanets around young and active stars and the characterisation of their atmosphere. Through the funding scheme "WOW" (a Way to Others Worlds), the Italian National Institute for Astrophysics (INAF) proposed to position GIANO at the focal station for which it was originally designed and the simultaneous use of these spectrographs with the aim to achieve high-resolution spectroscopy in a wide wavelength range (0.383-2.45μm) obtained in a single exposure, giving rise to the project called GIARPS (GIANO-B & HARPS-N). Because of its characteristics, GIARPS can be considered the first and unique worldwide instrument providing not only high resolution in a large wavelength band, but also a high-precision radial velocity measurement both in the visible and in the NIR arm, since in the next future GIANO-B will be equipped with gas absorption cells.

  13. Mount control system of the ASTRI SST-2M prototype for the Cherenkov Telescope Array

    Science.gov (United States)

    Antolini, Elisa; Tosti, Gino; Tanci, Claudio; Bagaglia, Marco; Canestrari, Rodolfo; Cascone, Enrico; Gambini, Giorgio; Nucciarelli, Giuliano; Pareschi, Giovanni; Scuderi, Salvo; Stringhetti, Luca; Busatta, Andrea; Giacomel, Stefano; Marchiori, Gianpietro; Manfrin, Cristiana; Marcuzzi, Enrico; Di Michele, Daniele; Grigolon, Carlo; Guarise, Paolo

    2016-08-01

    The ASTRI SST-2M telescope is an end-to-end prototype proposed for the Small Size class of Telescopes (SST) of the future Cherenkov Telescope Array (CTA). The prototype is installed in Italy at the INAF observing station located at Serra La Nave on Mount Etna (Sicily) and it was inaugurated in September 2014. This paper presents the software and hardware architecture and development of the system dedicated to the control of the mount, health, safety and monitoring systems of the ASTRI SST-2M telescope prototype. The mount control system installed on the ASTRI SST-2M telescope prototype makes use of standard and widely deployed industrial hardware and software. State of the art of the control and automation industries was selected in order to fulfill the mount related functional and safety requirements with assembly compactness, high reliability, and reduced maintenance. The software package was implemented with the Beckhoff TwinCAT version 3 environment for the software Programmable Logical Controller (PLC), while the control electronics have been chosen in order to maximize the homogeneity and the real time performance of the system. The integration with the high level controller (Telescope Control System) has been carried out by choosing the open platform communications Unified Architecture (UA) protocol, supporting rich data model while offering compatibility with the PLC platform. In this contribution we show how the ASTRI approach for the design and implementation of the mount control system has made the ASTRI SST-2M prototype a standalone intelligent machine, able to fulfill requirements and easy to be integrated in an array configuration such as the future ASTRI mini-array proposed to be installed at the southern site of the Cherenkov Telescope Array (CTA).

  14. The NEOShield-2 EU Project - The Italian contribution

    Science.gov (United States)

    Ieva, Simone; Dotto, Elisabetta; Mazzotta Epifani, Elena; Di Paola, Andrea; Speziali, Roberto; Cortese, Matteo; Lazzarin, Monica; Bertini, Ivano; Magrin, Sara; Barucci, Maria Antonietta; Perna, Davide; Perozzi, Ettore; Micheli, Marco

    2016-04-01

    The Near Earth Object (NEO) population comprehends small bodies that periodically approach or intersect the Earth's orbit. NEOs could have possible impacts with the Earth and, whatever the scenario, their physical characterization is essential to define successful mitigation strategies. Moreover, their study is important per se, since they represent the closest remnants of the planetary formation, 4.5 billion years ago, and the knowledge of their physical properties allows us to put constraints on the formation and early evolution of the Solar System. On the basis of these considerations, the NEO population is an important target for ground-based studies. Unfortunately, less than 15% of the 13500 known NEOs has a physical characterization, showing a great diversity - in sizes, shapes, rotational periods, albedos, and composition - and their increasing discovery rate (currently ˜1500 objects/year) makes the situation progressively worse. At a European level, the European Commission promoted the study on NEOs by approving and financing the NEOShield-2 project (2015-2017) in the framework of the Horizon 2020 program. The aims of NEOShield-2 are: i) to study detailed technologies and instruments to conduct close approach missions to NEOs or to undertake mitigation demonstration, and ii) to retrieve the physical properties of a wide number of NEOs, in order to design impact mitigation missions and assess the consequences of an impact on Earth. The Italian contributors to the NEOShield-2 project (INAF-OAR and Padova University) are responsible for the Task 10.2.1 'Colours and Phase function'. The aim of this task is to acquire photometric measurements for a wide sample of NEOs in order to i) perform phase function analysis, ii) retrieve surface colors and iii) obtain a preliminary taxonomical classification. This activity is developed in close collaboration with the ESA SSA NEO Coordination Centre.

  15. Voice-coil technology for the E-ELT M4 Adaptive Unit

    Science.gov (United States)

    Gallieni, D.; Tintori, M.; Mantegazza, M.; Anaclerio, E.; Crimella, L.; Acerboni, M.; Biasi, R.; Angerer, G.; Andrigettoni, M.; Merler, A.; Veronese, D.; Carel, J.-L.; Marque, G.; Molinari, E.; Tresoldi, D.; Toso, G.; Spanó, P.; Riva, M.; Mazzoleni, R.; Riccardi, A.; Mantegazza, P.; Manetti, M.; Morandini, M.; Vernet, E.; Hubin, N.; Jochum, L.; Madec, P.; Dimmler, M.; Koch, F.

    We present our design of the E-ELT M4 Adaptive Unit based on voice-coil driven deformable mirror technology. This technology was developed by INAF-Arcetri, Microgate and ADS team in the past 15 years and it has been adopted by a number of large ground based telescopes as the MMT, LBT, Magellan and lastly the VLT in the frame of the Adaptive Telescope Facility project. Our design is based on contactless force actuators made by permanent magnets glued on the back of the deformable mirror and coils mounted on a stiff reference structure. We use capacitive sensors to close a position loop co-located with each actuator. Dedicated high performance parallel processors are used to implement the local de-centralized control at actuator level and a centralized feed-forward computation of all the actuators forces. This allowed achieving in our previous systems dynamic performances well in line with the requirements of the M4 Adaptive Unit (M4AU) case. The actuator density of our design is in the order of 30-mm spacing for a figure of about 6000 actuators on the M4AU and it allows fulfilling the fitting error and corrections requirements of the E-ELT high order DM. Moreover, our contact-less technology makes the Deformable Mirror tolerant to up 5% actuators failures without spoiling system capability to reach its specified performances, besides allowing large mechanical tolerances between the reference structure and the deformable mirror. Finally, we present the Demonstration Prototype we are building in the frame of the M4AU Phase B study to measure the optical dynamical performances predicted by our design. Such a prototype will be fully representative of the M4AU features, in particular it will address the controllability of two adjacent segments of the 2-mm thick mirror and implement the actuators "brick" modular concept that has been adopted to dramatically improve the maintainability of the final unit.

  16. The RoPES project with HARPS and HARPS-N. I. A system of super-Earths orbiting the moderately active K-dwarf HD 176986

    Science.gov (United States)

    Suárez Mascareño, A.; González Hernández, J. I.; Rebolo, R.; Velasco, S.; Toledo-Padrón, B.; Udry, S.; Motalebi, F.; Ségrasan, D.; Wyttenbach, A.; Mayor, M.; Pepe, F.; Lovis, C.; Santos, N. C.; Figueira, P.; Esposito, M.

    2018-04-01

    We report the discovery of a system of two super-Earths orbiting the moderately active K-dwarf HD 176986. This work is part of the RoPES RV program of G- and K-type stars, which combines radial velocities (RVs) from the HARPS and HARPS-N spectrographs to search for short-period terrestrial planets. HD 176986 b and c are super-Earth planets with masses of 5.74 and 9.18 M⊕, orbital periods of 6.49 and 16.82 days, and distances of 0.063 and 0.119 AU in orbits that are consistent with circular. The host star is a K2.5 dwarf, and despite its modest level of chromospheric activity (log10 (RHK' = -4.90 ± 0.04), it shows a complex activity pattern. Along with the discovery of the planets, we study the magnetic cycle and rotation of the star. HD 176986 proves to be suitable for testing the available RV analysis technique and further our understanding of stellar activity. Full Table A.1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/612/A41Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF - Fundación Galileo Galilei at the Roche de Los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); observations made with the HARPS instrument on the ESO 3.6-m telescope at La Silla Observatory (Chile).

  17. The VIMOS Public Extragalactic Redshift Survey (VIPERS). Downsizing of the blue cloud and the influence of galaxy size on mass quenching over the last eight billion years

    Science.gov (United States)

    Haines, C. P.; Iovino, A.; Krywult, J.; Guzzo, L.; Davidzon, I.; Bolzonella, M.; Garilli, B.; Scodeggio, M.; Granett, B. R.; de la Torre, S.; De Lucia, G.; Abbas, U.; Adami, C.; Arnouts, S.; Bottini, D.; Cappi, A.; Cucciati, O.; Franzetti, P.; Fritz, A.; Gargiulo, A.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marulli, F.; Moutard, T.; Polletta, M.; Pollo, A.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Zamorani, G.; Bel, J.; Branchini, E.; Coupon, J.; Ilbert, O.; Moscardini, L.; Peacock, J. A.; Siudek, M.

    2017-08-01

    We use the full VIPERS redshift survey in combination with SDSS-DR7 to explore the relationships between star-formation history (using d4000), stellar mass and galaxy structure, and how these relationships have evolved since z 1. We trace the extents and evolutions of both the blue cloud and red sequence by fitting double Gaussians to the d4000 distribution of galaxies in narrow stellar mass bins, for four redshift intervals over 0 1011M⊙, d4000 parallel, their structures change, showing higher Sérsic indices and central stellar mass densities. For these galaxies, bulge growth is required for them to reach the high-mass limit of the blue cloud and be quenched by internal mechanisms. The blue-cloud galaxies that are being quenched at z 0.8 lie along the same size-mass relation as present day quiescent galaxies and seem the likely progenitors of today's S0s. Based on observations collected at the European Southern Observatory, Cerro Paranal, Chile, using the Very Large Telescope under programs 182.A-0886 and partly 070.A-9007. Also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS web site is http://www.vipers.inaf.it/

  18. Access to VIRTIS / Venus-Express post-operations data archive

    Science.gov (United States)

    Erard, Stéphane; Drossart, Pierre; Piccioni, Giuseppe; Henry, Florence; Politi, Romolo

    2016-10-01

    All data acquired during the Venus-Express mission are publicly available on ESA's Planetary Science Archive (PSA). The PSA itself is being redesigned to provide more comprehensive access to its content and a new interface is expected to be ready in the coming months.However, an alternative access to the VIRTIS/VEx dataset is also provided in the PI institutes as part of the Europlanet-2020 European programme. The VESPA user interface (http://vespa.obspm.fr) provides a query mechanism based on observational conditions and instrument parameters to select data cubes of interest in the PSA and to connect them to standard plotting and analysis tools. VESPA queries will also identify related data in other datasets responsive to this mechanism, e. g., contextual images or dynamic simulations of the atmosphere, including outcomes of the EuroVenus programme funded by the EU. A specific on-line spectral cube viewer has been developed at Paris Observatory (http://voplus.obspm.fr/apericubes/js9/demo.php). Alternative ways to access the VIRTIS data are being considered, including python access to PDS3 data (https://github.com/VIRTIS-VEX/VIRTISpy) and distribution in NetCDF format on IAPS website (http://planetcdf.iaps.inaf.it). In the near future, an extended data service will provide direct access to individual spectra on the basis of viewing angles, time, and location.The next step will be to distribute products derived from data analysis, such as surface and wind maps, atmospheric profiles, movies of the polar vortices or O2 emission on the night side, etc. Such products will be accessed in a similar way, and will make VIRTIS results readily available for future Venus studies. Similar actions are taken in the frame of Europlanet concerning atmospheric data from the Mars-Express mission and Cassini observations of Titan.

  19. IXPE the Imaging X-ray Polarimetry Explorer

    Science.gov (United States)

    Soffitta, Paolo

    2017-08-01

    IXPE, the Imaging X-ray Polarimetry Explorer, has been selected as a NASA SMEX mission to be flown in 2021. It will perform polarimetry resolved in energy, in time and in angle as a break-through in High Energy Astrophysics. IXPE promises to 're-open', after 40 years, a window in X-ray astronomy adding two more observables to the usual ones. It will directly measure the geometrical parameters of many different classes of sources eventually breaking possible degeneracies. The probed angular scales (30") are capable of producing the first X-ray polarization maps of extended objects with scientifically relevant sensitivity. This will permit mapping the magnetic fields in Pulsar Wind Nebulae and Super-Nova Remnants at the acceleration sites of 10-100 TeV electrons. Additionally, it will probe vacuum birefringence effects in systems with magnetic fields far larger than those reachable with experiments on Earth. The payload of IXPE consists of three identical telescopes with mirrors provided by MSFC/NASA. The focal plane is provided by ASI with IAPS/INAF responsible for the overall instrument that includes detector units that are provided by INFN. ASI also provides, in kind, the Malindi Ground Station. LASP is responsible for the Mission Operation Center while the Science Operation Center is at MSFC. The operations phase lasts at least two years. All the data including those related to polarization will be made available quickly to the general user. In this paper we present the mission, its payload and we discuss a few examples of astrophysical targets.

  20. Evaluation of software and electronics technologies for the control of the E-ELT instruments: a case study

    International Nuclear Information System (INIS)

    Di Marcantonio, P.; Cirami, R.; Coretti, I.; Chiozzi, G.; Kiekebusch, M.

    2012-01-01

    In the scope of the evaluation of architecture and technologies for the control system of the E-ELT (European-Extremely Large Telescope) instruments, a collaboration has been set up between the Instrumentation and Control Group of the INAF-OATs and the ESO Directorate of Engineering. The first result of this collaboration is the design and implementation of a prototype of a small but representative control system for a kind of multi-object (optical) spectrograph. The electronics has been based on PLCs (Programmable Logical Controller) and Ethernet based field-buses from different vendors but using international standards like the IEC 61131-3 and PLCopen Motion Control. The baseline design for the control software follows the architecture of the VLT (Very Large Telescope) Instrumentation application framework but it has been implemented using the ACS (ALMA Common Software), an open source software framework developed for the ALMA project and based on CORBA middle-ware. The communication among the software components is based on two models: CORBA calls for command/reply using the client/server paradigm and CORBA notification channel for distributing the devices status using the publisher/subscriber paradigm. The communication with the PLCs is based on OPC UA, an international standard for the communication with industrial controllers. The results of this work will contribute to the definition of the architecture of the control system that will be provided to all consortia responsible for the actual implementation of the E-ELT instruments. This paper presents the prototype motivation, its architecture, design and implementation. (authors)

  1. ROSAT Discovers Unique, Distant Cluster of Galaxies

    Science.gov (United States)

    1995-06-01

    Brightest X-ray Cluster Acts as Strong Gravitational Lens Based on exciting new data obtained with the ROSAT X-ray satellite and a ground-based telescope at the ESO La Silla Observatory, a team of European astronomers [2] has just discovered a very distant cluster of galaxies with unique properties. It emits the strongest X-ray emission of any cluster ever observed by ROSAT and is accompanied by two extraordinarily luminous arcs that represent the gravitationally deflected images of even more distant objects. The combination of these unusual characteristics makes this cluster, now known as RXJ1347.5-1145, a most interesting object for further cosmological studies. DISCOVERY AND FOLLOW-UP OBSERVATIONS This strange cluster of galaxies was discovered during the All Sky Survey with the ROSAT X-ray satellite as a moderately intense X-ray source in the constellation of Virgo. It could not be identified with any already known object and additional ground-based observations were therefore soon after performed with the Max-Planck-Society/ESO 2.2-metre telescope at the La Silla observatory in Chile. These observations took place within a large--scale redshift survey of X-ray clusters of galaxies detected by the ROSAT All Sky Survey, a so-called ``ESO Key Programme'' led by astronomers from the Max-Planck-Institut fur Extraterrestrische Physik and the Osservatorio Astronomico di Brera. The main aim of this programme is to identify cluster X-ray sources, to determine the distance to the X-ray emitting clusters and to investigate their overall properties. These observations permitted to measure the redshift of the RXJ1347.5-1145 cluster as z = 0.45, i.e. it moves away from us with a velocity (about 106,000 km/sec) equal to about one-third of the velocity of light. This is an effect of the general expansion of the universe and it allows to determine the distance as about 5,000 million light-years (assuming a Hubble constant of 75 km/sec/Mpc). In other words, we see these

  2. Comparison of existing syncope rules and newly proposed anatolian syncope rule to predict short-term serious outcomes after syncope in the Turkish population.

    Science.gov (United States)

    Kayayurt, Kamil; Akoglu, Haldun; Limon, Onder; Ergene, Asım Oktay; Yavasi, Ozcan; Bayata, Serdar; Berk, Nergiz Vanden; Unluer, Erden Erol

    2012-04-20

    We wished to compare the San Francisco Syncope Rule (SFSR), Evaluation of Guidelines in Syncope Study (EGSYS) and the Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) risk scores and to assess their efficacy in recognising patients with syncope at high risk for short-term adverse events (death, the need for major therapeutic procedures, and early readmission to the hospital). We also wanted to test those variables to designate a local risk score, the Anatolian Syncope Rule (ASR). This prospective, cohort study was conducted at the emergency department of a tertiary care centre. Between December 1 2009 and December 31 2010, we prospectively collected data on patients of ages 18 and over who presented to the emergency department with syncope. We enrolled 231 patients to the study. A univariate analysis found 23 variables that predicted syncope with adverse events. Dyspnoea, orthostatic hypotension, precipitating cause of syncope, age over 58 years, congestive heart failure, and electrocardiogram abnormality (termed DO-PACE) were found to predict short-term serious outcomes by logistic regression analysis and these were used to compose the ASR. The sensitivity of ASR, OESIL, EGSYS and SFSR for mortality were 100% (0.66 to 1.00); 90% (0.54 to 0.99), 80% (0.44 to 0.97) and 100% (0.66 to 1.00), respectively. The specificity of ASR, OESIL, EGSYS and SFSR for mortality were 78% (0.72 to 0.83); 76% (0.70 to 0.82); 80% (0.74 to 0.85) and 70% (0.63 to 0.76). The sensitivity of ASR, OESIL, EGSYS and SFSR for any adverse event were 97% (0.85 to 1.00); 70% (0.52 to 0.82); 56% (0.40 to 0.72) and 87% (0.72 to 0.95). The specificity of ASR, OESIL, EGSYS and SFSR for any adverse event were 72% (0.64 to 0.78); 82% (0.76 to 0.87); 84% (0.78 to 0.89); 78% (0.71 to 0.83), respectively. The newly proposed ASR appears to be highly sensitive for identifying patients at risk for short-term serious outcomes, with scores at least as good as those provided by existing diagnostic

  3. The Risk stratification Of Syncope in the Emergency department (ROSE) pilot study: a comparison of existing syncope guidelines.

    Science.gov (United States)

    Reed, Matthew J; Newby, David E; Coull, Andrew J; Jacques, Keith G; Prescott, Robin J; Gray, Alasdair J

    2007-04-01

    This study was conducted as a feasibility pilot for the Risk stratification Of Syncope in the Emergency department (ROSE) study. The secondary aim was to compare the performance of our existing emergency department (ED) guidelines with existing clinical decision rules (Osservatorio Epidemiologico sulla Sincope nel Lazio (OESIL) Score and San Francisco Syncope Rule; SFSR) at predicting short-term (1 week and 1 month) and medium-term (3 months) serious outcomes for patients with syncope presenting to the ED. This was a prospective cohort study. All patients presenting with syncope aged > or = 16 years between 7 November 2005 and 7 February 2006 were prospectively enrolled. 99 patients were recruited over a 3-month period. 44 patients were admitted and 55 discharged from the ED. 11 patients had a serious outcome: 8 by 7 days and a further 3 by 3 months. Five patients died by 3 months and six others had an alternative serious outcome. All 11 patients had been admitted from the ED, 7 were at high risk, 4 were at medium risk and none were at low risk according to our existing ED guidelines. Percentages of serious outcomes were 0%, 2.9%, 8.0%, 22.7% and 37.5% for OESIL scores of 0, 1, 2, 3 and 4 respectively. 40 patients had none of the 5 SFSR high-risk factors (0 serious outcomes = 0%) and 59 patients had an SFSR high-risk factor (11 serious outcomes = 18.6%). The risk of serious outcome at 7 days, 1 month and 3 months was 8.1%, 8.1% and 11.1%, respectively. A study to derive and validate a UK ED syncope clinical decision rule is feasible. This pilot study has evaluated the OESIL score, the SFSR and our existing ED guidelines, and has shown that each is able to identify an increased probability of medium-term serious outcome in patients with syncope. The SFSR shows good sensitivity at the expense of an increase in admissions to hospital; however, our existing ED syncope guidelines and the OESIL Score, although being able to successfully risk stratify patients, are not

  4. Web Based Seismological Monitoring (wbsm)

    Science.gov (United States)

    Giudicepietro, F.; Meglio, V.; Romano, S. P.; de Cesare, W.; Ventre, G.; Martini, M.

    generic data source it is sufficient to modify or substitute the interface modules. WBSM is running at the "Osservatorio Vesuviano" Monitoring Center since the beginning of 2001 and can be visited at http://ov.ingv.it.

  5. Soil Organic Carbon (SOC) distribution in two differents soil types (Podzol and Andosol) under natural forest cover.

    Science.gov (United States)

    Álvarez-Romero, Marta; Papa, Stefania; Verstraeten, Arne; Cools, Nathalie; Lozano-García, Beatriz; Parras-Alcántara, Luis; Coppola, Elio

    2017-04-01

    Andosols are young soils that shall know a successive evolution towards pedological types where the dominant pedogenetic processes are more evident. Vegetation and climate influence Andosols evolution to other order of soils. In cold and wet climates or on acid vulcanite under heavy leaching young Andosols could change into Podzols (Van Breemn and Buurman, 1998). Were investigated a Podzol soil (World References Base, 2014) at Zoniën (Belgium), were and an Andosol soil (World References Base, 2014) at Lago Laceno (Avellino, Italy). This study shows the data on the SOC (Soil Organic Carbon) fractionation in two profiles from two natural pine forest soils. Together with the conventional activities of sampling and analysis of soil profile were examined surveys meant to fractionation and characterization of SOC, in particular: Total Organic Carbon (TOC) and Total Extractable Carbon (TEC) soil contents were determined by Italian official method of soil analysis (Mi.P.A.F. (2000)). Different soil C fractions were also determined: Humic Acid Carbon (HAC), Fulvic Acid Carbon (FAC), Not Humic Carbon (NHC) and Humin Carbon (Huc) fractions were obtained by difference. In the whole profile, therefore, were also assayed cellulose and lignin contents. The aim of this work was to compare the distribution of different soil organic components in a podzol and a soil with andic properties. The data show great similarity, among the selected profiles, in the organic components distribution estudied. References: - Mi.P.A.F. - Ministero per le Politiche Agricole e Forestali - Osservatorio Nazionale Pedologico e per la Qualità del Suolo (2000): Metodi Ufficiali di Analisi Chimica del Suolo. In: Franco Angeli (Editor), Collana di metodi analitici per l'agricoltura diretta da Paolo Sequi, n. 1124.2, Milano, Italy. - Van Breemn N. and Buurman P. (1998) Chapter 12 Formation of Andisols. In: Soil formation. Kluwer Ed., Wageningen, The Netherlands, 271-289. -Ussiri D.A.N., Johnson C

  6. Criminalità e percezione della sicurezza a Pregnana Milanese. Uno studio di comunità

    Directory of Open Access Journals (Sweden)

    Ombretta Ingrascì

    2017-04-01

    Full Text Available L’articolo presenta i risultati di uno studio di comunità condotto dall’Osservatorio sulla Criminalità Organizzata dell’Università degli Studi di Milano riguardante la criminalità e la percezione della sicurezza a Pregnana Milanese, piccolo paese (7148 abitanti dell’hinterland milanese. Attraverso un approccio qualitativo (osservazione sul campo, interviste, focus group, integrato con l’analisi di dati statistici di tipo socio-economico e criminale, la ricerca ha ricostruito il tessuto socio-demografico, economico, urbanistico del paese, il panorama criminale e la percezione della sicurezza da parte della cittadinanza, e infine le risposte dell’amministrazione comunale di fronte alle sfide poste dalla criminalità e alle istanze di sicurezza avanzate dai cittadini.  I risultati dell’analisi mettono in luce l’assenza di processi di radicamento mafioso e attribuiscono la refrattarietà a tale fenomeno principalmente all’efficacia delle politiche locali, che hanno permesso alle istituzioni di “occupare” il territorio, così da non lasciare spazi vuoti che avrebbero potuto offrire alle mafie opportunità di infiltrazione e insediamento, così come accaduto in alcuni Comuni limitrofi. Parole chiave: Criminalità, percezione della sicurezza, mafia, comunità, politiche locali, controllo, territorio   The article shows the results of a community study carried out by the Monitoring Centre on Organized Crime of the University of Milan concerning the criminality and the perception of security in Pregnana Milanese, a little town of Milan’s hinterland. Throughout a qualitative approach (field observation, interviews, focus group, along with the analysis of socio-economic and criminal statistical data, the research has reconstructed the socio-demographic, economic, urbanistic fabric of the town, the criminal scenario and the citizens’ perception of security, and finally the responses of the local institutions to the challenges

  7. The Importance of Cultural Heritage in Earth Science

    Science.gov (United States)

    Avvisati, Gala; Di Vito, Mauro; Marotta, Enrica; Sangianantoni, Agata; Peluso, Rosario; de Vita, Sandro; Nave, Rosella; Vertechi, Enrico; De Natale, Giuseppe; Ghilardi, Massimo

    2016-04-01

    In recent years the Earth Sciences community is facing the need to achieve a more effective and efficient dissemination of its scientific culture. There is now a growing needing to integrate the use of "traditional" dissemination media of cultural heritage with the new digital technologies. Getting people involved in geoheritage site's activities represents a crucial issue in order to better communicate and increase the collective awareness of natural hazards, risk, and environmental change. The Reale Osservatorio Vesuviano (ROV) which is part of the Istituto Nazionale di Geofisica e Vulcanologia (INGV), owns collections unique in their combination of scientific, historical and artistic importance. The long history of ROV is extensively documented in its collections. This heritage - of great scientific and cultural value and unique for its abundance and variety - tells the story of the first observatory in the world, closely linked to the activity of Vesuvius, and the commitment of many scientists who dedicated their lives to study the volcano. The collections include: a) old books on volcanological matters, b) collection of rocks, minerals, volcanic ash and other materials from historical eruptions of Vesuvius, c) recordings on smoked paper of Vesuvius seismic activity from 1915 until 1970, d) scientific instruments, e) geological and geomorphological maps and models, f) vintage photographs and filmed sequences of eruptions, g) gouaches of Vesuvius and h) lava medals. The exposition of these collections, improved with the new digital contents, may trace new and unexplored routes for the dissemination of Earth Sciences related culture. The ethical duty of the ROV is the creation of an universal identity by taking a picture of the evolution of the society through the training of the culture of seismic and volcanic risk. A disappearance of its heritage could represent an huge impoverishment of its community: the ROV carries in fact the cultural identity of the

  8. [Screening for colorectal cancer in Italy, 2010 survey].

    Science.gov (United States)

    Zorzi, Manuel; Fedato, Chiara; Grazzini, Grazia; Sassoli de' Bianchi, Priscilla; Naldoni, Carlo; Pendenza, Melania; Sassatelli, Romano; Senore, Carlo; Visioli, Carmen Beatriz; Zappa, Marco

    2012-01-01

    We present the main results of the 2010 survey of the Italian screening programmes for colorectal cancer carried out by the National centre for screening monitoring (Osservatorio nazionale screening, ONS) on behalf of the Ministry of health. By the end of 2010, 105 programmes were active, 9 of which had been activated during the year, and 65% of Italians aged 50-69 years were residing in areas covered by organised screening programmes (theoretical extension). Twelve regions had their whole population covered. In the South of Italy and Islands, 5 new programmes were activated in 2010, with a theoretical extension of 29%. The majority of programmes employed the faecal occult blood test (FIT), while some adopted flexible sigmoidoscopy (FS) once in a lifetime and FIT for non-responders to FS. Overall, about 3,404,000 subjects were invited to undergo FIT, 47.2% of those to be invited within the year. The adjusted attendance rate was 48% and approximately 1,568,796 subjects were screened. Large differences in the attendance rate were observed among regions: 10% of programmes reported values lower than 24%. Positivity rate of FIT programmes was 5.5% at first screening (range: 1.6-11.3%) and 4.3% at repeat screening (range: 3.2-6.7%). The average attendance rate to total colonoscopy (TC) was 81.4% and in one region it was lower than 70%. Completion rate for total colonoscopy (TC) was 88.7%. Among the 740,281 subjects attending screening for the first time, the detection rate (DR) per 1,000 screened subjects was 2.4 for invasive cancer and 10.3 for advanced adenomas (AA - adenomas with a diameter ≥1 cm, with villous/tubulo-villous type or with high-grade dysplasia). As expected, the corresponding figures in the 843,204 subjects at repeat screening were lower (1.2‰ and 7.6‰ for invasive cancer and AA, respectively). The DR of cancer and adenomas increased with age and was higher among males. Many programmes reported some difficulties in guaranteeing TC in the

  9. Survey on attitudes of Italian pediatricians toward cough

    Directory of Open Access Journals (Sweden)

    Zanasi A

    2017-03-01

    Full Text Available Alessandro Zanasi,1 Luigi Morcaldi,2 Salvatore Cazzato,3 Massimiliano Mazzolini,4 Marzia Lecchi,5 Antonio Maria Morselli-Labate,6 Marianna Mastroroberto,6 Roberto W Dal Negro7 1Italian Association for Cough Study, Bologna, 2National Observatory of Health in Childhood and Adolescence (PAIDOSS: Osservatorio Nazionale sulla Salute dell’Infanzia e dell’Adolescenza, Rome, 3Department of Pediatrics, Salesi Children’s Hospital, Ancona, 4Department of Specialist, Diagnostic and Experimental Medicine, Respiratory and Critical Care Unit, S.Orsola-Malpighi Hospital, University of Bologna, Bologna, 5Department of Biotechnology and Biosciences, University of Milan Bicocca, Milan, 6Department of Medical and Surgical Sciences, Alma Mater Studiorum, University of Bologna, Bologna, 7National Centre for Respiratory Pharmacoeconomics and Pharmacoepidemiology, Verona, Italy Context: Children’s cough is a daily concern for most pediatricians. The management of both acute and chronic cough requires a systematic and comprehensive approach. Despite the approved protocols for management, the pediatric assessment of cough and the corresponding prescribing attitude frequently do not fit these protocols, which can be affected by parental suggestions – sometimes substantially. Objective: The objective of this study was to investigate both the perception and the behavior of a representative sample of Italian pediatricians toward cough in real life. Methods: A specific questionnaire consisting of 18 questions was prepared. The questionnaire was completed by 300 pediatricians (all members of PAIDOSS: Italian National Observatory on Health of Childhood and Adolescence who represented ~300,000 children. Results: A vast majority of children have cough throughout the year (99.3% of respondents have cough during autumn/winter and 64.7% in spring/summer. Allergic disease is the most frequent suspected cause of chronic cough in children (53%, and this is supported by the

  10. The Vesuvius/Campi Flegrei Supersite: state of the art and future perspectives

    Science.gov (United States)

    Borgstrom, Sven; Del Gaudio, Carlo; De Martino, Prospero; Prats-Iraola, Pau; Nannini, Matteo; Vecchioli, Francesco; Minati, Federico; Costantini, Mario; Stramondo, Salvatore; Bignami, Christian; Polcari, Marco; Fabrizia Buongiorno, Maria; Silvestri, Malvina; Pepe, Antonio; Pepe, Susi; Solaro, Giuseppe; Tizzani, Pietro; Siniscalchi, Valeria

    2017-04-01

    The Vesuvius/Campi Flegrei Supersite was established in April, 2014 with the aim of improving monitoring and knowledge of one of the areas with the highest volcanic risk worldwide, due to the strong urbanization of the city of Naples and surroundings, lying between two active volcanoes: Vesuvius on the east and Campi Flegrei on the west, this latter with a recorded uplift of about 35 centimeters from 2011 to date. Such deformation suggested to the Italian Civil Protection Department (ICPD) to move from the base (green) alert level to attention (yellow) level in the framework of the Campi Flegrei National Emergency Plan. In the first 2014-2016 biennial period, relevant results were carried out by the Supersite Science Team, apart from the outcomes of the ESA-SEOM INSARAP (Sentinel-1 INSAR Performance Study with TOPS data) project. Results are mainly focused on InSAR (S1-A, CSK, TSX) data processing, exploiting both SBAS and PS Interferometry over the Neapolitan volcanoes, with generation of ground deformation time series and comparison between LOS/inverted (E-W, vertical) InSAR and geodetic data, these latter from the INGV-Osservatorio Vesuviano monitoring networks. After the first biennial period, a detailed report on the Supersite activities has been submitted and approved by CEOS for satellite data provision for the next 2016-2018 period. Besides the continuation of the work in progress, future steps will consist in a detailed InSAR study of Vesuvius, mainly in the upper coherent part of the volcano, in order to characterize the area of interest from the engineering geology point of view. Moreover, DLR is planning an airborne campaign with their F-SAR sensor over Campi Flegrei; the contribution from INGV-OV to this campaign will consist in validating InSAR measurements with continuous GPS (cGPS) data. The campaign will take place around May and then again in 2018. With regard to the societal benefits of the current activities of the Supersite, the main

  11. A new data logger for integrated geophysical monitoring

    Science.gov (United States)

    Orazi, Massimo; Peluso, Rosario; Caputo, Antonio; Giudicepietro, Flora; Martini, Marcello

    2015-04-01

    GILDA digital recorder is a data logger developed at Osservatorio Vesuviano (INGV). It provides excellent data quality with low power consumption and low production cost. It is widely used in the multi-parametric monitoring networks of Neapolitan volcanoes and Stromboli volcano. We have improved the characteristics of GILDA recorder to realize a robust user-oriented acquisition system for integrated geophysical monitoring. We have designed and implemented new capabilities concerning the use of the low rate channels to get data of environmental parameters of the station. We also improved the stand-alone version of the data logger. This version can be particularly useful for scientific experiments and to rapidly upgrade permanent monitoring networks. Furthermore, the local storage can be used as back-up for the monitoring systems in continuous transmission, in case of failure of the transmission system. Some firmware changes have been made in order to improve the performance of the instrument. In particular, the low rate acquisition channels were conditioned to acquire internal parameters of the recorder such as the temperature and voltage. A prototype of the new version of the logger is currently installed at Campi Flegrei for a experimental application. Our experiment is aimed at testing the new version of GILDA data logger in multi-board configuration for multiparametric acquisitions. A second objective of the experiment is the comparison of the recorded data with geochemical data acquired by a multiparametric geochemical station to investigate possible correlations between seismic and geochemical parameters. The target site of the experiment is "Bocca Grande" fumarole in Solfatara volcano. By exploiting the modularity of GILDA, for the experiment has been realized an acquisition system based on three dataloggers for a total of 12 available channels. One of GILDA recorders is the Master and the other two are Slaves. The Master is responsible for the initial

  12. Observatory response to a volcanic crisis: the Campi Flegrei simulation exercise

    Science.gov (United States)

    Papale, Paolo; De Natale, Giuseppe

    2015-04-01

    In Febraury 2014 a simulation exercise was conducted at Campi Flegrei, Italy, in order to test the scientific response capabilities and the effectiveness of communication with Civil Protection authorities. The simulation was organized in the frame of the EU-VUELCO project, and involved the participation of the Osservatorio Vesuviano of INGV (INGV-OV) corroborated by other INGV scientists involved for their specific competencies; and the Italian Civil Protection, which was supported by an expert team formed by selected experts from the Italian academy and by VUELCO scientists from several EU and Latin American countries. The simulation included a previously appointed group of four volcanologists covering a range of expertise in volcano seismology, geodesy, geochemistry, and with experience both on the Campi Flegrei system and on other volcanic systems and crises in the world. The duty of this 'volcano team' was that of producing consistent sets of signals, that were sent to INGV-OV at the beginning of each simulation phase. In turn, the observatory response was that of i) immediately communicate the relevant observations to the Civil Protection; ii) analyze the synthetic signals and observations and extract a consistent picture and interpretation, including the analysis and quantification of uncertainties; iii) organize all the information produced in a bulletin, that was sent to the Civil Protection at the end of each simulation phase and that contained, according to national established agreements, a) the information available, and b) its interpretation including forecasts on the possible medium-short term evolution. The test included four simulation phases and it was blind, as only the volcano team knew the evolution and the final outcome; the volcano team was located at the INGV buildings in Rome, far from INGV-OV in Naples and the Civil Protection Dept. still in Rome, and with no contacts with any of them for the entire duration of the simulation. In this

  13. Improvement of ash plume monitoring, modeling and hazard assessment in the MED-SUV project

    Science.gov (United States)

    Coltelli, Mauro; Andronico, Daniele; Boselli, Antonella; Corradini, Stefano; Costa, Antonio; Donnadieu, Franck; Leto, Giuseppe; Macedonio, Giovanni; Merucci, Luca; Neri, Augusto; Pecora, Emilio; Prestifilippo, Michele; Scarlato, Piergiorgio; Scollo, Simona; Spinelli, Nicola; Spata, Gaetano; Taddeucci, Jacopo; Wang, Xuan; Zanmar Sanchez, Ricardo

    2014-05-01

    Volcanic ash clouds produced by explosive eruptions represent a strong problem for civil aviation, road transportation and other human activities. Since Etna volcano produced in the last 35 years more the 200 explosive eruptions of small and medium size. The INGV, liable for its volcano monitoring, developed since 2006 a specific system for forecasting and monitoring Etna's volcanic ash plumes in collaboration with several national and international institutions. Between 12 January 2011 and 31 December 2013 Etna produced forty-six basaltic lava fountains. Every paroxysm produced an eruption column ranging from a few up to eleven kilometers of height above sea level. The ash cloud contaminated the controlled airspace (CTR) of Catania and Reggio Calabria airports and caused tephra fallout on eastern Sicily sometime disrupting the operations of these airports. In order to give prompt and detailed warnings to the Aviation and Civil Protection authorities, ash plumes monitoring at Osservatorio Etneo, the INGV department in Catania, is carried out using multispectral (from visible to infrared) satellite and ground-based video-surveillance images; seismic and infrasound signals processed in real-time, a Doppler RADAR (Voldorad IIB) able to detect the eruption column in all weather conditions and a LIDAR (AMPLE) for retrieving backscattering and depolarization values of the ash clouds. Forecasting is performed running tephra dispersal models using weather forecast data, and then plotting results on maps published on a dedicated website. 24/7 Control Room operators were able to timely inform Aviation and Civil Protection operators for an effective aviation safety management. A variety of multidisciplinary activities are planned in the MED-SUV project with reference to volcanic ash observations and studies. These include: 1) physical and analogue laboratory experiments on ash dispersal and aggregation; 2) integration of satellite data (e.g. METEOSAT, MODIS) and ground

  14. R Aqr observing campaign

    Science.gov (United States)

    Waagen, Elizabeth O.

    2016-01-01

    Dr. George Wallerstein (University of Washington) has requested AAVSO coverage of the long period/symbiotic variable R Aquarii beginning immediately in support of high resolution spectroscopic observations planned for 2016 January 19 and 21. Several other astronomers, including Drs. Lee Anne Willson (Iowa State University), Ulisse Munari (INAF, Astronomical Observatory of Padua, Italy), and Fred Walter (Stony Brook University) are studying R Aqr closely and additional spectroscopic and other observations are planned for the near future. R Aqr is both a Mira (M) and a symbiotic (ZAND) - it is a close binary system consisting of a hot star and a late-type star (the Mira), both enveloped in nebulosity. As a result, the very interesting light curve shows not only the Mira pulsation but also complex eclipse behavior as the two stars interact. The period of Mira variation is 387.0 days; the eclipse period is 43.6-44 years. The cause of the eclipse is unknown; several theories h! ave been proposed, including a focused accretion stream, a disk or cloud around the secondary, and a triggered mass loss that produces an opaque cloud. Careful investigation of this upcoming event should help to resolve this question. The last eclipse of R Aqr was in 1978. The next eclipse is predicted for 2022, but may be early. The current behavior of R Aqr suggests that the eclipse, which lasts for several years, may either be beginning or its beginning may be imminent. R Aqr was at minimum in early December 2015 at magnitude V=11.4, and is currently at visual magnitude 11.0. During this phase of the approximately 44-year eclipse cycle, at maximum it may be as bright as V 6.0-6.5 but is not expected to become brighter. Beginning immediately, nightly BVRI CCD and DSLR photometry and visual observations are requested. As R Aqr brightens towards maximum and is in range, PEP observations are also requested. Ongoing spectroscopy over the next several years will be interesting to see as the system

  15. The K2 M67 Study: A Curiously Young Star in an Eclipsing Binary in an Old Open Cluster

    Science.gov (United States)

    Sandquist, Eric L.; Mathieu, Robert D.; Quinn, Samuel N.; Pollack, Maxwell L.; Latham, David W.; Brown, Timothy M.; Esselstein, Rebecca; Aigrain, Suzanne; Parviainen, Hannu; Vanderburg, Andrew; Stello, Dennis; Somers, Garrett; Pinsonneault, Marc H.; Tayar, Jamie; Orosz, Jerome A.; Bedin, Luigi R.; Libralato, Mattia; Malavolta, Luca; Nardiello, Domenico

    2018-04-01

    Galileo (TNG), operated on the island of La Palma by the INAF Fundacion Galileo Galilei (Spanish Observatory of Roque de los Muchachos of the IAC); and the Las Cumbres Observatory Global Telescope network.

  16. Transmission spectroscopy of the hot Jupiter TrES-3 b: Disproof of an overly large Rayleigh-like feature

    Science.gov (United States)

    Mackebrandt, F.; Mallonn, M.; Ohlert, J. M.; Granzer, T.; Lalitha, S.; García Muñoz, A.; Gibson, N. P.; Lee, J. W.; Sozzetti, A.; Turner, J. D.; Vaňko, M.; Strassmeier, K. G.

    2017-12-01

    the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.Newly observed photometric data from Sects. 2.2 and 2.3 and tables of the lightcurves are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/608/A26

  17. Aplanatic telescopes based on Schwarzschild optical configuration: from grazing incidence Wolter-like x-ray optics to Cherenkov two-mirror normal incidence telescopes

    Science.gov (United States)

    Sironi, Giorgia

    2017-09-01

    At the beginning of XX century Karl Schwarzschild defined a method to design large-field aplanatic telescopes based on the use of two aspheric mirrors. The approach was then refined by Couder (1926) who, in order to correct for the astigmatic aberration, introduced a curvature of the focal plane. By the way, the realization of normal-incidence telescopes implementing the Schwarzschild aplanatic configuration has been historically limited by the lack of technological solutions to manufacture and test aspheric mirrors. On the other hand, the Schwarzschild solution was recovered for the realization of coma-free X-ray grazing incidence optics. Wolter-like grazing incidence systems are indeed free of spherical aberration, but still suffer from coma and higher order aberrations degrading the imaging capability for off-axis sources. The application of the Schwarzschild's solution to X-ray optics allowed Wolter to define an optical system that exactly obeys the Abbe sine condition, eliminating coma completely. Therefore these systems are named Wolter-Schwarzschild telescopes and have been used to implement wide-field X-ray telescopes like the ROSAT WFC and the SOHO X-ray telescope. Starting from this approach, a new class of X-ray optical system was proposed by Burrows, Burg and Giacconi assuming polynomials numerically optimized to get a flat field of view response and applied by Conconi to the wide field x-ray telescope (WFXT) design. The Schwarzschild-Couder solution has been recently re-discovered for the application to normal-incidence Cherenkov telescopes, thanks to the suggestion by Vassiliev and collaborators. The Italian Institute for Astrophysics (INAF) realized the first Cherenkov telescope based on the polynomial variation of the Schwarzschild configuration (the so-called ASTRI telescope). Its optical qualification was successfully completed in 2016, demonstrating the suitability of the Schwarzschild-like configuration for the Cherenkov astronomy requirements

  18. HD 144548: A young triply eclipsing system in the Upper Scorpius OB association

    Science.gov (United States)

    Alonso, R.; Deeg, H. J.; Hoyer, S.; Lodieu, N.; Palle, E.; Sanchis-Ojeda, R.

    2015-12-01

    The star HD 144548 (=HIP 78977; TYP 6212-1273-1) has been known as a detached eclipsing binary and a bona-fide member of the Upper Scorpius OB association. Continuous photometry from the K2 mission on Campaign Two has revealed the presence of additional eclipses due to the presence of a third star in the system. These are explained by a system composed of the two previously known members of the eclipsing system (Ba and Bb) with a period of 1.63 d, orbiting around an F7-F8V star with a period of 33.945 ± 0.002 d in an eccentric orbit (eA = 0.2652 ± 0.0003). The timing of the eclipses of Ba and Bb reveals the same 33.9 d periodicity, which we interpret as the combination of a light time effect combined with dynamical perturbations on the close system. Here we combine radial velocities and analytical approximations for the timing of the eclipses to derive masses and radii for the three components of the system. We obtain a mass of 1.44 ± 0.04 M⊙ and radius of 2.41 ± 0.03 R⊙ for the A component, and almost identical masses and radii of about 0.96 M⊙ and 1.33 R⊙ for each of the two components of the close binary. HD 144548 is the first triply eclipsing system for which radial velocities of all components could be measured. Partially based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated by the Fundación Galileo Galilei of the INAF, the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association, and the William Herschel Telescope (programme DDT58 - PI Lodieu) operated by the Isaac Newton Group on the island of La Palma at the Spanish Observatorio Roque de los Muchachos of the IAC. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.Appendices are available in electronic form at http://www.aanda.org

  19. The VIMOS Public Extragalactic Redshift Survey (VIPERS). The distinct build-up of dense and normal massive passive galaxies

    Science.gov (United States)

    Gargiulo, A.; Bolzonella, M.; Scodeggio, M.; Krywult, J.; De Lucia, G.; Guzzo, L.; Garilli, B.; Granett, B. R.; de la Torre, S.; Abbas, U.; Adami, C.; Arnouts, S.; Bottini, D.; Cappi, A.; Cucciati, O.; Davidzon, I.; Franzetti, P.; Fritz, A.; Haines, C.; Hawken, A. J.; Iovino, A.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marulli, F.; Moutard, T.; Polletta, M.; Pollo, A.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Zamorani, G.; Bel, J.; Branchini, E.; Coupon, J.; Ilbert, O.; Moscardini, L.; Peacock, J. A.

    2017-10-01

    project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS web site is http://www.vipers.inaf.it/

  20. Characterization of Earth as an exoplanet on the basis of VIRTIS-Venus Express data analysis.

    Science.gov (United States)

    Oliva, Fabrizio; Piccioni, Giuseppe; D'Aversa, Emiliano; Bellucci, Giancarlo; Sindoni, Giuseppe; Grassi, Davide; Filacchione, Gianrico; Tosi, Federico; Capaccioni, Fabrizio

    2017-04-01

    The Visible and InfraRed Thermal Imaging Spectrometer (VIRTIS, Piccioni et al., 2007) on board the Venus Express spacecraft observed the planet Earth several times in the course of the mission. In particular, a subset of 48 observations has been taken from a distance at which our planet is imaged at sub-pixel size, as exoplanets are observed using current technologies. We studied this full subset to understand which spectral signatures, related to different surface and cloud types, can be identified from the integrated planet spectrum. As expected, we found that the cloud coverage has a key role in the identification of surface features and that vegetation is very difficult to be detected. To validate our results we built a simple tool capable to simulate observations of an Earth-like planet as seen from a VIRTIS-like spectrometer in the 0.3 - 5.0 μm range. The illumination and viewing geometries, along with the spectrometer instantaneous field of view and spectral grid and sampling, can be defined by the user. The spectral endmembers used to generate the planet have been selected from an observation of Earth registered from the instrument VIRTIS on board the ESA mission Rosetta, with similar characteristics, during the third flyby of the spacecraft around our planet, occurred in November 2009. Hence, we simulated planets made of: vegetation, desert, ocean, water ice clouds and liquid water clouds. Using different amounts for each spectral class we inferred the percentages that are required to identify each class when all the spectral information is integrated into a single pixel. The outcome of this analysis confirms that clouds are not a negligible issue in the research for spectral signatures, in particular those related to the habitability of a planet and its climate conditions, even when the cloud coverage is not so high. Acknowledgements: This study has been performed within the WOW project financed by INAF and thanks to the support from the Italian Space

  1. Pursuing the link between Scientific Research and Communication: the experience of the OAVdA and the Planetarium in the Aosta Valley

    Science.gov (United States)

    Ettore Bernagozzi, Andrea; Bertolini, Enzo; Calcidese, Paolo; Carbognani, Albino; Carlo Cenadelli, Davide; Christille, Jean Marc; Pellissier, Paolo; Recaldini, Paolo; Soldi, Matteo

    2015-08-01

    The Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA) and the Planetarium of Lignan are located in the Saint-Barthélemy Valley, in the Italian Alps at the border with France and Switzerland. They are managed by the non-profit organisation Fondazione Clément Fillietroz-ONLUS. The OAVdA opened in 2003, then the Planetarium followed in 2009.Scientific Research has been the main activity at the OAVdA since 2006, when an official agreement of cooperation was set up with the Italian National Institute for Astrophysics (INAF). Scientific Research made at the OAVdA contributes greatly to the development of high quality Public Outreach and Education programs. We adopt the principle that knowledge teachers and students meet in school is the result of scientific researches made by scientists in the past; then, knowledge they will meet in life tomorrow is the result of scientific researches that scientists are making today. To put this in practice, researchers are effectively involved, for at least 30% of their working time, in a vast spectrum of Public Outreach and Education initiatives where they illustrate several aspects of their work.In the presentation we explain why the theoretical framework informing our Public Outreach and Education programs was identified and how it has caused, after almost 10 years, a major change in the perception of the OAVdA and the Planetarium by all the stakeholders: institutional funding sources, other funding sources, participants to the initiatives (both schools and public at large), media, the researchers themselves. Among the activities, we report about three experiences strongly based on the establishment of a 'virtuous link' between Research and Communication: the Summer School in Astronomy in Saint-Barthélemy (targeted to public at large); "Saint-Roch Etoiles", a 5-year project with the Saint-Roch School in Aosta (students aged 5-12); the ESO Astronomy Camp co-organised in Lignan with the European Southern

  2. The Sardinia Radio Telescope . From a technological project to a radio observatory

    Science.gov (United States)

    Prandoni, I.; Murgia, M.; Tarchi, A.; Burgay, M.; Castangia, P.; Egron, E.; Govoni, F.; Pellizzoni, A.; Ricci, R.; Righini, S.; Bartolini, M.; Casu, S.; Corongiu, A.; Iacolina, M. N.; Melis, A.; Nasir, F. T.; Orlati, A.; Perrodin, D.; Poppi, S.; Trois, A.; Vacca, V.; Zanichelli, A.; Bachetti, M.; Buttu, M.; Comoretto, G.; Concu, R.; Fara, A.; Gaudiomonte, F.; Loi, F.; Migoni, C.; Orfei, A.; Pilia, M.; Bolli, P.; Carretti, E.; D'Amico, N.; Guidetti, D.; Loru, S.; Massi, F.; Pisanu, T.; Porceddu, I.; Ridolfi, A.; Serra, G.; Stanghellini, C.; Tiburzi, C.; Tingay, S.; Valente, G.

    2017-12-01

    Context. The Sardinia Radio Telescope (SRT) is the new 64 m dish operated by the Italian National Institute for Astrophysics (INAF). Its active surface, comprised of 1008 separate aluminium panels supported by electromechanical actuators, will allow us to observe at frequencies of up to 116 GHz. At the moment, three receivers, one per focal position, have been installed and tested: a 7-beam K-band receiver, a mono-feed C-band receiver, and a coaxial dual-feed L/P band receiver. The SRT was officially opened in September 2013, upon completion of its technical commissioning phase. In this paper, we provide an overview of the main science drivers for the SRT, describe the main outcomes from the scientific commissioning of the telescope, and discuss a set of observations demonstrating the scientific capabilities of the SRT. Aims: The scientific commissioning phase, carried out in the 2012-2015 period, proceeded in stages following the implementation and/or fine-tuning of advanced subsystems such as the active surface, the derotator, new releases of the acquisition software, etc. One of the main objectives of scientific commissioning was the identification of deficiencies in the instrumentation and/or in the telescope subsystems for further optimization. As a result, the overall telescope performance has been significantly improved. Methods: As part of the scientific commissioning activities, different observing modes were tested and validated, and the first astronomical observations were carried out to demonstrate the science capabilities of the SRT. In addition, we developed astronomer-oriented software tools to support future observers on site. In the following, we refer to the overall scientific commissioning and software development activities as astronomical validation. Results: The astronomical validation activities were prioritized based on technical readiness and scientific impact. The highest priority was to make the SRT available for joint observations as

  3. Modular VO oriented Java EE service deployer

    Science.gov (United States)

    Molinaro, Marco; Cepparo, Francesco; De Marco, Marco; Knapic, Cristina; Apollo, Pietro; Smareglia, Riccardo

    2014-07-01

    The International Virtual Observatory Alliance (IVOA) has produced many standards and recommendations whose aim is to generate an architecture that starts from astrophysical resources, in a general sense, and ends up in deployed consumable services (that are themselves astrophysical resources). Focusing on the Data Access Layer (DAL) system architecture, that these standards define, in the last years a web based application has been developed and maintained at INAF-OATs IA2 (Italian National institute for Astrophysics - Astronomical Observatory of Trieste, Italian center of Astronomical Archives) to try to deploy and manage multiple VO (Virtual Observatory) services in a uniform way: VO-Dance. However a set of criticalities have arisen since when the VO-Dance idea has been produced, plus some major changes underwent and are undergoing at the IVOA DAL layer (and related standards): this urged IA2 to identify a new solution for its own service layer. Keeping on the basic ideas from VO-Dance (simple service configuration, service instantiation at call time and modularity) while switching to different software technologies (e.g. dismissing Java Reflection in favour of Enterprise Java Bean, EJB, based solution), the new solution has been sketched out and tested for feasibility. Here we present the results originating from this test study. The main constraints for this new project come from various fields. A better homogenized solution rising from IVOA DAL standards: for example the new DALI (Data Access Layer Interface) specification that acts as a common interface system for previous and oncoming access protocols. The need for a modular system where each component is based upon a single VO specification allowing services to rely on common capabilities instead of homogenizing them inside service components directly. The search for a scalable system that takes advantage from distributed systems. The constraints find answer in the adopted solutions hereafter sketched. The

  4. HADES RV Programme with HARPS-N at TNG. VI. GJ 3942 b behind dominant activity signals

    Science.gov (United States)

    Perger, M.; Ribas, I.; Damasso, M.; Morales, J. C.; Affer, L.; Suárez Mascareño, A.; Micela, G.; Maldonado, J.; González Hernández, J. I.; Rebolo, R.; Scandariato, G.; Leto, G.; Zanmar Sanchez, R.; Benatti, S.; Bignamini, A.; Borsa, F.; Carbognani, A.; Claudi, R.; Desidera, S.; Esposito, M.; Lafarga, M.; Martinez Fiorenzano, A. F.; Herrero, E.; Molinari, E.; Nascimbeni, V.; Pagano, I.; Pedani, M.; Poretti, E.; Rainer, M.; Rosich, A.; Sozzetti, A.; Toledo-Padrón, B.

    2017-12-01

    Context. Short- to mid-term magnetic phenomena on the stellar surface of M-type stars can resemble the effects of planets in radial velocity data, and may also hide them. Aims: We analyze 145 spectroscopic HARPS-N observations of GJ 3942 taken over the past five years and additional photometry in order to disentangle stellar activity effects from genuine Doppler signals as a result of the orbital motion of the star around the common barycenter with its planet. Methods: To achieve this, we use the common methods of pre-whitening, and treat the correlated red noise by a first-order moving average term and by Gaussian-process regression following an MCMC analysis. Results: We identify the rotational period of the star at 16.3 days and discover a new super-Earth, GJ 3942 b, with an orbital period of 6.9 days and a minimum mass of 7.1 M⊕. An additional signal in the periodogram of the residuals is present, but at this point we cannot claim with sufficient significance that it is related to a second planet. If confirmed, this planet candidate would have a minimum mass of 6.3 M⊕ and a period of 10.4 days, which might indicate a 3:2 mean-motion resonance with the inner planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF - Fundación Galileo Galilei at the Roque de los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); photometric observations from the APACHE array located at the Astronomical Observatory of the Aosta Valley; photometric observations made with the robotic APT2 (within the EXORAP program) located at Serra La Nave on Mt. Etna.Table 9 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A63

  5. MASSIV: Mass Assembly Survey with SINFONI in VVDS. IV. Fundamental relations of star-forming galaxies at 1 < z < 1.6

    Science.gov (United States)

    Vergani, D.; Epinat, B.; Contini, T.; Tasca, L.; Tresse, L.; Amram, P.; Garilli, B.; Kissler-Patig, M.; Le Fèvre, O.; Moultaka, J.; Paioro, L.; Queyrel, J.; López-Sanjuan, C.

    2012-10-01

    Programs 179.A-0823, 177.A-0837, 78.A-0177, 75.A-0318, and 70.A-9007. This work also benefits from data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.All the data published in this paper are publicly available following this link: http://cosmosdb.lambrate.inaf.it/VVDS-SINFONI

  6. The NEOShield-2 EU Project - The first year of the Italian contribution

    Science.gov (United States)

    Ieva, Simone; Dotto, Elisabetta; Mazzotta Epifani, Elena; Di Paola, Andrea; Speziali, Roberto; Lazzarin, Monica; Bertini, Ivano; Barucci, Maria Antonieta; Perna, Davide; Lazzaro, Daniela; Silva, Sergio; Monteiro, Filipe; Perozzi, Ettore; Micheli, Marco; Cortese, Matteo

    2016-10-01

    The population of Near Earth Asteroids (NEAs) is responsible for a continuous flux of impactors with our planet. To date, more than 14500 NEAs are known, with a current discovery rate of ˜1500 objects/year.The NEA population show a great diversity in terms of composition and physical properties: (different shapes, rotational states, rotational periods...). NEA diversity is also emphasized by the different taxonomic types found within the population that give some hints about the NEA surface composition.The study of their physical nature is compelling in view of the potential hazard posed to our planet, since it has been acknowledged that whatever the mitigation scenario, it strongly depends upon the composition of the impactor. Unfortunately, only less than 15% of them have been physically characterized, and at the current discovery rate the situation is becoming progressively worse.Within the framework of the Horizon 2020 program, the European Commission promoted the study of NEAs by approving and financing the NEOShield-2 project (2015-2017). One of the main aims of the NEOShield-2 project is to undertake an extensive observational campaign to provide physical and compositional characterization of a large number of NEAs in the 50-300 m size range.INAF-OAR and Padova University, the Italian contributors to the NEOShield-2 project, are responsible for the Task 10.2.1 'Colours and Phase function', with the aim to acquire photometric measurements for a wide sample of NEOs. An operational interface is maintained together with the ESA SSA-NEO Coordination Centre (NEOCC) in order to optimize observations devoted to physical characterization.We will present the results of the first year of the Italian contribution to the project on i) phase function analysis, ii) surface colors and iii) preliminary taxonomical classification and the statistical analysis of the data obtained from several telescopes around the world.This research has been funded with support from the

  7. JIRAM-Juno: Overview of Preliminary Results in the Study of Jupiter "Infrared-Bright" Areas

    Science.gov (United States)

    Grassi, Davide; Adriani, Alberto; Bolton, Scott J.

    2017-04-01

    The JIRAM instrument on board the Juno spacecraft includes a spectrometer channel that operates in the range 2-5 microns with a spectral resolution of about 15 nm. Data from this channel are particularly valuable in the study of bright IR regions, where the upper cloud decks are relatively thin and the thermal radiation emitted at pressures down to 3-5 bars can be measured by infrared remote-sensing instruments. Previous studies using NIMS-Galileo [1] and VIMS-Cassini [2] data, as well as a specific assessment for the JIRAM instrument [3], have demonstrated the possibility of constraining the water, ammonia and phosphine content using moderate-resolution spectra spanning the methane transparency window at 5 microns. While considerable efforts have been devoted to the study of brightest features - the so-called "Hot-Spots", located between the Equatorial zone and the North equatorial Belt - other prominent bright areas over the disk of Jupiter remain largely uninvestigated. This talk reviews preliminary results of the JIRAM observations acquired around the first Juno "perijove" (closest approach of Jupiter) after orbit insertion. In general terms, the retrieved contents of the gaseous species mentioned above agree with the global latitudinal trends presented in [3] and [4]. Nonetheless, in several instances, the spatial capabilities of JIRAM allow one to detect specific spatial trends, likely to be associated to dynamic regimes at regional scale. This work was supported by the Italian Space Agency through ASI-INAF contract I/010/10/0 and 2014-050-R.0. JIL acknowledges support from NASA through the Juno Project. GSO acknowledges support from NASA through funds that were distributed to the Jet Propulsion Laboratory, California Institute of Technology. [1] Irwin et al., 1998, doi:10.1029/98JE00948 [2] Giles et al., 2015, doi:10.1016/j.icarus.2015.05.030 [3] Grassi et al., 2010, doi:10.1016/j.pss.2010.05.003 [4] Giles et al., 2016, arXiv:1610.09073

  8. Modeling of the Inner Coma of Comet 67P/Churyumov-Gerasimenko Constrained by VIRTIS and ROSINA Observations

    Science.gov (United States)

    Fougere, N.; Combi, M. R.; Tenishev, V.; Bieler, A. M.; Migliorini, A.; Bockelée-Morvan, D.; Toth, G.; Huang, Z.; Gombosi, T. I.; Hansen, K. C.; Capaccioni, F.; Filacchione, G.; Piccioni, G.; Debout, V.; Erard, S.; Leyrat, C.; Fink, U.; Rubin, M.; Altwegg, K.; Tzou, C. Y.; Le Roy, L.; Calmonte, U.; Berthelier, J. J.; Rème, H.; Hässig, M.; Fuselier, S. A.; Fiethe, B.; De Keyser, J.

    2015-12-01

    by a consortium formed by Italy, France and Germany, under the scientific responsibility of the IAPS of INAF, which guides also the scientific operations. The consortium includes also the LESIA of the Observatoire de Paris, and the Institut für Planetenforschung of DLR. The authors wish to thank the RSGS and the RMOC for their continuous support.

  9. Modeling of the VIRTIS-M Observations of the Coma of Comet 67P/Churyumov-Gerasimenko

    Science.gov (United States)

    Fougere, Nicolas; Combi, Michael R.; Tenishev, Valeriy; Bieler, Andre; Migliorini, Alessandra; Piccioni, Giuseppe; Capaccioni, Fabrizio; Filacchione, Gianrico; Toth, Gabor; Huang, Zhenguang; Gombosi, Tamas; Hansen, Kenneth; Bockelee-Morvan, Dominique; Debout, Vincent; Erard, Stephane; Leyrat, Cedric; Fink, Uwe; Rubin, Martin; Altwegg, Kathrin; Tzou, Chia-Yu; Le Roy, Lena; Calmonte, Ursina; Berthelier, Jean-Jacques; Reme, Henri; Hassig, Myrtha; Fuselier, Stephen; Fiethe, Bjorn; De Keyser, Johan

    2015-11-01

    The recent images of the inner coma of 67P/Churyumov-Gerasimenko (CG) made by the infrared channel of the VIRTIS-M instrument on board the Rosetta spacecraft show the gas distribution as it expands in the coma (Migliorini et al. 2015, DPS abstract).Since VIRTIS is a remote sensing instrument, a proper modeling of these observations requires the computation of the full coma of comet CG, which necessitates the use of a kinetic approach due to the rather low gas densities. Hence, we apply a Direct Simulation Monde Carlo (DSMC) method to solve the Boltzmann equation and describe CG’s coma from the nucleus surface up to a few hundreds of kilometers. The model uses the SHAP5 nucleus shape model from the OSIRIS team. The gas flux distribution takes into account solar illumination, including self-shadowing. The local activity at the surface of the nucleus is given by spherical harmonics expansion reproducing best the ROSINA-DFMS data. The densities from the DSMC model outputs are then integrated along the line-of-sight to create synthetic images that are directly comparable with the VIRTIS-M column density measurements.The good agreement between the observations and the model illustrates our continuously improving understanding of the physics of the coma of comet CG.AcknowledgementsWork at UofM was supported by contracts JPL#1266313, JPL#1266314 and NASA grant NNX09AB59G. Work at UoB was funded by the State of Bern, the Swiss National Science Foundation and by the European Space Agency PRODEX Program. Work at Southwest Research institute was supported by subcontract #1496541 from the JPL. Work at BIRA-IASB was supported by the Belgian Science Policy Office via PRODEX/ROSINA PEA 90020. The authors would like to thank ASI, CNES, DLR, NASA for supporting this research. VIRTIS was built by a consortium formed by Italy, France and Germany, under the scientific responsibility of the IAPS of INAF, which guides also the scientific operations. The consortium includes also the

  10. The WEBT Campaign on the Blazar 3C 279 in 2006

    Science.gov (United States)

    Böttcher, M.; Basu, S.; Joshi, M.; Villata, M.; Arai, A.; Aryan, N.; Asfandiyarov, I. M.; Bach, U.; Bachev, R.; Berduygin, A.; Blaek, M.; Buemi, C.; Castro-Tirado, A. J.; De Ugarte Postigo, A.; Frasca, A.; Fuhrmann, L.; Hagen-Thorn, V. A.; Henson, G.; Hovatta, T.; Hudec, R.; Ibrahimov, M.; Ishii, Y.; Ivanidze, R.; Jelínek, M.; Kamada, M.; Kapanadze, B.; Katsuura, M.; Kotaka, D.; Kovalev, Y. Y.; Kovalev, Yu. A.; Kubánek, P.; Kurosaki, M.; Kurtanidze, O.; Lähteenmäki, A.; Lanteri, L.; Larionov, V. M.; Larionova, L.; Lee, C.-U.; Leto, P.; Lindfors, E.; Marilli, E.; Marshall, K.; Miller, H. R.; Mingaliev, M. G.; Mirabal, N.; Mizoguchi, S.; Nakamura, K.; Nieppola, E.; Nikolashvili, M.; Nilsson, K.; Nishiyama, S.; Ohlert, J.; Osterman, M. A.; Pak, S.; Pasanen, M.; Peters, C. S.; Pursimo, T.; Raiteri, C. M.; Robertson, J.; Robertson, T.; Ryle, W. T.; Sadakane, K.; Sadun, A.; Sigua, L.; Sohn, B.-W.; Strigachev, A.; Sumitomo, N.; Takalo, L. O.; Tamesue, Y.; Tanaka, K.; Thorstensen, J. R.; Tosti, G.; Trigilio, C.; Umana, G.; Vennes, S.; Vitek, S.; Volvach, A.; Webb, J.; Yamanaka, M.; Yim, H.-S.

    2007-12-01

    The quasar 3C 279 was the target of an extensive multiwavelength monitoring campaign from 2006 January through April. An optical-IR-radio monitoring campaign by the Whole Earth Blazar Telescope (WEBT) collaboration was organized around target-of-opportunity X-ray and soft γ-ray observations with Chandra and INTEGRAL in 2006 mid-January, with additional X-ray coverage by RXTE and Swift XRT. In this paper we focus on the results of the WEBT campaign. The source exhibited substantial variability of optical flux and spectral shape, with a characteristic timescale of a few days. The variability patterns throughout the optical BVRI bands were very closely correlated with each other, while there was no obvious correlation between the optical and radio variability. After the ToO trigger, the optical flux underwent a remarkably clean quasi-exponential decay by about 1 mag, with a decay timescale of τd~12.8 days. In intriguing contrast to other (in particular, BL Lac type) blazars, we find a lag of shorter wavelength behind longer wavelength variability throughout the RVB wavelength ranges, with a time delay increasing with increasing frequency. Spectral hardening during flares appears delayed with respect to a rising optical flux. This, in combination with the very steep IR-optical continuum spectral index of α0~1.5-2.0, may indicate a highly oblique magnetic field configuration near the base of the jet, leading to inefficient particle acceleration and a very steep electron injection spectrum. An alternative explanation through a slow (timescale of several days) acceleration mechanism would require an unusually low magnetic field of B<~0.2 G, about an order of magnitude lower than inferred from previous analyses of simultaneous SEDs of 3C 279 and other flat-spectrum radio quasars with similar properties. For questions regarding the availability of the data from the WEBT campaign presented in this paper, please contact the WEBT President Massimo Villata at villata@oato.inaf.it.

  11. HADES RV Programme with HARPS-N at TNG. V. A super-Earth on the inner edge of the habitable zone of the nearby M dwarf GJ 625

    Science.gov (United States)

    Suárez Mascareño, A.; González Hernández, J. I.; Rebolo, R.; Velasco, S.; Toledo-Padrón, B.; Affer, L.; Perger, M.; Micela, G.; Ribas, I.; Maldonado, J.; Leto, G.; Zanmar Sanchez, R.; Scandariato, G.; Damasso, M.; Sozzetti, A.; Esposito, M.; Covino, E.; Maggio, A.; Lanza, A. F.; Desidera, S.; Rosich, A.; Bignamini, A.; Claudi, R.; Benatti, S.; Borsa, F.; Pedani, M.; Molinari, E.; Morales, J. C.; Herrero, E.; Lafarga, M.

    2017-09-01

    We report the discovery of a super-Earth orbiting at the inner edge of the habitable zone of the star GJ 625 based on the analysis of the radial-velocity (RV) time series from the HARPS-N spectrograph, consisting of 151 HARPS-N measurements taken over 3.5 yr. GJ 625 b is a planet with a minimum mass Msini of 2.82 ± 0.51 M⊕ with an orbital period of 14.628 ± 0.013 days at a distance of 0.078 AU from its parent star. The host star is the quiet M2 V star GJ 625, located at 6.5 pc from the Sun. We find the presence of a second radial-velocity signal in the range 74-85 days that we relate to stellar rotation after analysing the time series of Ca II H&K and Hα spectroscopic indicators, the variations of the FWHM of the CCF, and the APT2 photometric light curves. We find no evidence linking the short-period radial-velocity signal to any activity proxy. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF - Fundación Galileo Galilei at the Roche de Los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); photometric observations made with the robotic telescope APT2 (within the EXORAP programme) located at Serra La Nave on Mt. Etna; and lucky imaging observations made with the Telescopio Carlos Sánchez operated on the island of Tenerife by the Instituto de Astrofísica de Canarias in the Spanish Observatorio del Teide.Tables A.1-A.5 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/605/A92

  12. Guiding the Giant

    Science.gov (United States)

    1998-08-01

    . According to this, the Capodimonte Observatory will deliver to ESO a wide-field 2.6-m telescope, referred to as the VLT Survey Telescope (VST). The VST will be over 12 times more efficient than the 2.2-m telescope for survey work. When it goes into operation some years from now, ESO will consolidate its front-line position in wide-field imaging capabilities. Another survey, the DEep Near Infrared Southern Sky Survey (DENIS) , is now being carried out at La Silla. It is a joint European project that is conducted at the 1-m ESO telescope by a consortium of 20 astronomical institutes. More information Further information about EIS is available at http://www.eso.org/eis. From this site, it is possible to visit the EIS release page and to browse through pictures of the distant Universe and of individual objects, some of which will be observed with the VLT in the future. Notes [1] The home institutes of the astronomers involved in EIS include the European Southern Observatory, Osservatorio Astronomico di Trieste (Italy), Leiden Observatory (The Netherlands), Institut d'Astrophysique de Paris (France), Max-Planck Institut für Astrophysik (Germany), Astronomisk Observatorium (Copenhagen, Denmark), Istituto di Radioastronomia del CNR (Bologna, Italy), Landensternwarte Heidelberg-Königstuhl (Heidelberg, Germany), DAEC, Observatoire de Paris-Meudon (France), ESA/ESO Space Telescope-European Coordinating Facility (Garching, Germany), Osservatorio Astronomico di Pino Torinese, Torino (Italy) and Osservatorio Astronomico di Capodimonte (Napoli, Italy). [2] In astronomy, the redshift (z) denotes the fraction by which the lines in the spectrum of an object are shifted towards longer wavelengths. The observed redshift of a distant galaxy or quasar gives a direct estimate of the universal expansion (i.e. the `recession velocity'). Since this expansion rate increases with the distance, the velocity (and thus the redshift) is itself a function (the Hubble relation) of the distance to the

  13. Dust Measurements in the Coma of Comet 67P/Churyumov-Gerasimenko Inbound to the Sun Between 3.7 and 3.4 AU

    Science.gov (United States)

    Rotundi, Alessandra; Della Corte, Vincenzo; Fulle, Marco; Ferrari, Marco; Sordini, Roberto; Ivanovski, Stavro; Accolla, Mario; Lucarelli, Francesca; Zakharov, Vladimir; Mazzotta Epifani, Elena; López-Moreno, José J.; Rodríguez, Julio; Colangeli, Luigi; Palumbo, Pasquale; Bussoletti, Ezio; Crifo, Jean-Francois; Esposito, Francesca; Green, Simon F.; Grün, Eberhard; Lamy, Philippe L.

    2015-04-01

    data on grain speed and its optical cross section. The IS grain momentum measurement, when combined with the GDS detection time, provides a direct measurement of grain speed and mass. These combined measurements characterize single grain dust dynamics in the coma of 67P/CG. The first grain was detected on 1 August 2014 at 814 km from the comet nucleus. Between then and 13 Septem-ber 2014 GIADA detected 35 grains ranging in mass from ~ 5 x 10-10 to 8 x 10-8 kg. Including complementary data from the OSIRIS narrow angle camera, the dust mass loss was calculated over an additional three orders of magni-tude in mass, extending the ejected dust grain sizes up to 2 cm. Combined with data from the MIRO and the ROSINA instruments onboard Rosetta we find a dust/gas mass ratio of 4 +/- 2 averaged over the sunlit nucleus sur-face. The dust to gas ratio may change as the comet approaches closer to the Sun. Acknowledgments: GIADA was built by a consortium led by the Univ. Napoli "Parthenope" & INAF- Oss. Astr. Capodimonte, in collabo-ration with the Inst. de Astrofisica de Andalucia, Selex-ES, FI and SENER. GIADA is presently managed & operated by Ist. di Astrofisica e Planetologia Spaziali-INAF, IT. GIADA was funded and managed by the Agenzia Spaziale Italiana, IT, with the support of the Spanish Ministry of Education and Science MEC, ES. GIADA was developed from a PI proposal from the University of Kent; sci. & tech. contribution were pro-vided by CISAS, IT, Lab. d'Astr. Spat., FR, and Institutions from UK, IT, FR, DE and USA. We thank the RSGS/ESAC, RMOC/ESOC & Rosetta Project/ESTEC for their outstanding work. Science support provided was by NASA through the US Rosetta Project managed by the Jet Propulsion Laboratory/California Institute of Technology. GIADA calibrated data will be available through ESA's PSA web site(www.rssd.esa.int/index.php?project=PSA&page=in dex). We would like to thank Angioletta Coradini for her contribution as a GIADA Co-I. We thank the MIRO, OSIRIS and

  14. New opportunities in planetary geomorphology: an assessment of the capabilities of the Colour and Stereo Surface Imaging System (CaSSIS) on The Exomars Trace Gas Orbiter through Image Simulation.

    Science.gov (United States)

    Tornabene, Livio Leonardo; Seelos, Frank; Pommerol, Antoine; Thomas, Nick; Caudill, Christy; Conway, Susan J.

    2017-04-01

    single-band images, or when missed by the HiRISE colour swath. Another result based on our colour analysis includes, excellent separation of ferrous- and ferric-bearing surface materials provided by band ratio colour composite images utilizing the two NIR bands of CaSSIS (3RED, 4NIR). These images will be particularly useful for associating CaSSIS colour units with spectral units defined by orbiting spectrometers (e.g., CRISM), and thereby extend spectral mapping to CaSSIS spatial scales. This will particularly be beneficial for landing sites where it is difficult to achieve continuous colour coverage with HiRISE. Our analysis shows that dune movement can be detected at the scale of CaSSIS, given a long enough baseline. Other results include resolving: 1) larger individual or sets of Recurring Slope Lineae (RSL), 2) small impacts (including ice excavators), and 3) surface changes associated with landers/rovers (NOTE: lander/rovers and their tracks are not resolvable). References: [1] Thomas N. et al. (2016), submitted to SSR. [2] Tornabene L. et al. (2017), submitted to SSR. [3] Tornabene L. et al. (2016) LPSC 47, Abstract #2695. [4] Vago J. et al. (2015) SSR, 49 518-528. [5] Cremonese G. et al. (2017) LPSC 48. [6] Seelos F. et al. (2011) AGU Fall, vol. 23, Abstract #1714. [7] Delamere A. et al. (2010), Icarus, 205, 38-52. Acknowledgements: The authors wish to thank the spacecraft and instrument engineering teams for the successful completion of the instrument. CaSSIS is a project of the University of Bern and funded through the Swiss Space Office via ESA's PRODEX programme. The instrument hardware development was also supported by the Italian Space Agency (ASI) (ASI-INAF agreement no.I/018/12/0), INAF/Astronomical Observatory of Padova, and the Space Research Center (CBK) in Warsaw. Support from SGF (Budapest), the University of Arizona Lunar and Planetary Laboratory, and NASA are also gratefully acknowledged. The lead author also acknowledges personal Canadian

  15. Quantitative Planetary Protection for Sample Return from Ocean Worlds

    Science.gov (United States)

    Neveu, Marc; Takano, Yoshinori; Porco, Carolyn; McKay, Christopher P.; Glavin, Daniel; Anbar, Ariel; Sherwood, Brent; Yano, Hajime

    2016-07-01

    compliance of specific designs, would be a crucial step towards ocean world sample return missions, which are uniquely poised to inform us about the likelihood of life on other worlds. A possible path to setting policy could involve tasking experts (including COSPAR PP Panel members) to recommend quantitative means of evaluating provisions (F1)-(F7) and (B1)-(B6), and whether to include (B3)-(B5) in the COSPAR PP Policy [13]. The ongoing European Planetary Protection of Outer Solar System effort, seeking to "provide science and policy recommendations for the definition, improvement, and implementation of an adequate [PP] policy for outer solar system bodies" [27], may achieve this task. References: [1] Porco et al. (2006) Science 311, 1393. [2] Roth et al. (2014) Science 343, 171. [3] Tsou et al. (2012) Astrobiol 12, 730. [4] McKay et al. (2014) Astrobiol 14, 352. [5] Kivelson et al. (2000) Science 289, 1340. [6] Thomas et al. (2016) Icarus 264, 37. [7] Hsu et al. (2015) Nature 519, 207. [8] Waite et al. (2009) Nature 460, 487. [9] Takai et al. (2008) PNAS 105, 10949. [10] Sekine et al. (2015) Nature Comm 6, 8604. [11] Worth et al. (2013) Astrobiol 13, 1155. [12] Space Studies Board (1998) doi: 10.17226/6281. [13] Kminek and Rummel (2015) Space Res Today 193, 7. [14] NASA NPR 8020.12D (2011). [15] Summons et al. (2014) Astrobiol 14, 969. [16] Mileikowsky et al. (2000) Icarus 145, 391. [17] Hand et al. (2007) Astrobiol 7, 1006. [18] Nicholson (2009) Trends Microbiol 17, 243. [19] Showman and Han (2005) Icarus 177, 425. [20] Price and Sowers (2004) PNAS 101, 4631. [21] Silveira et al. (2005) Nature 437, 257. [22] Younse et al. (2012) doi: 10.1109/AERO.2012.6187048. [23,24] Yano et al. (2016a,b) 41 ^{st COSPAR Sci. Assy.} (this volume). [25] Takano et al. (2014) Adv Space Res 53, 1135. [26] Daspit et al. (1975) Acta Astro 2, 649. [27] INAF (retrieved 2/19/2016) PPOSS. http://www.inaf.it/it/sedi/sede-centrale-nuova/direzione-scientifica/relazioni-internazionali/pposs.

  16. Recent variability of the solar spectral irradiance and its impact on climate modelling

    Science.gov (United States)

    Ermolli, I.; Matthes, K.; Dudok de Wit, T.; Krivova, N. A.; Tourpali, K.; Weber, M.; Unruh, Y. C.; Gray, L.; Langematz, U.; Pilewskie, P.; Rozanov, E.; Schmutz, W.; Shapiro, A.; Solanki, S. K.; Woods, T. N.

    2013-04-01

    The lack of long and reliable time series of solar spectral irradiance (SSI) measurements makes an accurate quantification of solar contributions to recent climate change difficult. Whereas earlier SSI observations and models provided a qualitatively consistent picture of the SSI variability, recent measurements by the SORCE (SOlar Radiation and Climate Experiment) satellite suggest a significantly stronger variability in the ultraviolet (UV) spectral range and changes in the visible and near-infrared (NIR) bands in anti-phase with the solar cycle. A number of recent chemistry-climate model (CCM) simulations have shown that this might have significant implications on the Earth's atmosphere. Motivated by these results, we summarize here our current knowledge of SSI variability and its impact on Earth's climate. We present a detailed overview of existing SSI measurements and provide thorough comparison of models available to date. SSI changes influence the Earth's atmosphere, both directly, through changes in shortwave (SW) heating and therefore, temperature and ozone distributions in the stratosphere, and indirectly, through dynamical feedbacks. We investigate these direct and indirect effects using several state-of-the art CCM simulations forced with measured and modelled SSI changes. A unique asset of this study is the use of a common comprehensive approach for an issue that is usually addressed separately by different communities. We show that the SORCE measurements are difficult to reconcile with earlier observations and with SSI models. Of the five SSI models discussed here, specifically NRLSSI (Naval Research Laboratory Solar Spectral Irradiance), SATIRE-S (Spectral And Total Irradiance REconstructions for the Satellite era), COSI (COde for Solar Irradiance), SRPM (Solar Radiation Physical Modelling), and OAR (Osservatorio Astronomico di Roma), only one shows a behaviour of the UV and visible irradiance qualitatively resembling that of the recent SORCE

  17. On Solar Granulations, Limb Darkening, and Sunspots: Brief Insights in Remembrance of Father Angelo Secchi

    Directory of Open Access Journals (Sweden)

    Robitaille P.-M.

    2011-07-01

    Full Text Available Father Angelo Secchi used the existence of solar granulation as a central line of rea- soning when he advanced that the Sun was a gaseous body with a photosphere contain- ing incandescent particulate matter (Secchi A. Sulla Struttura della Fotosfera Solare. Bullettino Meteorologico dell’Osservatorio del Collegio Romano , 30 November 1864, v.3(11, 1–3. Secchi saw the granules as condensed matter emitting the photospheric spectrum, while the darkened intergranular lanes conveyed the presence of a gaseous solar interior. Secchi also considered the nature of sunspots and limb darkening. In the context of modern solar models, opacity arguments currently account for the emis- sive properties of the photosphere. Optical depth is thought to explain limb darkening. Both temperature variations and magnetic fields are invoked to justify the weakened emissivities of sunspots, even though the presence of static magnetic fields in materi- als is not usually associated with modified emissivity. Conversely, within the context of a liquid metallic hydrogen solar model, the appearance of granules, limb darkening, and sunspots can be elegantly understood through the varying directional emissivity of condensed matter. A single explanation is applicable to all three phenomena. Granular contrast can be directly associated with the generation of limb darkening. Depending on size, granules can be analyzed by considering Kolmogoroff’s formulations and B ́ enard convection, respectively, both of which were observed using incompressible liquids, not gases. Granules follow the 2-dimensional space filling laws of Aboav-Weiner and Lewis. Their adherence to these structural laws provides supportive evidence that the granular surface of the Sun represents elements which can only be constructed from condensed matter. A gaseous Sun cannot be confined to a 2-dimensional framework. Mesogranules, supergranules, and giant cells constitute additional entities which further

  18. The SISTEMA Project contribution in the implementation of the GEO Geohazards Supersite initiative

    Science.gov (United States)

    Vilardo, Giuseppe; Sangianantoni, Agata; Borgstrom, Sven; D'Auria, Luca; De Martino, Prospero; Dolce, Mario; Isaia, Roberto; Marotta, Enrica; Martini, Marcello; Obrizzo, Francesco; Peluso, Rosario; Sansivero, Fabio; Scarpato, Giovanni; Siniscalchi, Valeria; Tammaro, Umberto; Tulino, Sabrina; Castellano, Mario; Bianco, Francesca

    2017-04-01

    SISTEMA Project has been funded by the PO FESR 2007-2013 action, supported by the Campania Region (Italy). The project fosters the integrated use of multidisciplinary data in order to improve the understanding of the volcanic processes at Campi Flegrei and Ischia and to progress in science and surveillance of the territory according to the rationale of Supersite GEO initiative to Campi Flegrei, currently identified as Permanent Supersite. The mission of SISTEMA is to upgrade the existing monitoring and surveillance systems through the design, purchase and installation of new instrumentation, equipment, technology and methods addressing the need of delivering, with improved rapidity, scientific information for decision makers and end-users. The redundancy of monitoring systems is an important issue to guarantee the full operability during emergencies. The Monitoring Centre of INGV-Osservatorio Vesuviano is currently located within the red zone (potentially at risk of invasion by pyroclastic flows in case of eruption) of Campi Flegrei volcano. Its position offers various logistic benefits but at the onset of a volcanic crisis, of course it will be required to shift this Center in a safer area. For this reason, within the SISTEMA project, we envisioned a backup system which, when needed, could guarantee a shift of the Center in a virtually zero time. This can be achieved by fully duplicating the processing system and the data storage. In case of emergency, it would be required only to switch on the visualization systems in the new Center and transferring the personnel involved in the surveillance activities. SISTEMA project has also enabled the development of a permanent GPS and CRs (Corner Reflectors) networks, the latter supporting SAR Interferometry, by helping to improve knowledge of the Campi Flegrei deformation field, both on local and wide scale. In addition, in order to enhance the heat flux measurements from ground based thermal camera observations, the

  19. SYMBIOTIC STAR BLOWS BUBBLES INTO SPACE

    Science.gov (United States)

    2002-01-01

    . The jets of material in the lower left and upper right corners may have been accelerated by the white dwarf's accretion disk and probably are part of the older eruption. The nebula, located in the Southern Hemisphere constellation of Centaurus, is a few thousand light-years from Earth. This image, taken in May 1999, captures the glow of nitrogen gas energized by the white dwarf's intense radiation. These results were presented at the 'Asymmetrical Planetary Nebulae II: From Origins to Microstructures' conference, which took place at the Massachusetts Institute of Technology, August 3-6, 1999. Credits: Romano Corradi, Instituto de Astrofisica de Canarias, Tenerife, Spain; Mario Livio, Space Telescope Science Institute, Baltimore, Md.; Ulisse Munari, Osservatorio Astronomico di Padova-Asiago, Italy; Hugo Schwarz, Nordic Optical Telescope, Canarias, Spain; and NASA

  20. Exploring the connection between the stellar wind and the non-thermal emission in LS 5039

    Science.gov (United States)

    Bosch-Ramon, V.; Motch, C.; Ribó, M.; Lopes de Oliveira, R.; Janot-Pacheco, E.; Negueruela, I.; Paredes, J. M.; Martocchia, A.

    2007-10-01

    compact object, or the density in the system is 3 to 27 times smaller than that predicted by a spherical symmetric wind model. We suggest that the multiwavelength non-thermal emission of LS 5039 is related to the observed extended radio jets and is unlikely to be produced inside the binary system. The Hα results presented here are based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under program IDs 67.D-0229(A), 69.D-0628(A) and 075.D-0591(A); the Observatoire de Haute-Provence; the Observatório do Pico dos Dias / LNA, Brazil; the G. D. Cassini telescope operated at the Loiano Observatory by the Osservatorio Astronómico di Bologna; and the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias (those data were taken using ALFOSC, which is owned by the Instituto de Astrofísica de Andalucía (IAA) and operated at the Nordic Optical Telescope under agreement between IAA and the NBIfAFG of the Astronomical Observatory of Copenhagen). Table 2 is only available in electronic form at http://www.aanda.org

  1. Challenges in communicating research and research careers: lesson learned from the European Researchers' Nights at INGV

    Science.gov (United States)

    D'Addezio, Giuliana; Rubbia, Giuliana; Musacchio, Gemma; Lanza, Tiziana

    2014-05-01

    frequent comment was the invitation to repeat more frequently such events. With no doubt, the visit to seismic surveillance room contributes to give more information and clarification about seismicity of the territory, dispel the myth or deepen the debate on deterministic earthquake prediction and regain at least part of the reputational damage following both the earthquake and the L'Aquila trial (Amato et al., EGU2013-12140). Nevertheless, it remains challenging to measure effects of such initiatives on middle terms, and performance indicators are desirable. It is worth noting that, while INGV organizes this kind of events for several years, it seem that researchers who take active part in this organization are still a limited number. In fact, participants where mainly technician and fixed-term position personnel, mostly women. Is this unavailability related to weak curricular evaluation of third-mission activity in research careers? This require a reflection. Moreover, a video realized by INGV Osservatorio Etneo dealing with working conditions of women in research, presented during the 2012 edition, allows to reflect about the need for more family friendly practices to balance family care and work as well as to promote participation of female researchers to decision making bodies.

  2. Studies Of A Local Ground Deformation Episode Measured By Gps, During The 2001 Eruption, In The Upper Southern Flank Of Mt. Etna

    Science.gov (United States)

    Puglisi, G.; Bonforte, A.; Guglielmino, F.; Palano, M.; Galvani, A.; Pesci, A.

    During the July - August 2001 Mt Etna eruption, GPS measurements have been car- ried out almost daily on a E-W profile, consisting of 16 stations along the SP92 route from Serra la Nave up to the Rifugio Sapienza area and crossing the 1989 fracture field. Most benchmarks of the profile have been installed close to the gravity stations of INGV, section of Catania, and some of them are in common with the levelling line, installed by the Osservatorio Vesuviano. The E-W profile, unlike other GPS networks on Mt. Etna, has no self-centring benchmarks so, besides the levelling ones, all bench- marks consist in nails. They are occupied putting the GPS antenna on a staff, kept in vertical position by the operator or by a small tripod. This profile has been measured in Stop and Go kinematic technique with sample rate of 5 seconds and two occupa- tions of 3 minutes for each station. The profile has been measured together with more than one station occupied in static mode, in order to give better quality solutions. Mea- surements along this profile have been carried out since the first days of eruption (18 July 2001), few hours after the opening of the eruptive fissure at 2100 m a.s.l., and just before the lava flow crossed the road at the Rifugio Sapienza area. For this reason, only on the first day it was possible to carry out an unique measurement on the whole profile; on the following days, in fact, the profile was split into two segments (the East segment and the West segment), each consisting of 8 stations. This profile has been measured 7 time during the period of the eruption and it has been repeated again few days after its end. During the processing, all kinematic and static occupations have been linked to the Mt. Etna GPS permanent network. The resulting network has been then adjusted, fixing the co-ordinates of the southernmost station of the permanent network (NICO) which in turn has been tied, session by session, to external reference stations. The resulting

  3. 19 years of tilt data on Mt. Vesuvius: state of the art and future perspectives

    Directory of Open Access Journals (Sweden)

    Ciro Ricco

    2013-11-01

    Full Text Available Mt. Vesuvius, located along the SW border of the Campania Plane graben, is one of the most studied volcanoes worldwide, from both the volcanological and the geophysical, geochemical and geodetic point of view. In order to better understand its dynamics, the deformation of the volcano has been already studied since the early ’70s by setting up levelling lines and, since a few years later, through trilateration networks, whereas ground tilt monitoring started in 1993. Tilt variations were recorded by an automatic surface station set up at the Osservatorio Vesuviano (O.V. bunker (OVO and data recorded were transmitted to the O.V. Surveillance Centre in Naples. Afterwards, in 1996 two more identical stations were set up close to Torre del Greco (CMD, and close to Trecase (TRC. In 2002 the data acquisition system was replaced, while at the end of 2011 a Lily borehole sensor was set up at 26 m depth, replacing the old TRC tilt station. The paper describes in details the tilt network of Mt. Vesuvius, its development over time and the data processing procedure; moreover, the ground deformation pattern is discussed, as inferred from the study of 19 years of data and its change during the seismic crises of 1995-1996 and 1999-2000. From the information obtained from the tiltmetric monitoring, a complex deformation pattern can be deduced, strongly dependent on the position of the sites in which the sensors were set up with respect to the morphology of the volcanic edifice and its structural outlines. If we consider the signals as they were recorded, although previously corrected for the influences of the thermo-elastic strain on the sensors, the tilting occurs mainly in the SW direction with rates of about 11 µradians/year on both the western and eastern flanks and of about 13 µradians/year on the southern one. Because tilt vectors point in the long term outward from the summit and towards the subsiding area, this supports the hypothesis of a southern

  4. First observations of Ceres by VIR on Dawn mission

    Science.gov (United States)

    De Sanctis, M. Cristina; Ammannito, Eleonora; Fonte, Sergio; Magni, Gianfranco; Capaccioni, Fabrizio; Capria, M. Teresa; Raymond, Carol. A.; Russell, Christopher T.

    2015-04-01

    The Dawn spacecraft [1] is now approaching Ceres, the second of its targets. Ceres represents the key to understand some important points relative to the role of the protoplanet size and the water content in the evolution of these bodies. Ceres is thought to be differentiated, and hydrated minerals were proposed to exist on its surface [2,3,4]. Its low density [3] associated with the presence of transient water vapour, suggests a high content of ice inside the body and on its surface. Ceres seems to have been subject to differentiation and hydrothermal activity, and might host a liquid subsurface layer even today. Dawn is equipped with a Visible and InfraRed Mapping Spectrometer (VIR-MS) [5]. VIR-MS is an imaging spectrometer coupling high spectral and spatial resolution in the VIS (0.25-1 micron) and IR (0.95-5 micron) spectral ranges. The surface composition of Ceres is poorly understood through its nearly featureless visible spectrum. Its visible reflectance spectrum has a steep UV absorption edge that begins at a relatively short wavelength, around 0.4 micron, unlike many C-type asteroids where the UV drop-off begins around 0.6 to 0.7 micron[6]. The near-IR spectrum has a strong absorption band centered at about 3-micron. The absorption features in the 3-micron region were attributed to structural water in clay minerals [7,8] but could also be ammoniated clays [9]. [10] reported the discovery of carbonates and iron-rich clays from measurements of weak 3-micron features, and the results are consistent with the mid-IR spectra of clay minerals. On approach to Ceres, Dawn will obtain images and hyperspectral . VIR data, with resolution larger than Hubble images will reveal the first details of the Ceres' surface composition. Here we report about the first data obtained by VIR during its approach to Ceres. Acknowledgments VIR is funded by the Italian Space Agency-ASI and was developed under the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali, Rome

  5. VLT/X-Shooter spectroscopy of the afterglow of the Swift GRB 130606A. Chemical abundances and reionisation at z ~ 6

    Science.gov (United States)

    Hartoog, O. E.; Malesani, D.; Fynbo, J. P. U.; Goto, T.; Krühler, T.; Vreeswijk, P. M.; De Cia, A.; Xu, D.; Møller, P.; Covino, S.; D'Elia, V.; Flores, H.; Goldoni, P.; Hjorth, J.; Jakobsson, P.; Krogager, J.-K.; Kaper, L.; Ledoux, C.; Levan, A. J.; Milvang-Jensen, B.; Sollerman, J.; Sparre, M.; Tagliaferri, G.; Tanvir, N. R.; de Ugarte Postigo, A.; Vergani, S. D.; Wiersema, K.; Datson, J.; Salinas, R.; Mikkelsen, K.; Aghanim, N.

    2015-08-01

    Instituto de Astrofísica de Canarias. Partly based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, under programme A26TAC_63.Appendix A is available in electronic form at http://www.aanda.orgThe reduced spectrum (FITS file) is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/580/A139

  6. Europlanet - Joining the European Planetary Research Information Service

    Science.gov (United States)

    Capria, M. T.; Chanteur, G.; Schmidt, W.

    2009-04-01

    to data to be integrated into the VO features of IDIS? Any combination and many more alternatives are possible. 3. Contact the staff of the selected node(s) to go through the details 4. The node's expert team will evaluate the information to ensure that it is compliant with the minimum requirements for Europlanet information providers like correct address, related field of competence, quality of data if any etc. 5. The new resource meta data (addresses, contents etc) will be added to the IDIS system including update of the search facilities 6. If data are offered for on-line access, the IDIS team will provide tools to generate a network-compatible generic interface. This one-time effort will make it possible to search the new data sets and combine them with related in-formation from other sources. Benefits for the information provider: - wide advertisement for the own resources and capabilities with increase in scientific references to the own activities and publications - new co-operation possibilities with so far unknown teams. Team exchange might be financially supported by other segments of the Europlanet RI - strong arguments for new funding applications and many more aspects List of contact web-sites: Technical node for support and management aspects: http://www.europlanet-idis.fi/ Planetary Surfaces and Interiors node: http://europlanet.dlr.de/ Planetary Plasma node: http://europlanet-plasmanode.oeaw.ac.at/ Planetary Atmospheres node: http://idis.ipsl.jussieu.fr/ Virtual Observatory Paris Data Centre: http://vo.obspm.fr/ Small Bodies and Dust node: http://www.ifsi-roma.inaf.it/europlanet/

  7. Rings Research in the Next Decade

    Science.gov (United States)

    Burns, J. A.; Tiscareno, M. S.

    2009-12-01

    -based observations. Members of the Rings White Paper Team include: Matthew S. Tiscareno (Cornell U), Nicole Albers (U of Colorado), Todd Bradley (U of Central Florida), André Brahic (U of Paris, France), Shawn Brooks (JPL), Joseph Burns (Cornell U), Carlos Chavez (UNAM, Mexico), Joshua Colwell (U of Central Florida), Jeff Cuzzi (NASA Ames), Imke de Pater (U of California), Luke Dones (SwRI), Richard Durisen (Indiana U), Michael Evans (Cornell U), Cecile Ferrari (CEA Saclay, France), Gianrico Filacchione (INAF-IASF, Italy), Silvia Giuliatti Winter (UNESP, Brazil), Mitch Gordon (SETI), Amara Graps (SwRI), Eberhard Gruen (MPI, Germany), Douglas Hamilton (U of Maryland), Matthew Hedman (Cornell U), Mihaly Horanyi (U of Colorado), Sascha Kempf (MPI, Germany), Harald Krueger (MPI, Germany), Steve Larson (U of Arizona), Mark Lewis (Trinity U), Jack Lissauer (NASA Ames), Colin Mitchell (CICLOPS/SSI), Carl Murray (QMUL, England), Philip Nicholson (Cornell U), Cathy Olkin (SwRI), Robert Pappalardo (JPL), Frank Postberg (MPI, Germany), Heikki Salo (U of Oulu, Finland), Juergen Schmidt (U of Potsdam, Germany), David Seal (JPL), Mark Showalter (SETI), Frank Spahn (U of Potsdam, Germany), Linda Spilker (JPL), Joseph Spitale (CICLOPS/SSI), Ralf Srama (MPI, Germany), Miodrag Sremcevic (U of Colorado), Glen Stewart (U of Colorado), John Weiss (Carleton College), Padma Yanamandra-Fisher (JPL)

  8. Evidence of a massive planet candidate orbiting the young active K5V star BD+20 1790

    Science.gov (United States)

    Hernán-Obispo, M.; Gálvez-Ortiz, M. C.; Anglada-Escudé, G.; Kane, S. R.; Barnes, J. R.; de Castro, E.; Cornide, M.

    2010-03-01

    (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Based on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias with financial support from the UK Science and Technology Facilities Council.Our radial velocity data from Table 3 are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/512/A45

  9. Long-term magnetic activity in close binary systems. I. Patterns of color variations

    Science.gov (United States)

    Messina, S.

    2008-03-01

    is found in less than 40% of observation seasons when the fainter component has a non-negligible level of activity and/or hot faculae are present but they are either spatially or temporally uncorrelated to spots. I dedicate this paper to the memory of the P.I. of this project, Prof. Marcello Rodonò, who suddenly passed away on October 23, 2005. To him my sincere estimation and deepest gratitude. Based on observations collected at INAF-Catania Astrophysical Observatory, Italy.

  10. Results from VIRTIS on board Venus Express after the end of the mission operations

    Science.gov (United States)

    Piccioni, G.; Drossart, P.; VIRTIS Venus Express Team

    }. Multiwavelength clouds tracking and thermal fields allowed to study the wind fields and the global dynamics, in particular the complex details of the polar vortex \\citep{Garate-Lopez2013,Garcia2009, Hueso2008,Limaye2009,Luz2011,Peralta2012,Piccioni2007b,Sanchez-Lavega2008,Titov2008}. A review of the main results is here reported along some question of what is still needed to progress in the knowledge of our sister planet from ground based observations and future space missions. We acknowledge the support from the funding agencies, in particular ASI thorugh the contract ASI INAF I/050/10/0.

  11. The 1:3M geologic map of Mercury: progress and updates

    Science.gov (United States)

    Galluzzi, Valentina; Guzzetta, Laura; Mancinelli, Paolo; Giacomini, Lorenza; Malliband, Christopher C.; Mosca, Alessandro; Wright, Jack; Ferranti, Luigi; Massironi, Matteo; Pauselli, Cristina; Rothery, David A.; Palumbo, Pasquale

    2017-04-01

    After the end of Mariner 10 mission a 1:5M geologic map of seven of the fifteen quadrangles of Mercury [Spudis and Guest, 1988] was produced. The NASA MESSENGER mission filled the gap by imaging 100% of the planet with a global average resolution of 200 m/pixel and this led to the production of a global 1:15M geologic map of the planet [Prockter et al., 2016]. Despite the quality gap between Mariner 10 and MESSENGER images, no global geological mapping project with a scale larger than 1:5M has been proposed so far. Here we present the status of an ongoing project for the geologic mapping of Mercury at an average output scale of 1:3M based on the available MESSENGER data. This project will lead to a fuller grasp of the planet's stratigraphy and surface history. Completing such a product for Mercury is an important goal in preparation for the forthcoming ESA/JAXA BepiColombo mission to aid selection of scientific targets and to provide context for interpretation of new data. At the time of this writing, H02 Victoria [Galluzzi et al., 2016], H03 Shakespeare [Guzzetta et al., 2016] and H04 Raditladi [Mancinelli et al., 2016] have been completed and H05 Hokusai [Rothery et al., 2017], H06 Kuiper [Giacomini et al., 2017], H07 Beethoven and H10 Derain [Malliband et al., 2017] are being mapped. The produced geologic maps were merged using the ESRI ArcGIS software adjusting discontinuous contacts along the quadrangle boundaries. Contact discrepancies were reviewed and discussed among the mappers of adjoining quadrangles in order to match the geological interpretation and provide a unique consistent stratigraphy. At the current stage, more than 20% of Mercury has now a complete 1:3M map and more than 40% of the planet will be covered soon by the maps that are being prepared. This research was supported by the Italian Space Agency (ASI) within the SIMBIOSYS project (ASI-INAF agreement no. I/022/10/0). References Galluzzi V. et al. (2016). Geology of the Victoria Quadrangle (H

  12. Carbon and nitrogen abundances of stellar populations in the globular cluster M 2

    Science.gov (United States)

    Lardo, C.; Pancino, E.; Mucciarelli, A.; Milone, A. P.

    2012-12-01

    . Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias (PROGRAM ID: A22TAC_20).Full Table 1 and photometric data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/548/A107

  13. The VIMOS Public Extragalactic Redshift Survey (VIPERS). An unbiased estimate of the growth rate of structure at ⟨z⟩ = 0.85 using the clustering of luminous blue galaxies

    Science.gov (United States)

    Mohammad, F. G.; Granett, B. R.; Guzzo, L.; Bel, J.; Branchini, E.; de la Torre, S.; Moscardini, L.; Peacock, J. A.; Bolzonella, M.; Garilli, B.; Scodeggio, M.; Abbas, U.; Adami, C.; Bottini, D.; Cappi, A.; Cucciati, O.; Davidzon, I.; Franzetti, P.; Fritz, A.; Iovino, A.; Krywult, J.; Le Brun, V.; Le Fèvre, O.; Maccagni, D.; Małek, K.; Marulli, F.; Polletta, M.; Pollo, A.; Tasca, L. A. M.; Tojeiro, R.; Vergani, D.; Zanichelli, A.; Arnouts, S.; Coupon, J.; De Lucia, G.; Ilbert, O.; Moutard, T.

    2018-02-01

    . Based on observations collected at the European Southern Observatory, Cerro Paranal, Chile, using the Very Large Telescope under programs 182.A-0886 and partly 070.A-9007. Also based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. The VIPERS web site is http://www.vipers.inaf.it/

  14. A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups

    Science.gov (United States)

    Maldonado, J.; Martínez-Arnáiz, R. M.; Eiroa, C.; Montes, D.; Montesinos, B.

    2010-10-01

    ía (CSIC) and observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.Appendices and Tables 1, 5-15 are available in electronic form at http://www.aanda.orgTable 1 is also available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/521/A12

  15. Internal dynamics of the radio-halo cluster A2219: A multi-wavelength analysis

    Science.gov (United States)

    Boschin, W.; Girardi, M.; Barrena, R.; Biviano, A.; Feretti, L.; Ramella, M.

    2004-03-01

    with the Italian Telescopio Nazionale Galileo (TNG) operated by the Centro Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) and with the 1.0 m Jacobus Kapteyn Telescope (JKT) operated by the Isaac Newton Group at the Spanish Observatorio de Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Table 1 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/416/839

  16. Galactic Teamwork Makes Distant Bubbles

    Science.gov (United States)

    Kohler, Susanna

    2016-03-01

    During the period of reionization that followed the dark ages of our universe, hydrogen was transformed from a neutral state, which is opaque to radiation, to an ionized one, which is transparent to radiation. But what generated the initial ionizing radiation? The recent discovery of multiple distant galaxies offers evidence for how this process occurred.Two Distant GalaxiesWe believe reionization occurred somewhere between a redshift of z = 6 and 7, because Ly-emitting galaxies drop out at roughly this redshift. Beyond this distance, were generally unable to see the light from these galaxies, because the universe is no longer transparent to their emission. This is not always the case, however: if a bubble of ionized gas exists around a distant galaxy, the radiation can escape, allowing us to see the galaxy.This is true of two recently-discovered Ly-emitting galaxies, confirmed to be at a redshift of z~7 and located near one another in a region known as the Bremer Deep Field. The fact that were able to see the radiation from these galaxies means that they are in an ionized HII region presumably one of the earlier regions to have become reionized in the universe.But on their own, neither of these galaxies is capable of generating an ionized bubble large enough for their light to escape. So what ionized the region around them, and what does this mean for our understanding of how reionization occurred in the universe?A Little Help From FriendsLocation in different filters of the objects in the Hubble Bremer Deep Field catalog. The z~7 selection region is outlined by the grey box. BDF-521 and BDF-3299 were the two originally discovered galaxies; the remaining red markers indicate the additional six galaxies discovered in the same region. [Castellano et al. 2016]A team of scientists led by Marco Castellano (Rome Observatory, INAF) investigated the possibility that there are other, faint galaxies near these two that have helped to ionize the region. Performing a survey

  17. Watch Out for Falling Plasma

    Science.gov (United States)

    Kohler, Susanna

    2016-12-01

    The path taken by the falling fragment in the June 2011 event. [Adapted from Petralia et al. 2016]Sometimes plasma emitted from the Sun doesnt escape into space, but instead comes crashing back down to the solar surface. What can observations and models of this process tell us about how the plasma falls and the local conditions on the Sun?Fallback from a FlareOn 7 June 2011, an M-class flare erupted from the solar surface. As the Solar Dynamics Observatorys Atmospheric Imaging Assembly looked on, plasma fragments from the flare arced away from the Sun and then fell back to the surface.Some fragments fell back where the Suns magnetic field was weak, returning directly to the surface. But others fell within active regions, where they crashed into the Suns magnetic field lines, brightening the channels and funneling along them through the dense corona and back to the Suns surface.The authors model of the falling blobs at several different times in their simulation. The blobs get disrupted when they encounter the field lines, and are then funneled along the channels to the solar surface. [Adapted from Petralia et al. 2016]This sort of flare and fall-back event is a common occurrence with the Sun, and SDOs observations of the June 2011 event present an excellent opportunity to understand the process better. A team of scientists led by Antonino Petralia (University of Palermo, Italy and INAF-OAPA) modeled this event in an effort to learn more about how the falling plasma interacts with strong magnetic fields above the solar surface.Magnetic Fields as GuidesPetralia and collaborators used three-dimensional magnetohydrodynamical modeling to attempt to reproduce the observations of this event. They simulated blobs of plasma as they fall back to the solar surface and interact with magnetic field lines over a range of different conditions.The team found that only simulations that assume a relatively strong magnetic field resulted in the blobs funneling along a channel to the

  18. The intriguing nature of the high-energy gamma ray source XSS J12270-4859

    Science.gov (United States)

    de Martino, D.; Falanga, M.; Bonnet-Bidaud, J.-M.; Belloni, T.; Mouchet, M.; Masetti, N.; Andruchow, I.; Cellone, S. A.; Mukai, K.; Matt, G.

    2010-06-01

    .32 hr that could be ascribed to the binary orbital period. Near-IR, possibly ellipsoidal, variations are detected. Large amplitude variability on shorter (tens mins) timescales is found to be non-periodic. Conclusions: The observed variability at all wavelengths together with the spectral characteristics strongly favour a low-mass atypical low-luminosity X-ray binary and are against a magnetic cataclysmic variable nature. The association with a Fermi/LAT high-energy gamma ray source further strengths this interpretation. Based on observations obtained with XMM-Newton and INTEGRAL, ESA science missions with instruments and contributions directly funded by ESA Member States and NASA, with Fermi a NASA mission with contributions from France, Germany, Italy, Japan, Sweden and USA and with the REM Telescope INAF at ESO, La Silla, Chile

  19. Does Titan have an Active Surface?

    Science.gov (United States)

    Nelson, R.

    2009-12-01

    Robert M. Nelson-1, L. W. Kamp-1, R. M. C. Lopes-1, D. L. Matson-1, R. L. Kirk-2, B. W. Hapke-3, M. D. Boryta-4, F. E. Leader-1, W. D. Smythe-1, K. L. Mitchell-1, K. H. Baines-1, R. Jaumann-5, C. Sotin-1, R. N. Clark-6, D. P. Cruikshank-7 , P. Drossart-8, J. I. Lunine-9, M. Combes-10, G. Bellucci-11, J.-P. Bibring-12, F. Capaccioni-11, P. Cerroni-11, A. Coradini-11, V. Formisano-11, G. Filacchione-11, Y. Langevin-12, T. B. McCord-13, V. Mennella-14, B. Sicardy-8, P. G. J. Irwin-15 ,J.C. Pearl-16 1-JPL, 4800 Oak Grove Drive, Pasadena CA 91109;2-USGS, Flagstaff; 3-U Pittsburgh; 4-Mt. San Antonio College; 5-DLR, Berlin;6-USGS Denver; 7-NASA AMES; 8-U Paris-Meudon; 9-U Arizona; 10- Obs de Paris; 11-INAF-ISAF Rome; 12-U Paris -Sud. Orsay; 13-Bear Flt Cntr. Winthrop WA;14-Obs Capodimonte Naples; 15-Clarendon Laboratory, Oxford, UK, 16-Goddard Space Flight Center, Greenbelt MD Surface changes on Saturn’s moon Titan have been reported during the Cassini spacecraft’s four-year orbital tour of the Saturnian system based on Cassini Visual and Infrared Mapping Spectrometer (VIMS) data [1]. Titan’s surface is hard to observe because it’s atmosphere is opaque at visual wavelengths due to absorption by methane in Titan’s atmosphere. VIMS is able to image the surface through “windows” at infrared wavelengths where the methane is relatively transparent [1,2]. VIMS infrared images find surface reflectance variability at Hotei Reggio (26S,78W) and suggest that the variability might be due to deposition, followed by coverage or dissipation, of ammonia frost. Subsequently, Cassini RADAR images found that Hotei Reggio, has lobate “flow” forms, consistent with the morphology of volcanic terrain [3]. Here we report the discovery of lobate “flow” patterns at Hotei Reggio based on VIMS infrared images taken during Cassini close flybys during 2008-2009. This new evidence is consistent with the suggestion that the brightness variability at Hotei Reggio is associated with

  20. ESA `Huygens and Mars Express' science highlights - call to press

    Science.gov (United States)

    2005-11-01

    'Aéronomie/CNRS, France 16:40 - Bruno Bezard, Co-Investigator, Descent Imager/Spectral Radiometer, Laboratoire d'études spatiales et d'instrumentation en astrophysique, Observatoire de Paris, France 16:45 - Jonathan Lunine, Interdisciplinary Scientist, Titan surface-atmosphere interactions, LPL/U, Arizona (USA) and INAF/IFSI, Rome (Italy) 16:55 - Questions and AnswersV 17:05 - Coffee break 17:10 - Mars Express: results in the overall context of Martian science, Agustin Chicarro, ESA Mars Express Project Scientist 17:15 - Giovanni Picardi, MARSIS Radar Principal Investigator, University of Rome La Sapienza, Italy Jeffrey Plaut, MARSIS Co-Principal Investigator, NASA/JPL, USA 17:25 - Martin Pätzold, Mars Radio Science Experiment, Principal Investigator, Universität Koln, Cologne, Germany 17:30 - Jean-Pierre Bibring, OMEGA Principal Investigator, Institut d’Astrophysique spatiale, Orsay, France 17:40 - Gerhard Neukum, HRSC Camera Principal Investigator, Freie Universität Berlin, Germany 17:45 - Questions and Answers 17:55 - Interview opportunities

  1. Integrated Access to Solar Observations With EGSO

    Science.gov (United States)

    Csillaghy, A.

    2003-12-01

    {\\b Co-Authors}: J.Aboudarham (2), E.Antonucci (3), R.D.Bentely (4), L.Ciminiera (5), A.Finkelstein (4), J.B.Gurman(6), F.Hill (7), D.Pike (8), I.Scholl (9), V.Zharkova and the EGSO development team {\\b Institutions}: (2) Observatoire de Paris-Meudon (France); (3) INAF - Istituto Nazionale di Astrofisica (Italy); (4) University College London (U.K.); (5) Politecnico di Torino (Italy), (6) NASA Goddard Space Flight Center (USA); (7) National Solar Observatory (USA); (8) Rutherford Appleton Lab. (U.K.); (9) Institut d'Astrophysique Spatial, Universite de Paris-Sud (France) ; (10) University of Bradford (U.K) {\\b Abstract}: The European Grid of Solar Observations is the European contribution to the deployment of a virtual solar observatory. The project is funded under the Information Society Technologies (IST) thematic programme of the European Commission's Fifth Framework. EGSO started in March 2002 and will last until March 2005. The project is categorized as a computer science effort. Evidently, a fair amount of issues it addresses are general to grid projects. Nevertheless, EGSO is also of benefit to the application domains, including solar physics, space weather, climate physics and astrophysics. With EGSO, researchers as well as the general public can access and combine solar data from distributed archives in an integrated virtual solar resource. Users express queries based on various search parameters. The search possibilities of EGSO extend the search possibilities of traditional data access systems. For instance, users can formulate a query to search for simultaneous observations of a specific solar event in a given number of wavelengths. In other words, users can search for observations on the basis of events and phenomena, rather than just time and location. The software architecture consists of three collaborating components: a consumer, a broker and a provider. The first component, the consumer, organizes the end user interaction and controls requests

  2. VNIR reflectance spectroscopy of glassy igneous material with variable oxidation states

    Science.gov (United States)

    Carli, Cristian; Di Genova, Danilo; Roush, Ted L.; Ertel-Ingrisch, Werner; Capaccioni, Fabrizio; Dingwell, Donald B.

    2017-04-01

    Silicate glasses with igneous compositions may represent an abundant component of planetary surface material via effusive volcanism or impact cratering processes. Several planetary surfaces are mapped with hyper-spectrometers in the visible and near-infrared (VNIR). In this spectral range, crystal field (C.F.) absorptions are useful to discriminate iron-bearing silicate components. At the same time, in the VNIR reflectance spectroscopy iron bearing glasses may exhibit a C.F. absorption at ˜1.1 μm. A weak C.F. absorption is also present at ˜1.9 μm. These absorptions can be therefore diagnostic for glassy component and can also affect the C.F. absorptions of mafic minerals when mixed in the regolith. So far, few studies investigated the spectral properties of systematic glasses compositions and at different oxygen fucacity. For these reasons studying glassy materials, and their optical constants, represents an important effort to document and to interpret, spectral features of Solar System silicate crusts where glasses are present, but may be difficult to map. In previous work Carli et al. (2016) considered the composition of glassy igneous materials produced in Earth-like atmospheric conditions (i.e. oxidized conditions). Here, we expand on that effort by including glasses formed under more reducing condition. In this study, glasses were produced at -9.3 log fO2 and 1400 ˚ C for a duration of 4 h at the Department of Earth and Environmental Sciences at the University of Munich using a gas-mixing furnace. The major element composition, sample homogeneity, and the Fe3+/Fetot. ratio of run products were analytically determined. Moreover, Raman spectra of the same samples were also acquired. Afterwards, powders were produced with nine-grain size from 250-224 μm to 50-20 μm and measured in bidirectional reflectance at Spectroscopy LABoratory (IAPS-INAF, Rome). Reflectance spectra were acquired from 0.35 to 2.5 μm with a Field-Pro Spectrometer mounted on a

  3. The Capodimonte Deep Field

    Science.gov (United States)

    2001-04-01

    A Window towards the Distant Universe Summary The Osservatorio Astronomico Capodimonte Deep Field (OACDF) is a multi-colour imaging survey project that is opening a new window towards the distant universe. It is conducted with the ESO Wide Field Imager (WFI) , a 67-million pixel advanced camera attached to the MPG/ESO 2.2-m telescope at the La Silla Observatory (Chile). As a pilot project at the Osservatorio Astronomico di Capodimonte (OAC) [1], the OACDF aims at providing a large photometric database for deep extragalactic studies, with important by-products for galactic and planetary research. Moreover, it also serves to gather experience in the proper and efficient handling of very large data sets, preparing for the arrival of the VLT Survey Telescope (VST) with the 1 x 1 degree 2 OmegaCam facility. PR Photo 15a/01 : Colour composite of the OACDF2 field . PR Photo 15b/01 : Interacting galaxies in the OACDF2 field. PR Photo 15c/01 : Spiral galaxy and nebulous object in the OACDF2 field. PR Photo 15d/01 : A galaxy cluster in the OACDF2 field. PR Photo 15e/01 : Another galaxy cluster in the OACDF2 field. PR Photo 15f/01 : An elliptical galaxy in the OACDF2 field. The Capodimonte Deep Field ESO PR Photo 15a/01 ESO PR Photo 15a/01 [Preview - JPEG: 400 x 426 pix - 73k] [Normal - JPEG: 800 x 851 pix - 736k] [Hi-Res - JPEG: 3000 x 3190 pix - 7.3M] Caption : This three-colour image of about 1/4 of the Capodimonte Deep Field (OACDF) was obtained with the Wide-Field Imager (WFI) on the MPG/ESO 2.2-m telescope at the la Silla Observatory. It covers "OACDF Subfield no. 2 (OACDF2)" with an area of about 35 x 32 arcmin 2 (about the size of the full moon), and it is one of the "deepest" wide-field images ever obtained. Technical information about this photo is available below. With the comparatively few large telescopes available in the world, it is not possible to study the Universe to its outmost limits in all directions. Instead, astronomers try to obtain the most detailed

  4. Hipparcos reveals that the Milky Way is changing shape

    Science.gov (United States)

    1998-04-01

    deformations of its disk. About half of all other disk galaxies are seen to be misshapen. This remarkably high proportion may mean that galaxies are so rigid that any warp, once established, lasts for billions of years. Alternatively, galaxies may be very floppy, with new warps being created all the time. The Hipparcos result on the Milky Way may favour the latter, more dynamic interpretation. The riddle of what warps galaxies has puzzled astronomers for decades. Explanations on offer range from intergalactic winds to magnetic contortions. A popular theory blames the warp in the Milky Way on the gravitational pull of invisible dark matter in the halo of the Galaxy. This would imply that the present warp should be a long-lived phenomenon. As the warp may now be only temporary, other explanations will be favoured. Mario Lattanzi, of the Turin group, puts it this way: "As is often the case in experimental science, better experimental data challenge our current understanding of how the Milky Way works." Prominent among the rival proposals about the warping of galaxies is the gravitational (tidal) effect of other galaxies passing close by. In the case of the Milky Way, the Magellanic Clouds and the recently discovered Sagittarius Dwarf Galaxy are candidates as warping agents. But Smart and his colleagues confess themselves to be baffled. "We are obliged to conclude," they write, "that there is currently no convincing interpretation of the implications of Hipparcos data for the dynamics of the warp in the Galactic disk." The reference to the "Nature" paper is: Vol. 392, pp. 471-473. The authors are R.L. Smart,R. Drimmel, M.G. Lattanzi (Osservatorio Astronomico di Torino, Pino Torinese, TO 10025, Italy) and J.J. Binney (Department of Physics, University of Oxford, Oxford OX1 3NP, UK).

  5. Evidence for Ultra-Energetic Particles in Jet from Black Hole

    Science.gov (United States)

    2006-06-01

    shoot out from the black hole at close to the speed of light and then release their energy as radiation as far out as they are seen, the particles have to be accelerated locally, where they produce their emission. Both teams also used data from the third of NASA's Great Observatories, the Hubble Space Telescope, and the radio telescopes of the Very Large Array (VLA). The three space telescopes and the VLA "see" emission of different wavelengths from celestial objects, and the combined data was essential to reveal the new comprehensive perspective on the jets. "The new observations show that the flow structure of this jet is more complicated than had been assumed previously," Jester explains. "That the present evidence favors the synchrotron model deepens the mystery of how jets produce the ultra-energetic particles that radiate at X-ray wavelengths." "Our results call for a radical rethink of the physics of relativistic jets that black holes drive," said Uchiyama. "But, we now have a crucial new clue to solving one of the major mysteries in high-energy astrophysics." Other authors on the papers include Jeffrey Van Duyne and Paolo Coppi at Yale; C.C. Cheung at Stanford University; Rita Sambruna at NASA/GSFC, Greenbelt, MD; Tadayuki Takahashi at ISAS/JAXA, Japan; Laura Maraschi and Fabrizio Tavecchio at the Osservatorio Astronomico di Brera, Milan; Dan Harris from the SAO; Herman Marshall at MIT; and Klaus Meisenheimer at Max Planck Institute for Astronomy in Heidelberg. Grant and contract funding from NASA supported the research. Additional images and background material are available at: http://www.astro.soton.ac.uk/~jester/3C273.html and http://www.astro.isas.jaxa.jp/~uchiyama/Site2/Spitzer_3C273.html

  6. GOODS Missing Black Hole Report: Hundreds Found!

    Science.gov (United States)

    2007-10-01

    can see the elephant for the first time." Consistent results were also recently obtained by Fabrizio Fiore of the Osservatorio Astronomico di Roma and his team. Their results will appear in the Jan 1, 2008, issue of Astrophysical Journal. NASA's Marshall Space Flight Center, Huntsville, Ala., manages the Chandra program for the agency's Science Mission Directorate. The Smithsonian Astrophysical Observatory controls science and flight operations from the Chandra X-ray Center in Cambridge, Mass. NASA's Jet Propulsion Laboratory, Pasadena, Calif., manages the Spitzer Space Telescope mission for NASA's Science Mission Directorate, Washington. Science operations are conducted at the Spitzer Science Center at the California Institute of Technology, also in Pasadena. Caltech manages JPL for NASA

  7. New study reveals twice as many asteroids as previously believed

    Science.gov (United States)

    2002-05-01

    sky corresponding to that covered by four full moons as seen from Earth. Then, a model developed by Tedesco and the astronomers Alberto Cellino and Vincenzo Zappala (Osservatorio Astronomico di Torino, Italy), allowed them to estimate the whole asteroid population in the main belt: between 1.1 million and 1.9 million asteroids with a diameter larger than 1 kilometre. "If you consider the average value of 1.5 million asteroids, the ISO result is about twice as high as estimated by two other recent studies in visible light," Tedesco says. The study by Durda et al., published in 1998, gave an estimate of about 860 000 asteroids larger than 1 kilometre in the main belt. In 2001, Ivezic et al. obtained an even lower figure of 740 000 asteroids based on preliminary data from the Sloan Digital Sky Survey. Why the discrepancy? The fact that visually dark objects - such as asteroids - are better detected in the infrared might explain the discrepancy between visible and infrared results. For an optical telescope, the brightness of an asteroid depends on the visible light it reflects from the Sun. Observations with infrared telescopes, on the other hand, detect the 'heat' of the asteroid, which does not depend that much on the reflected sunlight, but on the absorbed sunlight. As an example, let’s consider two spheres of the same size, and located close to each other in the asteroid belt, one of which reflects ten times as much of the visible light striking it as the other. As seen by an optical telescope, the sphere which reflects more appears ten times brighter than the other sphere which might be even invisible. However, for ISO both spheres would be visible. Actually, the 'dark' sphere would appear brighter in the infrared because it would have a higher temperature (as it has absorbed more sunlight). Expert’s ‘best estimate’ Tedesco assumes that both visible and infrared searches might have their own biases, which is the reason why the given results have an error

  8. Spectroscopy of λ Bootis stars

    International Nuclear Information System (INIS)

    Heiter, U.

    2000-05-01

    λ Bootis stars are defined as metal-poor Population I A- to F-type stars, which exhibit nearly solar element abundance for C, N, O and S (e.g. Paunzen E., Weiss W.W., Heiter U. and North P., 1997, A and AS 123, 93). The classification of λ Bootis stars based on photometric indices or low resolution spectra is not sufficient for a final decision concerning a membership to this group. A detailed spectroscopic investigation is necessary to rule out stars with similar classification spectra but different abundance patterns. Therefore a program on abundance analyses of λ Bootis candidates was established, which makes use of a software package that enables the analysis of high signal-to-noise spectra with high resolution (R = 30000 to 60000). The first part of the thesis deals with the effects of using several different codes for the model atmosphere calculation on the synthetic spectra of three stars with different atmospheric parameters and degrees of underabundance. It is shown that using opacity distribution functions (ODFs) calculated for individual abundance patterns instead of pretabulated solar scaled ODFs does not change the synthetic spectra significantly. On the other hand, for the coolest star the treatment of overshooting within the calculation of the convective flux has a non-negligible influence on the derived abundance. Taking these findings into account, the results of the application of the abundance analysis tools on eleven candidate λ Bootis stars are presented in the second part of the thesis. They are based on high resolution echelle spectra obtained by the author at the Osservatorio Astronomico di Padova (Asiago, Italy). Two of these stars were found to be spectroscopic binaries during the analysis. Particular consideration is given to the estimation of the errors of the derived abundance and the problems faced when examining stars with large differences in abundance of different elements and large rotational broadening of the spectral lines

  9. New Efforts to Identify Dark Matter

    Science.gov (United States)

    Kohler, Susanna

    2016-09-01

    among them.In the early universe, small density perturbations on sub-galactic scales produce dwarf galaxies in the lambda-CDM model. But in the warm dark matter model, the longer free streaming length of the dark matter particles smooth out some of those small perturbations. This results in the formation of fewer dwarf galaxies which fits better with our current observations.Limits on Warm Dark MatterSo how can we test this alternative model? The maximum number density of dark-matter halos predicted by the warm dark matter model at a given redshift depends on the mass of the candidate dark matter particle: a larger particle mass means that more halos form. We therefore can set lower limits on the mass of dark matter particles in a two-step process:Calculate the maximum number density of dark matter halos predicted by models, andCompare this to the measured abundance of the faintest galaxies at a given redshift.Another way of looking at it: for different values of the dark matter particle mass mX, this shows the maximum number density of dark matter halos predicted at z = 6. The shaded areas represent the observed number density of faint galaxies at different confidence levels. [Menci et al. 2016]Recently, unprecedented new Hubble observations of ultra-faint, lensed galaxies in the Hubble Frontier Fields at z~6 have allowed for the discovery of more faint galaxies at this redshift than ever before. Now, a team of scientists led by Nicola Menci (INAF Rome) have used these observations to set a new limit on the lowest mass that candidate dark matter particles can have.Menci and collaborators find that these new observations constrain the particle masses to be above 2.9 keV at the 1 confidence level. These constitute the tightest constraints on the mass of candidate warm dark matter particles derived to date, and they even allow us to rule out some production mechanisms for theorized particles.Extending this analysis to other clusters with deep observations will only

  10. Galaxy Cluster Smashes Distance Record

    Science.gov (United States)

    2009-10-01

    he most distant galaxy cluster yet has been discovered by combining data from NASA's Chandra X-ray Observatory and optical and infrared telescopes. The cluster is located about 10.2 billion light years away, and is observed as it was when the Universe was only about a quarter of its present age. The galaxy cluster, known as JKCS041, beats the previous record holder by about a billion light years. Galaxy clusters are the largest gravitationally bound objects in the Universe. Finding such a large structure at this very early epoch can reveal important information about how the Universe evolved at this crucial stage. JKCS041 is found at the cusp of when scientists think galaxy clusters can exist in the early Universe based on how long it should take for them to assemble. Therefore, studying its characteristics - such as composition, mass, and temperature - will reveal more about how the Universe took shape. "This object is close to the distance limit expected for a galaxy cluster," said Stefano Andreon of the National Institute for Astrophysics (INAF) in Milan, Italy. "We don't think gravity can work fast enough to make galaxy clusters much earlier." Distant galaxy clusters are often detected first with optical and infrared observations that reveal their component galaxies dominated by old, red stars. JKCS041 was originally detected in 2006 in a survey from the United Kingdom Infrared Telescope (UKIRT). The distance to the cluster was then determined from optical and infrared observations from UKIRT, the Canada-France-Hawaii telescope in Hawaii and NASA's Spitzer Space Telescope. Infrared observations are important because the optical light from the galaxies at large distances is shifted into infrared wavelengths because of the expansion of the universe. The Chandra data were the final - but crucial - piece of evidence as they showed that JKCS041 was, indeed, a genuine galaxy cluster. The extended X-ray emission seen by Chandra shows that hot gas has been detected

  11. Europlanet Research Infrastructure: Planetary Simulation Facilities

    Science.gov (United States)

    Davies, G. R.; Mason, N. J.; Green, S.; Gómez, F.; Prieto, O.; Helbert, J.; Colangeli, L.; Srama, R.; Grande, M.; Merrison, J.

    2008-09-01

    physical properties of ice samples formed under planetary conditions to assess how rheology varies with pressure and temperature and grain size to gain a far better understanding of how tectonics may operate on icy moons. Hot planetary surfaces simulation chamber at DLR The planetary simulation chamber is to study the behaviour of planetary analogue materials on the surface of hot (airless) bodies in the solar system. Samples can be heated up to temperatures of 500°C simulating conditions found on the surface of Mercury and Venus. This enables highly accurate thermal emission measurements using the integrated infrared spectrometer and calibrated sources. Thermal gradients can be applied to samples to simulate diurnal thermal cycles and examine thermal stresses in materials. The chamber can be placed under vacuum or purged with gas. In addition, to the high temperature chamber a number of further planetary simulation chambers are available equipped with LIBS and Raman-spectroscopy equipment. Dust analogue simulation chamber at INAF/OACN This facility produces and characterises dust analogues (arc discharge, laser ablation, grinding of minerals, ices) in a variety of simulation chambers under variable pressure (10-6 - 10-3 mbar), temperature (80 - 330 K) and gas composition. Dust and analogues are characterised by a variety of Spectroscopic (absorption, transmission, diffuse-specular reflectance) and imaging techniques (SEM) and can be subjected to thermal annealing, ion bombardment and UV irradiation. Dust accelerator facility at Max Planck Institüt Nuclear Physics, Heidelberg. This facility allows the investigation of hypervelocity dust impacts onto various materials. Dust grain materials from nano to micron sizes are accelerated using a 2 MV Vande- Graaff to velocities between 1 and 60 km/s comparable to the planetary rings of the giant gas planets and impact ejecta processes on the surface of small bodies (asteroids, comets) as well as moons and planetary surfaces

  12. ESO Council Visits First VLT Unit Telescope Structure in Milan

    Science.gov (United States)

    1995-12-01

    (UT4). Mirrors and Instruments As earlier announced, ESO officially received the first 8.2-metre VLT mirror from REOSC in Paris [3] on November 21. The polishing of the second mirror has already started and, based on the experience gained with the first, it is expected that this work will be accomplished in less time. The third blank is already at REOSC and the fourth will soon be ready at Schott Glaswerke in Mainz (Germany). Following extended studies, and as yet another move towards new technology within the VLT project, it has now been decided to make the 1.2-metre secondary VLT mirrors of beryllium, a very light, exotic metal. The contracting firm is Dornier of the DASA group (Germany). This saves much weight and allows these relatively large mirrors to be efficiently used in the `chopping and tilting' mode needed for observations in the infrared wavelength region as well as for the critical, image-sharpening adaptive optics system. Significant progress has also been achieved on the first astronomical instruments which will be installed at the VLT. The integration of the first two of these, ISAAC and CONICA which will be installed on UT1 in the course of 1997, has already started in the ESO laboratories at the Headquarters in Garching. Important advances have also taken place within the FORS (managed by a consortium of Landessternwarte Heidelberg, Universitaets-Sternwarte Goettingen and Institut fuer Astronomie und Astrophysik der Ludwig Maximilians Universitaet Muenchen) and FUEGOS (Paris Observatory, Meudon Observatory, Toulouse Observatory, Geneva Observatory and Bologna Observatory) projects. More details about these and other VLT instruments will be given in later communications. Notes: [1] The Council of ESO consists of two representatives from each of the eight member states. It is the highest legislative authority of the organisation and normally meets twice a year. This time, Council was invited to Milan by the Director of the Osservatorio di Brera (Milan

  13. Charting the Giants

    Science.gov (United States)

    2004-06-01

    the very massive galaxy cluster RXCJ1131.9-1955 at redshift z = 0.306 [3] in a very rich galaxy field with two major concentrations. It was originally found by George Abell and designated "Abell 1300". The image was obtained with the ESO/MPG 2.2-m telescope and the WFI camera at La Silla. ESO PR Photo 18c/04 ESO PR Photo 18c/04 Galaxy Cluster RXCJ0937.9-2020 [Preview - JPEG: 400 x 746 pix - 60k] [Normal - JPEG: 800 x 1491 pix - 1.3M] [HiRes - JPEG: 2380 x 4437 pix - 14.2M] Caption: PR Photo 18c/04 shows the much smaller, more nearby galaxy group RXCJ0937.9-2020 at a redshift of z = 0.034 [3]. It is dominated by the massive elliptical galaxy seen at the top of the image. The photo covers only the southern part of this group. Such galaxy groups with typical masses of a few 1013 solar masses constitute the smallest objects included in the REFLEX catalogue. This image was obtained with the FORS1 multi-mode instrument on the ESO 8.2-m VLT Antu telescope. ESO PR Video Clip 05/04 ESO PR Video Clip 05/04 Galaxy Clusters in the REFLEX Catalogue (3D-visualization) [MPG - 11.7Mb] Caption: ESO PR Video Clip 05/04 illustrates the three-dimensional distribution of the galaxy clusters identfied in the ROSAT All-Sky survey in the northern and southern sky. In addition to the galaxy clusters in the REFLEX catalogue this movie also contains those identified during the ongoing, deeper search for X-ray clusters: the extension of the southern REFLEX Survey and the northern complementary survey that is conducted by the MPE team at the Calar Alto observatory and at US observatories in collaboration with John Huchra and coworkers at the Harvard-Smithonian Center for Astrophysics. In total, more than 1400 X-ray bright galaxy cluster have been found to date. (Prepared by Ferdinand Jamitzky.) Following this idea, a European team of astronomers [2], under the leadership of Hans Böhringer (MPE, Garching, Germany), Luigi Guzzo (INAF, Milano, Italy), Chris A. Collins (JMU, Liverpool), and Peter

  14. First Light with a 67-Million-Pixel WFI Camera

    Science.gov (United States)

    1999-01-01

    The newest astronomical instrument at the La Silla observatory is a super-camera with no less than sixty-seven million image elements. It represents the outcome of a joint project between the European Southern Observatory (ESO) , the Max-Planck-Institut für Astronomie (MPI-A) in Heidelberg (Germany) and the Osservatorio Astronomico di Capodimonte (OAC) near Naples (Italy), and was installed at the 2.2-m MPG/ESO telescope in December 1998. Following careful adjustment and testing, it has now produced the first spectacular test images. With a field size larger than the Full Moon, the new digital Wide Field Imager is able to obtain detailed views of extended celestial objects to very faint magnitudes. It is the first of a new generation of survey facilities at ESO with which a variety of large-scale searches will soon be made over extended regions of the southern sky. These programmes will lead to the discovery of particularly interesting and unusual (rare) celestial objects that may then be studied with large telescopes like the VLT at Paranal. This will in turn allow astronomers to penetrate deeper and deeper into the many secrets of the Universe. More light + larger fields = more information! The larger a telescope is, the more light - and hence information about the Universe and its constituents - it can collect. This simple truth represents the main reason for building ESO's Very Large Telescope (VLT) at the Paranal Observatory. However, the information-gathering power of astronomical equipment can also be increased by using a larger detector with more image elements (pixels) , thus permitting the simultaneous recording of images of larger sky fields (or more details in the same field). It is for similar reasons that many professional photographers prefer larger-format cameras and/or wide-angle lenses to the more conventional ones. The Wide Field Imager at the 2.2-m telescope Because of technological limitations, the sizes of detectors most commonly in use in

  15. Chandra and the VLT Jointly Investigate the Cosmic X-Ray Background

    Science.gov (United States)

    2001-03-01

    representative of this elusive class of objects (referred to as ' Type II Quasars ') which are believed to account for approximately 90% of the black-hole-powered quasars in the distant Universe. The 'sum' of the identified Chandra X-ray sources in the CDFS was found to match both the intensity and the spectral properties of the observed X-ray background. This important result is a significant step forward towards the definitive resolution of this long-standing cosmological problem. Naturally, ESO astronomer Piero Rosati and his colleagues are thrilled: " It is clearly the combination of the new and detailed Chandra X-ray observations and the enormous light-gathering power of the VLT that has been instrumental to this success. " However, he says, " the identification of the remaining Chandra X-ray sources will be the next challenge for the VLT since they are extremely faint. This is because they are either heavily obscured by dust or because they are extremely distant ". More Information This Press Release is issued simultaneously with a NASA Press Release (see also the Harvard site ). Some of the first results are described in a research paper ("First Results from the X-ray and Optical Survey of the Chandra Deep Field South" available on the web at astro-ph/0007240. More information about science results from the Chandra X-Ray Observatory may be found at: http://asc.harvard.edu/. The optical survey of CDFS at ESO with the Wide-Field Imager is described in connection with PR Photos 46a-b/99 ('100,000 galaxies at a glance'). An image of the Chandra Deep Field South is available at the ESO website on the EIS Image Gallery webpage. . Notes [1]: The Chandra Team is lead by Riccardo Giacconi (Association of Universities Inc. [AUI], Washington, USA) and includes: Piero Rosati , Jacqueline Bergeron , Roberto Gilmozzi , Vincenzo Mainieri , Peter Shaver (European Southern Observatory [ESO]), Paolo Tozzi , Mario Nonino , Stefano Borgani (Osservatorio Astronomico, Trieste, Italy), Guenther

  16. The VLT Unravels the Nature of the Fastest Binary Star

    Science.gov (United States)

    2002-03-01

    wave space experiment, the European Space Agency's Laser Interferometer Space Antenna (LISA) that will be launched in about 10 years' time, will be sufficiently sensitive to be able to reveal this radiation from RX J0806.3+1527 with a high degree of confidence. Such an observational feat would open an entirely new window on the universe. More information The results described in this Press Release were announced in IAU Circular 7835 and will shortly appear in print in the European research journal Astronomy & Astrophysics Letters ("RX J0806.3+1527: a double degenerate binary with the shortest known orbital period (321 s)" by G.L. Israel and co-authors), cf. astro-ph/0203043. The 5-min optical modulation was detected independently by another group led by G. Ramsay, cf. astro-ph/0203053. Note [1]: The team consists of GianLuca Israel and Luigi Stella at the Astronomical Observatory of Rome (Italy), Stefano Covino and Sergio Campana at the Astronomical Observatory of Brera (Milan, Italy), Wolfgang Hummel, Gianni Marconi and Gero Rupprecht at the European Southern Observatory, Immo Appenzeller and Otmar Stahl at the University of Heidelberg (Germany), Wolfgang Gassler and Karl-Heinz Mantel at the University of Munich (Germany), Christopher Mauche at the Lawrence Livermore National Laboratory (USA), Ulisse Munari at the Astronomical Observatory of Padua (Italy), Ignacio Negueruela at the Astronomical Observatory of Strasbourg (France), Harald Nicklas at the University of Göttingen (Germany), and Richard Smart at the Astronomical Observatory of Turin (Italy). [2]: See the research article by Israel et al. (1999, Astronomy &A, Vol. 349, p. L1). Contact GianLuca Israel Osservatorio Astronomico di Roma Italy Tel.: +39 06 9428 6437 email: gianluca@ulysses.mporzio.astro.it Technical information about the photos PR Photo 10a/02 is reproduced from FORS1-exposures, obtained in November 1999 in the U- and R-bands, and both lasting 300 sec. The field measures 2.0 x 1.5 arcmin 2. PR

  17. Dying Stars Indicate Lots of Dark Matter in Giant Galaxy

    Science.gov (United States)

    1994-04-01

    result is that these measurements also allow an estimate of how much of this giant galaxy is in the form of dark matter. From the large spread in the observed velocities of the 37 planetary nebulae, it is apparent that the total mass of NGC 1399 must be very large, and that no more than 10 percent of this mass is contained in the stars and gas we observe in it. In other words: the remaining 90 percent of the mass of NGC 1399 must consist of dark, ``invisible'' matter. This is another very clear observational confirmation of the apparent presence of dark matter in the Universe, already indicated by various other types of astronomical investigations. Although many suggestions have been made about the nature of this dark matter, nothing is known for sure at this moment. The most important implication of the existence of dark matter is that its gravitational attraction may be sufficient to ultimately stop the current expansion of the Universe. If so, the Universe will later begin to contract and probably end its present phase in a ``Big Crunch'', many billions of years from now. 1 Magda Arnaboldi Gnidica and Ken C. Freeman (Mt. Stromlo Observatory, Canberra ACT, Australia), Xiaohui Hui (Astronomy Department, California Institute of Technology, Pasadena, California, U.S.A.), Massimo Capaccioli (Dipartimento di Astronomia, Universita' di Padova, Padova, and Osservatorio Astronomico di Capodimonte, Napoli, Italy) and Holland Ford (Physics and Astronomy Department, The Johns Hopkins University, Baltimore, Maryland, U.S.A.) 2 Planetary Nebulae are formed when stars like our Sun are about to die and throw off a great shining shell of gas. This gives them the appearance of a small nebula surrounding a central star, and this is why they are called ``planetary'', although they have nothing to do with planets. 3 This light is emitted at wavelength 500.7 nm by doubly ionised oxygen atoms ([O III]) FIGURE CAPTION ESO PR PHOTO 05/94: PLANETARY NEBULAE IN NGC 1399 This photo shows some of