117 results on '"Riccardo Smareglia"'
Search Results
2. Integrated data access, visualization and analysis for Galactic Plane surveys: the VIALACTEA case.
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Sergio Molinari, Robert Butora, Stefano Cavuoti, Marco Molinaro 0003, Giuseppe Riccio, Eva Sciacca, Fabio Vitello, Ugo Becciani, Massimo Brescia, Alessandro Costa, and Riccardo Smareglia
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- 2016
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3. Application of Google Cloud Platform in Astrophysics.
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Marco Landoni, Giuliano Taffoni, Andrea Bignamini, and Riccardo Smareglia
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- 2019
4. The AstroBID: Preserving and Sharing the Italian Astronomical Heritage.
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Mauro Gargano, Antonella Gasperini, Emilia Olostro Cirella, Riccardo Smareglia, and Valeria Zanini
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- 2015
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5. Italian center for Astronomical Archives publishing solution: modular and distributed.
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Marco Molinaro 0003, Nicola F. Calabria, Robert Butora, Sonia Zorba, and Riccardo Smareglia
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- 2018
6. Enabling Grid Technologies for Simulating the Planck LFI Simulated Mission.
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Giuliano Taffoni, Davide Maino, Claudio Vuerli, Giuliano Castelli, Riccardo Smareglia, Andrea Zacchei, Torsten A. Ensslin, and Fabio Pasian
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- 2005
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7. Enabling Grid technologies for Planck space mission.
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Giuliano Taffoni, Davide Maino, Claudio Vuerli, Giuliano Castelli, Riccardo Smareglia, Andrea Zacchei, and Fabio Pasian
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- 2007
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8. The INAF Radio Data Archive: towards a modern Science Gateway
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Fabio Vitello, Cristina Knapic, Marco Molinaro, Sergio Poppi, A. Pellizzonil, E. Egron, Elisa Londero, Raimondo Concu, Alessandro Costa, Simona Righini, Mauro Nanni, M. Sponza, F. Bedosti, Sonia Zorba, Karl-Heinz Mack, Andrea Orlati, F. Tinarelli, V. Galluzzi, A. Zanichelli, Matteo Stagni, Antonietta Fara, Andrea Bignamini, Riccardo Smareglia, and ITA
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Radio telescope ,Exploit ,Distributed database ,business.industry ,Computer science ,Process (engineering) ,Big data ,Use case ,business ,Data science ,Radio astronomy ,Variety (cybernetics) - Abstract
In the Big Data era, the amount and complexity of astronomical data more and more often prevents the scientist from locally store and process her/his data. As a consequence, the geographically distributed approach to data archiving and processing is rapidly becoming a requisite. To fulfill this need, we are realizing a prototype of Science Gateway (SG) for the Italian radio telescopes. The huge amount of significantly complex and resource-demanding datasets delivered by the Italian radio telescopes and the variety of use cases from the different observing modes represent an ideal test bed for the implementation and verification of a SG environment where the scientists can exploit, manage and analyse data. To this aim, we are exploiting our previous experience in the realization of a geographically-distributed radio data archive and processing tools as well as in the design of SG prototypes. Such a coordinated approach and harmonization of resources will maximize the return for the Italian observing facilities and, moreover, will match the requirements of the international community for a state-of-the-art, highly-performant environment in which to conduct successful science.
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- 2021
9. The high-frequency upgrade of the Sardinia Radio Telescope
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Francesco Gaudiomonte, Tonino Pisanu, G. Serra, Matteo Murgia, Sergio Poppi, Raimondo Concu, Carolina Belli, P. Marongiu, Stefano Palmas, A. Scalambra, Alessandro Attoli, Mauro Pili, Antonietta Fara, Luca Schirru, Riccardo Smareglia, Franco Buffa, Giuseppe Carboni Maria, Pietro Bolli, Alessandro Orfei, S. Mariotti, Teresa Caria, I. Porceddu, Ugo Becciani, Ettore Carretti, Carlo Migoni, Andrea Orlati, J. Roda, M. Poloni, Giovanni Comoretto, A. Maccaferri, A. Poddighe, Luca Olmi, Federica Govoni, Simona Righini, Davide Fierro, Francesco Schillirò, Emilio Molinari, A. Cattani, Andrea Possenti, Pierluigi Ortu, Renzo Nesti, Luca Cresci, Fabio Vitello, Letizia Caito, Andrea Melis, A. Ladu, G. P. Vargiu, F. Fiocchi, M. Morsiani, and Alessandro Navarrini
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Computer science ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Polarimetry ,Astronomy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,law.invention ,Telescope ,Radio telescope ,Interferometry ,Upgrade ,law ,Astrophysics::Solar and Stellar Astrophysics ,Angular resolution ,Radio frequency ,Astrophysics::Galaxy Astrophysics ,Radio astronomy - Abstract
We present the status of the Sardinia Radio Telescope (SRT) and its forthcoming update planned in the next few years. The post-process scenario of the upgraded infrastructure will allow the national and international scientific community to use the SRT for the study of the Universe at high radio frequencies (up to 116 GHz), both in single dish and in interferometric mode. A telescope like SRT, operating at high frequencies, represents a unique resource for the scientific community. The telescope will be ideal for mapping quickly and with relatively high angular resolution extended radio emissions characterized by low surface brightness. It will also be essential for spectroscopic and polarimetric studies of both Galactic and extragalactic radio sources. With the use of the interferometric technique, SRT and the other Italian antennas (Medicina and Noto) will operate within the national and international radiotelescope network, allowing astronomers to obtain images of radio sources at very high angular resolution.
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- 2021
10. Status of the High-Frequency Upgrade of the Sardinia Radio Telescope
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Adelaide Ladu, Ettore Carretti, Simona Righini, Giampaolo Serra, Davide Fierro, Alessandro Attoli, Giuseppe Carboni, Antonio Poddighe, Renzo Nesti, Luca Schirru, Sergio Poppi, Riccardo Smareglia, and Giovanni Comoretto
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- 2021
11. Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field
- Author
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C. A. Volpicelli, Enrico Cascone, M. Belluso, Stefano Basso, Riccardo Smareglia, Cyril Blanpain, A. Andreis, G. Monti, M. E. Bertaina, S. Masiero, Tonino Pisanu, G. Interrante, F. Lippolis, G. Tigani Sava, G. Valente, D. Barghini, Sonia Zorba, Alberto Buzzoni, V. Gagliarducci, M. Soldi, Fabio Manca, Cristina Knapic, Cristian Carli, M. Montesarchio, Giovanni Pratesi, S. Rubinetti, D. Licchelli, T. Avoscan, A. Misiano, D. Cricchio, F. Federici, P. Colombetti, M. Romeo, G. Ascione, Daniele Gardiol, Alberto Cellino, A. Gerardi, François Colas, M. Suvieri, F. Strafella, R. Di Luca, F. Bernardi, A. Nastasi, J. L. Rault, S. Jeanne, C. Simoncelli, R. Stanga, Monica Lazzarin, C. Romeni, C. Cattaneo, S. Rasetti, Albino Carbognani, A. Malgoyre, Jader Monari, P. Demaria, Carla Taricco, M. Tombelli, Gabriele Giuli, Giuseppe Leto, A. Di Dato, N. Rizzi, M. Di Carlo, R. Serra, A. Pegoraro, Sylvain Bouley, S. Pietronave, Matteo Albani, R. Baldini, D. Guidetti, F. Salvati, M. Montemaggi, G. D’Agostino, Elisa Londero, A. Zollo, Chiara Marmo, F. Mannucci, W. Riva, J. Vaubaillon, Brigitte Zanda, Mirel Birlan, M. Rigoni, P. Morini, Jérôme Gattacceca, U. Repetti, M. Pavone, R. Zagarella, G. Cremonese, S. Meucci, S. Lera, R. Bellitto, M. D’Elia, A. Balestrero, F. Affaticati, M. De Maio, T. Carriero, R. Masi, S. Mancuso, Giovanni B. Valsecchi, Emilio Molinari, N. Pugno, R. Salerno, R. Bonino, R. Pardini, Pierre Vernazza, P. Russo, A. Bussi, V. Moggi Cecchi, C. Benna, G. M. Stirpe, K. Boros, J. Lecubin, P. Bacci, Gabriele Umbriaco, M. Costa, D. Selvestrel, E. Pace, M. Di Martino, R. Vairetti, E. Colombi, L. Betti, P. Trivero, P. Volpini, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA), Gardiol, D., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Salerno, R., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Affaticati, F., Albani, M., Andreis, A., Ascione, G., Avoscan, T., Bacci, P., Baldini, R., Balestrero, A., Basso, S., Bellitto, R., Belluso, M., Benna, C., Bernardi, F., Bertaina, M. E., Betti, L., Bonino, R., Boros, K., Bussi, A., Carli, C., Carriero, T., Cascone, E., Cattaneo, C., Cellino, A., Colombetti, P., Colombi, E., Costa, M., Cremonese, G., Cricchio, D., D'Agostino, G., D'Elia, M., De Maio, M., Demaria, P., Di Dato, A., Di Luca, R., Federici, F., Gagliarducci, V., Gerardi, A., Giuli, G., Guidetti, D., Interrante, G., Lazzarin, M., Lera, S., Leto, G., Licchelli, D., Lippolis, F., Manca, F., Mancuso, S., Mannucci, F., Masi, R., Masiero, S., Meucci, S., Misiano, A., Moggi Cecchi, V., Molinari, E., Monari, J., Montemaggi, M., Montesarchio, M., Monti, G., Morini, P., Nastasi, A., Pace, E., Pardini, R., Pavone, M., Pegoraro, A., Pietronave, S., Pisanu, T., Pugno, N., Repetti, U., Rigoni, M., Rizzi, N., Romeni, C., Romeo, M., Rubinetti, S., Russo, P., Salvati, F., Selvestrel, D., Serra, R., Simoncelli, C., Smareglia, R., Soldi, M., Stanga, R., Strafella, F., Suvieri, M., Taricco, C., Tigani Sava, G., Tombelli, M., Trivero, P., Umbriaco, G., Vairetti, R., Valente, G., Volpini, P., Zagarella, R., Zollo, A., Gardiol D., Barghini D., Buzzoni A., Carbognani A., Di Carlo M., Di Martino M., Knapic C., Londero E., Pratesi G., Rasetti S., Riva W., Salerno R., Stirpe G.M., Valsecchi G.B., Volpicelli C.A., Zorba S., Colas F., Zanda B., Bouley S., Jeanne S., Malgoyre A., Birlan M., Blanpain C., Gattacceca J., Lecubin J., Marmo C., Rault J.L., Vaubaillon J., Vernazza P., Affaticati F., Albani M., Andreis A., Ascione G., Avoscan T., Bacci P., Baldini R., Balestrero A., Basso S., Bellitto R., Belluso M., Benna C., Bernardi F., Bertaina M.E., Betti L., Bonino R., Boros K., Bussi A., Carli C., Carriero T., Cascone E., Cattaneo C., Cellino A., Colombetti P., Colombi E., Costa M., Cremonese G., Cricchio D., D'Agostino G., D'Elia M., De Maio M., Demaria P., Di Dato A., Di Luca R., Federici F., Gagliarducci V., Gerardi A., Giuli G., Guidetti D., Interrante G., Lazzarin M., Lera S., Leto G., Licchelli D., Lippolis F., Manca F., Mancuso S., Mannucci F., Masi R., Masiero S., Meucci S., Misiano A., Moggi Cecchi V., Molinari E., Monari J., Montemaggi M., Montesarchio M., Monti G., Morini P., Nastasi A., Pace E., Pardini R., Pavone M., Pegoraro A., Pietronave S., Pisanu T., Pugno N., Repetti U., Rigoni M., Rizzi N., Romeni C., Romeo M., Rubinetti S., Russo P., Salvati F., Selvestrel D., Serra R., Simoncelli C., Smareglia R., Soldi M., Stanga R., Strafella F., Suvieri M., Taricco C., Tigani Sava G., Tombelli M., Trivero P., Umbriaco G., Vairetti R., Valente G., Volpini P., Zagarella R., Zollo A., and ITA
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meteoroids -methods: data analysis -techniques: image processing ,010502 geochemistry & geophysics ,01 natural sciences ,Strewn field ,meteorites ,0103 physical sciences ,meteors ,meteoroids ,010303 astronomy & astrophysics ,meteoroid ,0105 earth and related environmental sciences ,Physics ,Meteoroid ,image processing ,methods: data analysis ,techniques ,meteor ,Astronomy ,Astronomy and Astrophysics ,meteorite ,Meteorite ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,data analysi [methods] ,Trajectory ,Orbit (control theory) - Abstract
Two meteorite pieces have been recovered in Italy, near the town of Cavezzo (Modena), on 2020 January 4th. The associated fireball was observed on the evening of New Year’s Day 2020 by eight all-sky cameras of the PRISMA fireball network, a partner of FRIPON. The computed trajectory had an inclination angle of approximately 68° and a velocity at infinity of 12.8 km s−1. Together with the relatively low terminal height, estimated as 21.5 km, those values were indicating the significant possibility of a meteorite dropping event, as additionally confirmed by the non-zero residual total mass. The strewn-field was computed taking into account the presence of two bright light flashes, revealing that the meteoroid had been very likely subject to fragmentation. Three days after the event, two samples, weighing 3.1 and 52.2 g, were collected as a result of a dedicated field search and thanks to the involvement of the local people. The two pieces were immediately recognized as freshly fallen fragments of meteorite. The computed orbital elements, compared with the ones of known Near-Earth Asteroids from the NEODyS database, are compatible with one asteroid only; 2013 VC10. The estimated original mass of the meteoroid, 3.5 kg, and size, approximately 13 cm, is so far the smallest among the current 35 cases in which meteorites were recovered from precise strewn-field computation thanks to observational data. This result demonstrates the effectiveness of accurate processing of fireball network data even on challenging events generated by small size meteoroids.
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- 2021
12. Neutral Iron Emission Lines From The Day-side Of KELT-9b -- The GAPS Programme With HARPS-N At TNG XX
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Luca Malavolta, Alessandro Sozzetti, A. F. Lanza, C. Lovis, Riccardo Claudi, B. Lavie, I. Pagano, P. Giacobbe, A. S. Bonomo, Lorenzo Pino, Aldo F. M. Fiorenzano, Giampaolo Piotto, Jean-Michel Desert, Luca Fossati, Marco Pedani, Aurélien Wyttenbach, Mario Damasso, Giuseppina Micela, Francesco Borsa, G. Frustagli, David Ehrenreich, G. Scandariato, M. Rainer, Matteo Brogi, Ilaria Carleo, Riccardo Smareglia, Antonio Maggio, Domenico Nardiello, A. Bignamini, L. Di Fabrizio, A. Magazzu, Romain Allart, E. Covino, G. Bruno, Luigi Mancini, Rosario Cosentino, Laura Affer, Silvano Desidera, Ennio Poretti, Jens Hoeijmakers, K. Biazzo, Vatsal Panwar, V. Nascimbeni, G. Leto, Avet Harutyunyan, S. Benatti, Michael R. Line, Luca Borsato, J. Maldonado, Elisa Molinari, Low Energy Astrophysics (API, FNWI), Pino, L, Desert, J, Brogi, M, Malavolta, L, Wyttenbach, A, Line, M, Hoeijmakers, J, Fossati, L, Bonomo, A, Nascimbeni, V, Panwar, V, Affer, L, Benatti, S, Biazzo, K, Bignamini, A, Borsa, F, Carleo, I, Claudi, R, Cosentino, R, Covino, E, Damasso, M, Desidera, S, Giacobbe, P, Harutyunyan, A, Lanza, A, Leto, G, Maggio, A, Maldonado, J, Mancini, L, Micela, G, Molinari, E, Pagano, I, Piotto, G, Poretti, E, Rainer, M, Scandariato, G, Sozzetti, A, Allart, R, Borsato, L, Bruno, G, Fabrizio, L, Ehrenreich, D, Fiorenzano, A, Frustagli, G, Lavie, B, Lovis, C, Magazz, A, Nardiello, D, Pedani, M, and Smareglia, R
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astro-ph.SR ,010504 meteorology & atmospheric sciences ,Continuum (design consultancy) ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,01 natural sciences ,Exoplanet atmospheres ,Exoplanet atmospheric composition ,High resolution spectroscopy ,Atmosphere ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,Spectral resolution ,010303 astronomy & astrophysics ,Spectrograph ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Line (formation) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Settore FIS/05 ,Astronomy and Astrophysics ,Exoplanet ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,astro-ph.EP ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,astro-ph.IM - Abstract
We present the first detection of atomic emission lines from the atmosphere of an exoplanet. We detect neutral iron lines from the day-side of KELT-9b (Teq $\sim$ 4, 000 K). We combined thousands of spectrally resolved lines observed during one night with the HARPS-N spectrograph (R $\sim$ 115, 000), mounted at the Telescopio Nazionale Galileo. We introduce a novel statistical approach to extract the planetary parameters from the binary mask cross-correlation analysis. We also adapt the concept of contribution function to the context of high spectral resolution observations, to identify the location in the planetary atmosphere where the detected emission originates. The average planetary line profile intersected by a stellar G2 binary mask was found in emission with a contrast of 84 $\pm$ 14 ppm relative to the planetary plus stellar continuum (40 $\pm$ 5$\%$ relative to the planetary continuum only). This result unambiguously indicates the presence of an atmospheric thermal inversion. Finally, assuming a modelled temperature profile previously published (Lothringer et al. 2018), we show that an iron abundance consistent with a few times the stellar value explains the data well. In this scenario, the iron emission originates at the $10^{-3}$-$10^{-5}$ bar level., Comment: Accepted for publication on ApJL; 19 pages, 4 figures, 3 tables
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- 2020
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13. Immuni e privacy: il parere di un astroinformatico
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Riccardo Smareglia
- Abstract
Negli ultimi giorni l’app Immuni, dopo l’appello del presidente del Consiglio a scaricarla, è di nuovo al centro dell’attenzione. Molti si domandano quanto sia o meno invasiva per la privacy. Media Inaf lo ha chiesto a Riccardo Smareglia, responsabile Ict e Science Data Management dell’Inaf
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- 2020
- Full Text
- View/download PDF
14. The GAPS Programme with HARPS-N at TNG: . Atmospheric Rossiter-McLaughlin effect and improved parameters of KELT-9b
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Riccardo Claudi, Rosario Cosentino, Avet Harutyunyan, Antonio Maggio, Andrea Bignamini, Aldo F. M. Fiorenzano, Cristina Knapic, Luca Fossati, Jesus Maldonado, Paolo Giacobbe, Mario Damasso, Roxanne Ligi, Marco Pedani, Giampaolo Piotto, Alessandro Sozzetti, Katia Biazzo, S. Masiero, F. Borsa, Matteo Brogi, Emilio Molinari, Monica Rainer, Gloria Andreuzzi, Luigi Mancini, Luca Malavolta, Massimiliano Esposito, Serena Benatti, Elvira Covino, D. Barbato, A. Garrido Rubio, Silvano Desidera, Antonino F. Lanza, Lorenzo Pino, L. Affer, Valerio Nascimbeni, Ilaria Carleo, Giuseppe Leto, Giuseppina Micela, Isabella Pagano, E. González-Álvarez, Ennio Poretti, Riccardo Smareglia, Aldo S. Bonomo, Gaetano Scandariato, Low Energy Astrophysics (API, FNWI), ITA, USA, GBR, DEU, ESP, and AUT
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010504 meteorology & atmospheric sciences ,Rossiter–McLaughlin effect ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Spectral line ,Atmosphere ,techniques: radial velocities ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,planetary systems ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,planets and satellites: atmospheres ,Physics ,Settore FIS/05 ,Astronomy and Astrophysics ,Planetary system ,stars: individual: KELT-9 ,Exoplanet ,Radial velocity ,Amplitude ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Planetary mass ,techniques: spectroscopic ,Astrophysics - Earth and Planetary Astrophysics - Abstract
In the framework of the GAPS project, we observed the planet-hosting star KELT-9 (A-type star, VsinI$\sim$110 km/s) with the HARPS-N spectrograph at the TNG. In this work we analyse the spectra and the extracted radial velocities (RVs), to constrain the physical parameters of the system and to detect the planetary atmosphere of KELT-9b. We extracted from the high-resolution optical spectra the mean stellar line profiles with an analysis based on the Least Square Deconvolution technique. Then, we computed the stellar RVs with a method optimized for fast rotators, by fitting the mean stellar line profile with a purely rotational profile instead of using a Gaussian function. The new spectra and analysis led us to update the orbital and physical parameters of the system, improving in particular the value of the planetary mass to $M_{\rm p}=2.88\pm0.35\,M_{\rm Jup}$. We discovered an anomalous in-transit RV deviation from the theoretical Rossiter-McLaughlin effect solution, calculated from the projected spin-orbit angle $\lambda=-85.78\pm0.46$ degrees measured with Doppler tomography. We prove that this deviation is caused by the planetary atmosphere of KELT-9b, thus we name this effect Atmospheric Rossiter-McLaughlin effect. By analysing the magnitude of the RV anomaly, we obtained information on the extension of the planetary atmosphere as weighted by the model used to retrieve the stellar mean line profiles, which is up to $1.22\pm0.02\,R_{\rm p}$. The Atmospheric Rossiter-McLaughlin effect will be observable for other exoplanets whose atmosphere has non-negligible correlation with the stellar mask used to retrieve the RVs, in particular ultra-hot Jupiters with iron in their atmosphere. The duration and amplitude of the effect will depend not only on the extension of the atmosphere, but also on the in-transit planetary RVs and on the projected rotational velocity of the parent star., Comment: accepted for publication in A&A. Language edited version
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- 2019
15. A new archival infrastructure for highly-structured astronomical data
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M. Sponza, Riccardo Smareglia, Erik Dovgan, and Cristina Knapic
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Multimedia ,010308 nuclear & particles physics ,Computer science ,computer.internet_protocol ,business.industry ,Big data ,Data discovery ,Astronomy and Astrophysics ,Virtual observatory ,computer.software_genre ,01 natural sciences ,Data modeling ,Radio telescope ,Space and Planetary Science ,0103 physical sciences ,Very-long-baseline interferometry ,Persistent data structure ,business ,010303 astronomy & astrophysics ,computer ,XML - Abstract
With the advent of the 2020 Radio Astronomy Telescopes era, the amount and format of the radioastronomical data is becoming a massive and performance-critical challenge. Such an evolution of data models and data formats require new data archiving techniques that allow massive and fast storage of data that are at the same time also efficiently processed. A useful expertise for efficient archiviation has been obtained through data archiving of Medicina and Noto Radio Telescopes. The presented archival infrastructure named the Radio Archive stores and handles various formats, such as FITS, MBFITS, and VLBI’s XML, which includes description and ancillary files. The modeling and architecture of the archive fulfill all the requirements of both data persistence and easy data discovery and exploitation. The presented archive already complies with the Virtual Observatory directives, therefore future service implementations will also be VO compliant. This article presents the Radio Archive services and tools, from the data acquisition to the end-user data utilization.
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- 2018
16. Asiago Astronomical Archive: Status and Features
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Elisa Londero, Sonia Zorba, Marco Molinaro, Cristina Knapic, Lina Tomasella, Aldo Frigo, Riccardo Smareglia, and ITA
- Abstract
We present the new archiving system that has been installed at INAF OAPd - Asiago Observatory. Its main features comprise fast and reliable distribution capabilities, prompt monitoring and easy access to the data through a newly-designed web-interface.
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- 2019
17. The GAPS Programme with HARPS-N at TNG. XVIII. Two new giant planets around the metal-poor stars HD 220197 and HD 233832
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Jesus Maldonado, Luca Malavolta, Nuno C. Santos, A. F. Martinez Fiorenzano, Paolo Giacobbe, Ennio Poretti, João P. Faria, S. Masiero, Marco Molinaro, E. González-Álvarez, Avet Harutyunyan, Valerio Nascimbeni, Giuseppina Micela, Riccardo Smareglia, Raffaele Gratton, Rosario Cosentino, E. Molinari, Giampaolo Piotto, Antonio Maggio, Monica Rainer, L. Di Fabrizio, Andrea Bignamini, Marco Pedani, Riccardo Claudi, F. Borsa, Luigi Mancini, Aldo S. Bonomo, Serena Benatti, Alessandro Sozzetti, D. Barbato, L. Affer, I. Carleo, Silvano Desidera, Isabella Pagano, Mario Damasso, Elvira Covino, Antonino F. Lanza, Giuseppe Leto, Katia Biazzo, M. Esposito, Gaetano Scandariato, L. S. Colombo, and Matteo Pinamonti
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Stars: Individual: HD 220197 ,010504 meteorology & atmospheric sciences ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,01 natural sciences ,Settore FIS/05 - Astronomia e Astrofisica ,Planet ,Methods: Data analysis ,0103 physical sciences ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Planetary systems ,Stars: Abundances ,Stars: Individual: HD 233832 ,Techniques: Radial velocities ,Astronomy and Astrophysics ,Space and Planetary Science ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Giant planet ,Planetary system ,Orbital period ,Exoplanet ,Orbit ,Stars ,13. Climate action ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Statistical studies of exoplanets have shown that giant planets are more commonly hosted by metal-rich dwarf stars than low-metallicity ones, while such a correlation is not evident for lower-mass planets. The search for giant planets around metal-poor stars and the estimate of their occurrence $f_p$ is an important element in providing support to models of planet formation. We present results from the HARPS-N search for giant planets orbiting metal-poor ($-1.0\leq[Fe/H]\leq-0.5$ dex) stars in the northern hemisphere complementing a previous HARPS survey on southern stars in order to update the estimate of $f_p$. High-precision HARPS-N observations of 42 metal-poor stars are used to search for planetary signals to be fitted using differential evolution MCMC single-Keplerian models. We then join our detections to the results of the previous HARPS survey on 88 metal-poor stars to provide a preliminar estimate of the two-hemisphere $f_p$. We report the detection of two new giant planets around HD 220197 and HD 233832. The first companion has M$\sin{i}=0.20_{-0.04}^{+0.07}$ M$_{\rm Jup}$ and orbital period of $1728_{-80}^{+162}$ days, and for the second companion we find two solutions of equal statistical weight having periods $2058_{-40}^{+47}$ and $4047_{-117}^{+91}$ days and minimum masses of $1.78_{-0.06}^{+0.08}$ and $2.72_{-0.23}^{+0.23}$ M$_{\rm Jup}$, respectively. Joining our two detections with the three from the southern survey we obtain a preliminary and conservative estimate of global frequency of $f_p=3.84_{-1.06}^{+2.45}\%$ for giant planets around metal-poor stars. The two new giant planets orbit dwarf stars at the metal-rich end of the HARPS-N metal-poor sample, corroborating previous results suggesting that giant planet frequency still is a rising function of host star [Fe/H]. We also note that all detections in the overall sample are giant long-period planets., Comment: 15 pages, 8 figures, 5 tables, accepted for publication in A&A
- Published
- 2019
18. Integrated data access, visualization and analysis for Galactic Plane surveys: the VIALACTEA case
- Author
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Stefano Cavuoti, Riccardo Smareglia, Giuseppe Riccio, Eva Sciacca, Alessandro Costa, Fabio Vitello, Massimo Brescia, Sergio Molinari, Marco Molinaro, Ugo Becciani, Robert Butora, Massimo Brescia, S. G. Djorgovski, Eric D. Feigelson, Giuseppe Longo, Stefano Cavuoti, Molinari, S., Butora, R., Cavuoti, S., Molinaro, M., Riccio, G., Sciacca, E., Vitello, F., Becciani, U., Brescia, M., Costa, A., and Smareglia, R.
- Subjects
Physics ,Visual analytics ,010308 nuclear & particles physics ,Star formation ,Milky Way ,Extinction (astronomy) ,astronomical data bases: miscellaneous, methods: data analysis, stars: formation ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Galactic plane ,01 natural sciences ,Galaxy ,Visualization ,Metadata ,Space and Planetary Science ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
The VIALACTEA project brings to a common forum the major new-generation surveys of the Milky Way Galactic Plane from 1μm to the radio, both in thermal continuum and in atomic and molecular lines, to attack in a systematic way the characterization of the Milky Way as a star formation engine. Images, catalogues, spectroscopic datacubes and radiative transfer models of the Spectral Energy Distributions (SEDs) of sites of star formation have been incorporated and indexed in the VIALACTEA Knowledge Base (VLKB). The VLKB consists of a combination of a relational database where the VIALACTEA data and metadata are homogenised and stored, and a filesystem-based stored information. This infrastructure allowed, among others, the generation of extensive catalogue for compact sources and extended structures in the Galactic Plane, the implementation of data-mining algorithms for the band-merging of multiwavelength data and expert systems for the automated analysis of molecular line surveys to extract critical kinematical information and derive distances using Galaxy rotation curves and new 3D extinction maps. A new VIALACTEA 3D Visual Analytics interface has been developed that provides integrated access and analysis of continuum and spectroscopic images together with catalogue data directly interfacing with the VLKB.
- Published
- 2016
19. Achieving a rolled-up view of SKA TM health status and state: definition and analysis of aggregation methods
- Author
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Matteo Canzari, Riccardo Smareglia, Mauro Dolci, and Matteo Di Carlo
- Subjects
System requirements ,Data aggregator ,Operator (computer programming) ,Computer science ,Aggregate (data warehouse) ,Systems architecture ,Dependability ,State (computer science) ,Performance indicator ,Reliability engineering - Abstract
One basic system requirement for the SKA Project is aimed to providing both a rolled-up and a drilled-down view of the Operational (Health) Status, as well as the State, for each Element. The first one is a performance indicator that must be properly structured in order an operator can understand it. The second one is a logic enumerative that has to contain at least the following values: start-up, shutdown, standby and operational. In this paper an aggregation algorithm, defined for the Health Status of the SKA Telescope Manager (TM) but abstract enough in order to be extended to a generic complex system, is analyzed in terms of the three main indications it has to provide: fully operating, degraded performance, faulty. The analysis shows that the distinction among critical and non-critical components, along with their state and weight on the overall system, is enough to completely achieve a rolled-up view of the system. System architecture only affects the weights, which are the result of a dependability analysis initially performed on the system itself. The aggregation can be applied to selected subsets of components, so providing hints for a drilling-down of the monitoring data, when this is necessary. Finally, using the algorithm to aggregate the states essentially fails: a different approach based on logic relationships will have to be adopted in order to manage states, but to this purpose an important role can be played by the aggregated health status.
- Published
- 2018
20. HDB@ELK: another noSql customization for the HDB++ archiving system
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Mauro Dolci, M. Di Carlo, Matteo Canzari, Riccardo Smareglia, and ITA
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Database ,Computer science ,Software system ,Architecture ,computer.software_genre ,NoSQL ,computer ,Term (time) ,Personalization - Abstract
The TANGO controls framework community has put a lot of effort in creating the HDB++ software system that is an high performance, event-driven archiving system. Its design allows storing data into traditional database management systems such as MySQL as well as NoSQL database such as Apache Cassandra. The architecture allow also to easily extend it to other noSql database like, for instance, ELK. This paper describes the step needed to extend the HDB++ and explore the possibilities to use the ELK technology in term of analysis being enabled and tools provided.
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- 2018
21. A GUI prototype for SKA1 TM services: compliance with user-centered design approach
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Matteo Canzari, Sergio Poppi, Mauro Dolci, I. Khokhriakov, Riccardo Smareglia, and M. Di Carlo
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business.industry ,Computer science ,Word error rate ,Usability ,computer.software_genre ,01 natural sciences ,Control room ,010309 optics ,0103 physical sciences ,Scalability ,Web application ,Plug-in ,business ,Software engineering ,010303 astronomy & astrophysics ,computer ,User-centered design ,Graphical user interface - Abstract
Adopting the recommendations for the control room obtained by a user-centered design approach for the Square Kilometer Array (SKA), the following characteristics for the SKA Graphical User Interface (GUI) have been identified: scalability, integrated tools, extendability and completeness. The lack of one or more of these characteristics could lead to usability problems like low user’s efficiency, high error rate, high user’s mental load and user’s frustration. In this paper one of the most recent web technologies that enable the user-centered design are analyzed. TangoWebApp, a pluggable web platform integrated with TANGO Control REST API, appears very suitable also taking into account the adoption of TANGO as the SKA control framework. Starting from a SKA Telescope Manager (TM) Services use case, a prototype has been developed composed by a series of TANGO WebApp plugins that allow the operator to correctly and efficiently complete the tasks of the scenario. Some of the plugins, in particular, have been developed to extend the functionalities of the TANGO WebApp itself to make it fully compliant with the User Centered Design. As a result of this work, the TangoWebapp proved itself not only fully compliant with the User Centered Design, but also flexible enough to add functionalities in the form of properly developed plugins. These characteristics of the TangoWebapp, together with its unique feature to be integrated into TANGO, make it a good candidate to be the SKA GUI platform.
- Published
- 2018
22. The GAPS programme with HARPS-N at TNG XVI. Measurement of the Rossiter-McLaughlin effect of transiting planetary systems HAT-P-3, HAT-P-12, HAT-P-22, WASP-39, and WASP-60
- Author
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Andrea Bignamini, Riccardo Smareglia, Marco Pedani, Luca Malavolta, Isabella Pagano, Ivan Bruni, Jesus Maldonado, John Southworth, Antonio Maggio, Alexis M. S. Smith, Matteo Brogi, Giampaolo Piotto, Aldo S. Bonomo, S. Masiero, R. Cosentino, Laura Affer, E. Gonzalez-Alvarez, Emilio Molinari, Riccardo Claudi, E. Covino, Raffaele Gratton, Serena Benatti, Alessandro Sozzetti, Gloria Andreuzzi, Th. Henning, Giuseppe Leto, Gaetano Scandariato, A. Martinez-Fiorenzano, Giuseppina Micela, C. Boccato, I. Carleo, Daniel F. Evans, A. F. Lanza, Monica Rainer, Avet Harutyunyan, P. Giacobbe, M. Esposito, Paula Sarkis, F. Borsa, Silvano Desidera, K. Biazzo, Luigi Mancini, Valerio Nascimbeni, E. Poretti, Simona Ciceri, Mario Damasso, and ITA
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Rotation period ,Orbital plane ,Extrasolar planets – Stars: late-type ,WASP-60 ,Rossiter–McLaughlin effect ,FOS: Physical sciences ,HAT-P-22 ,Astrophysics ,photometric – Stars: individual: HAT-P-3 ,01 natural sciences ,Settore FIS/05 - Astronomia e Astrofisica ,0103 physical sciences ,Hot Jupiter ,QB460 ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,HAT-P-12 ,Astronomy and Astrophysics ,Planetary system ,Light curve ,Exoplanet ,HAT-P-39 ,Radial velocity ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,fundamental parameters – Techniques: radial velocities ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We characterised five transiting planetary systems (HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60) and determined their sky-projected planet orbital obliquity through the measurement of the RM effect. We used HARPS-N high-precision radial velocity measurements, gathered during transit events, to measure the RM effect in the target systems and determine the sky-projected angle between the planetary orbital plane and the stellar equator. The characterisation of stellar atmospheric parameters was performed exploiting the HARPS-N spectra, using line equivalent width ratios, and spectral synthesis methods. Photometric parameters of the five transiting exoplanets were re-analysed through 17 new light curves, obtained with an array of medium-class telescopes, and other light curves from the literature. Survey-time-series photometric data were analysed for determining the rotation periods of the five stars and their spin inclination. From the analysis of the RM effect we derived a sky-projected obliquity of 21.2 degree, -54 degree, -2.1 degree, 0 degree and -129 degree for HAT-P-3b, HAT-P-12b, HAT-P-22b, WASP-39b and WASP-60b, respectively. The latter value indicates that WASP-60b is moving on a retrograde orbit. These values represent the first measurements of \lambda for the five exoplanetary systems under study. The stellar activity of HAT-P-22 indicates a rotation period of 28.7 days, which allowed us to estimate the true misalignment angle of HAT-P-22b, \psi=24 degree. The revision of the physical parameters of the five exoplanetary systems returned values that are fully compatible with those existing in the literature. The exception to this is the WASP-60 system, for which, based on higher quality spectroscopic and photometric data, we found a more massive and younger star and a larger and hotter planet., Comment: 21 pages, 10 figure, accepted for publication in Astronomy & Astrophysics
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- 2018
23. Eyes on K2-3: A system of three likely sub-Neptunes characterized with HARPS-N and HARPS
- Author
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Nuno C. Santos, Giampaolo Piotto, Damien Ségransan, David F. Phillips, Andrew Vanderburg, L. Di Fabrizio, Courtney D. Dressing, Riccardo Smareglia, Luigi Mancini, David Charbonneau, Francesco Pepe, Antonio Maggio, Valerio Nascimbeni, Annelies Mortier, E. Poretti, Mercedes López-Morales, Gaetano Scandariato, Ilaria Carleo, R. Cosentino, Andrew Collier Cameron, Ken Rice, Stéphane Udry, Pedro Figueira, Michel Mayor, Andrea Bignamini, M. Esposito, S. Masiero, Giuseppe Leto, Jonathan Irwin, E. González-Álvarez, Serena Benatti, Alessandro Sozzetti, X. Delfosse, Rim Fares, F. Borsa, Fatemeh Motalebi, A. Wünsche, J. Maldonado, Monica Rainer, X. Bonfils, T. Forveille, Christopher A. Watson, Mario Damasso, Eric D. Lopez, F. Bouchy, Christophe Lovis, Dimitar Sasselov, Aldo S. Bonomo, Jose-Manuel Almenara, Emilio Molinari, Riccardo Claudi, Isabella Pagano, E. Covino, Silvano Desidera, K. Biazzo, Raphaëlle D. Haywood, Giuseppina Micela, David W. Latham, Felipe Murgas, Raffaele Gratton, Lars A. Buchhave, Ararat Harutyunyan, J. Asher Johnson, P. Giacobbe, Aldo F. M. Fiorenzano, Luca Malavolta, Li Zeng, Nicola Astudillo-Defru, A. F. Lanza, Laura Affer, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Universidad de Concepción [Chile], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Osaka City University Advanced Mathematical Institute (OCAMI), Osaka Media Center, University of Granada/Dept of Paediatrics, University of Granada [Granada], INAF - Osservatorio Astrofisico di Catania (OACT), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, INAF - Osservatorio Astrofisico di Arcetri (OAA), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of St Andrews [Scotland], INAF - Osservatorio Astronomico di Padova (OAPD), Telescopio Nazionale Galileo (TNG), RN, Sciences pour l'environnement (SPE), Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Osserv Astrofis Catania, Ist Nazl Astrofis, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), INAF - Osservatorio Astronomico di Palermo (OAPa), INAF - Osservatorio Astronomico di Brera (OAB), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Universidade do Porto [Porto], Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Harvard University [Cambridge]-Smithsonian Institution, Osservatorio Astronomico di Brera, Osaka City university Advanced Mathematical Institute [Osaka] (OCAMI), Osaka City University (OCU), European Commission, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Universidad de Concepción - University of Concepcion [Chile], SUPA School of Physics and Astronomy [University of St Andrews], University of St Andrews [Scotland]-Scottish Universities Physics Alliance (SUPA), Universidad de Granada = University of Granada (UGR), Università degli Studi di Padova = University of Padua (Unipd), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Harvard University-Smithsonian Institution, and Université de Genève = University of Geneva (UNIGE)
- Subjects
individual: K2-3 [stars] ,planets and satellites: detection ,detection [planets and satellites] ,fundamental parameters [Planets and satellites] ,FOS: Physical sciences ,Astrophysics ,stars: individual: 2MASS 11292037-0127173 ,01 natural sciences ,individual: EPIC 201367065 [stars] ,Settore FIS/05 - Astronomia e Astrofisica ,Planet ,0103 physical sciences ,techniques: radial velocities ,QB Astronomy ,stars: individual: K2-3 ,composition [planets and satellites] ,010303 astronomy & astrophysics ,QC ,QB ,individual: 2MASS 11292037-0127173 [stars] ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,stars: individual: EPIC 201367065 ,Planetary habitability ,010308 nuclear & particles physics ,Stellar rotation ,planets and satellites: composition ,radial velocities [techniques] ,Astronomy and Astrophysics ,3rd-DAS ,Orbital period ,Radial velocity ,Stars ,individual: K2-3 (2MASS 11292037-0127173, EPIC 201367065) [Stars] ,QC Physics ,Amplitude ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics::Earth and Planetary Astrophysics ,Circumstellar habitable zone ,Astrophysics - Earth and Planetary Astrophysics - Abstract
M-dwarf stars are promising targets for identifying and characterizing potentially habitable planets. K2-3 is a nearby (45 pc), early-type M dwarf hosting three small transiting planets, the outermost of which orbits close to the inner edge of the stellar (optimistic) habitable zone. The K2-3 system is well suited for follow-up characterization studies aimed at determining accurate masses and bulk densities of the three planets. Using a total of 329 radial velocity measurements collected over 2.5 years with the HARPS-N and HARPS spectrographs and a proper treatment of the stellar activity signal, we aim to improve measurements of the masses and bulk densities of the K2-3 planets. We use our results to investigate the physical structure of the planets. We analyse radial velocity time series extracted with two independent pipelines by using Gaussian process regression. We adopt a quasi-periodic kernel to model the stellar magnetic activity jointly with the planetary signals. We use Monte Carlo simulations to investigate the robustness of our mass measurements of K2-3\,c and K2-3\,d, and to explore how additional high-cadence radial velocity observations might improve them. Despite the stellar activity component being the strongest signal present in the radial velocity time series, we are able to derive masses for both planet b ($M_{\rm b}=6.6\pm1.1$ $M_{\rm \oplus}$) and planet c ($M_{\rm c}=3.1^{+1.3}_{-1.2}$ $M_{\rm \oplus}$). The Doppler signal due to K2-3\,d remains undetected, likely because of its low amplitude compared to the radial velocity signal induced by the stellar activity. The closeness of the orbital period of K2-3\,d to the stellar rotation period could also make the detection of the planetary signal complicated. [...], 14 pages, 15 figures, accepted for publication in A&A
- Published
- 2018
24. KAFE: the Key-analysis Automated FITS-images Explorer
- Author
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Matteo Bonato, S. Burkutean, Quirino D'Amato, Kazi L.J. Rygl, V. Galluzzi, Cristina Knapic, Riccardo Smareglia, Claudia Mancuso, A. Giannetti, Felix Stoehr, Marcella Massardi, Elisabetta Liuzzo, Jan Brand, and F. Bedosti
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Information retrieval ,010308 nuclear & particles physics ,Computer science ,Mechanical Engineering ,Astronomy and Astrophysics ,Image processing ,01 natural sciences ,Electronic, Optical and Magnetic Materials ,Metadata ,Space and Planetary Science ,Control and Systems Engineering ,0103 physical sciences ,010303 astronomy & astrophysics ,Instrumentation - Abstract
We present KAFE—the Key-analysis Automated FITS-images Explorer. KAFE is a web-based FITS image postprocessing analysis tool designed to be applicable in the radio to sub-mm wavelength domain. KAFE was developed to complement selected FITS files with metadata based on a uniform image analysis approach as well as to provide advanced image diagnostic plots. It is ideally suited for data mining purposes and multiwavelength/multi-instrument data samples that require uniform data diagnostic criteria. We present the code structure and interface, the keyword definitions, the products generated for selected users’ science cases, and application examples.
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- 2018
25. Vialactea Visual Analytics Tool for Star Formation Studies of the Galactic Plane
- Author
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Stefano Cavuoti, Marco Molinaro, Robert Butora, Fabio Vitello, Ugo Becciani, Riccardo Smareglia, A. Di Giorgio, Marilena Bandieramonte, E. Schisano, Massimo Brescia, S. J. Liu, Davide Elia, Eva Sciacca, Milena Benedettini, Sergio Molinari, Alessandro Costa, Giuseppe Riccio, ITA, Vitello, F., Sciacca, E., Becciani, U., Costa, A., Bandieramonte, M., Benedettini, M., Brescia, M., Butora, R., Cavuoti, S., Di Giorgio, A. M., Elia, D., Liu, S. J., Molinari, S., Molinaro, M., Riccio, G., Schisano, E., and Smareglia, R.
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Visual analytics ,Exploit ,Computer science ,Milky Way ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,02 engineering and technology ,01 natural sciences ,Space exploration ,0103 physical sciences ,0202 electrical engineering, electronic engineering, information engineering ,media_common.cataloged_instance ,European union ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,Star formation ,Suite ,Astronomy and Astrophysics ,Galactic plane ,Data science ,Galaxy: structure, methods: data analysis, stars: formation, surveys, techniques: image processing, Online material: color figures ,Space and Planetary Science ,020201 artificial intelligence & image processing ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 607380 (VIALACTEA) and from the European Commissions Horizon 2020 research and innovation programme under the grant agreement No. 739563 (EOSCPilot.eu) We present a visual analytics tool, based on the VisIVO suite, to exploit a combination of all new-generation surveys of the Galactic Plane to study the star formation process of the Milky Way. The tool has been developed within the VIALACTEA project, founded by the 7th Framework Programme of the European Union, that creates a common forum for the major new-generation surveys of the Milky Way Galactic Plane from the near-infrared to the radio, both in thermal continuum and molecular lines. Massive volumes of data are produced by space missions and ground-based facilities and the ability to collect and store them is increasing at a higher pace than the ability to analyze them. This gap leads to new challenges in the analysis pipeline to discover information contained in the data. Visual analytics focuses on handling these massive, heterogeneous, and dynamic volumes of information accessing the data previously processed by data mining algorithms and advanced analysis techniques with highly interactive visual interfaces offering scientists the opportunity for in-depth understanding of massive, noisy, and high-dimensional data.
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- 2018
26. The GAPS Programme with HARPS-N at TNG XV. A substellar companion around a K giant star identified with quasi-simultaneous HARPS-N and GIANO measurements
- Author
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Jesus Maldonado, Giampaolo Piotto, Aldo S. Bonomo, A. F. Lanza, Gaetano Scandariato, Silvano Desidera, Serena Benatti, Alessandro Sozzetti, Monica Rainer, Antonio Maggio, Luca Malavolta, E. González-Álvarez, Giuseppina Micela, A. Martinez-Fiorenzano, Paolo Giacobbe, Marco Pedani, Isabella Pagano, Riccardo Smareglia, F. Massi, Raffaele Gratton, Nicoletta Sanna, S. Masiero, Valerio Nascimbeni, Emilio Molinari, Riccardo Claudi, E. Poretti, I. Carleo, Ernesto Oliva, M. Esposito, Elvira Covino, Katia Biazzo, Valentina D'Orazi, Mario Damasso, R. Cosentino, Avet Harutyunyan, F. Borsa, Laura Affer, ITA, and ESP
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Physics ,stars: individual: TYC 4282-605-1 ,010308 nuclear & particles physics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics ,Planetary system ,Light curve ,Giant star ,01 natural sciences ,Radial velocity ,Amplitude ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Planet ,techniques: radial velocities ,0103 physical sciences ,Thick disk ,infrared: stars ,planetary systems ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Context. Identification of planetary companions of giant stars is made difficult because of the astrophysical noise, that may produce radial velocity (RV) variations similar to those induced by a companion. On the other hand any stellar signal is wavelength dependent, while signals due to a companion are achromatic. Aims. Our goal is to determine the origin of the Doppler periodic variations observed in the thick disk K giant star TYC 4282-605-1 by HARPS-N at the Telescopio Nazionale Galileo (TNG) and verify if they can be due to the presence of a substellar companion. Methods. Several methods have been used to exclude the stellar origin of the observed signal including detailed analysis of activity indicators and bisector and the analysis of the photometric light curve. Finally we have conducted an observational campaign to monitor the near infrared (NIR) RV with GIANO at the TNG in order to verify whether the NIR amplitude variations are comparable with those observed in the visible. Results. Both optical and NIR RVs show consistent variations with a period at 101 days and similar amplitude, pointing to the presence of a companion orbiting the target. The main orbital properties obtained for our giant star with a derived mass of M=0.97+-0.03M_sun are M_Psini=10.78+-0.12MJ;P=101.54+-0.05days;e=0.28+-0.01 and a=0.422+-0.009AU. The chemical analysis shows a significant enrichment in the abundance of Nai, Mgi, Ali and S i while the rest of analyzed elements are consistent with the solar value demonstrating that the chemical composition corresponds with an old K giant (age = 10.1 Gyr) belonging to local thick disk. Conclusions. We conclude that the substellar companion hypothesis for this K giant is the best explanation for the observed periodic RV variation. This study also shows the high potential of multi-wavelength RV observations for the validation of planet candidates., Comment: Accepted in Journal reference A&A 14/06/2017
- Published
- 2017
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27. The GAPS Programme with HARPS-N at TNG: XIII. the orbital obliquity of three close-in massive planets hosted by dwarf K-type stars: WASP-43, HAT-P-20 and Qatar-2
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Gloria Andreuzzi, R. Zanmar Sanchez, Aldo S. Bonomo, Avet Harutyunyan, F. Borsa, A. F. Martinez Fiorenzano, Giampaolo Piotto, Riccardo Smareglia, Marco Molinaro, Luca Borsato, Thomas Henning, Emilio Molinari, Riccardo Claudi, E. Covino, R. Cosentino, Marco Pedani, A. F. Lanza, John Southworth, L. Di Fabrizio, Isabella Pagano, P. Giacobbe, Andrea Bignamini, A. Suárez Mascareño, Gaetano Scandariato, C. Boccato, Silvano Desidera, K. Biazzo, Giuseppe Leto, Paolo Molaro, Giuseppina Micela, V. Granata, Monica Rainer, Luca Malavolta, S. Masiero, Oliver Turner, M. Esposito, Antonio Maggio, Raffaele Gratton, Serena Benatti, Alessandro Sozzetti, David R. Anderson, Luigi Mancini, Jesus Maldonado, Laura Affer, Simona Ciceri, Mario Damasso, Valerio Nascimbeni, E. Poretti, and ITA
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stars: individual: Qatar-2 ,Planetary systems ,Stars: Individual: HAT-P-20 ,Stars: Individual: Qatar-2 ,Stars: Individual: WASP-43 ,Techniques: Photometric ,Techniques: Radial velocities ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,techniques: photometric ,Settore FIS/05 - Astronomia e Astrofisica ,Planet ,0103 physical sciences ,techniques: radial velocities ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,010306 general physics ,010303 astronomy & astrophysics ,planetary systems ,Astrophysics::Galaxy Astrophysics ,QB ,Orbital elements ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,stars: individual: WASP-43 ,Astronomy and Astrophysics ,Effective temperature ,Light curve ,Exoplanet ,Radial velocity ,Stars ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,stars: individual: HAT-P-20 ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Context. The orbital obliquity of planets with respect to the rotational axis of their host stars is a relevant parameter for the characterization of the global architecture of planetary systems and a key observational constraint to discriminate between different scenarios proposed to explain the existence of close-in giant planets. Aims: In the framework of the GAPS project, we conduct an observational programme aimed at determinating the orbital obliquity of known transiting exoplanets. The targets are selected to probe the obliquity against a wide range of stellar and planetary physical parameters. Methods: We exploit high-precision radial velocity (RV) measurements, delivered by the HARPS-N spectrograph at the 3.6 m Telescopio Nazionale Galileo, to measure the Rossiter-McLaughlin (RM) effect in RV time-series bracketing planet transits, and to refine the orbital parameters determinations with out-of-transit RV data. We also analyse new transit light curves obtained with several 1-2 m class telescopes to better constrain the physical fundamental parameters of the planets and parent stars. Results: We report here on new transit spectroscopic observations for three very massive close-in giant planets: WASP-43 b, HAT-P-20 b and Qatar-2 b (Mp = 2.00, 7.22, 2.62 MJ; a = 0.015, 0.036, 0.022 AU, respectively) orbiting dwarf K-type stars with effective temperature well below 5000 K (Teff = 4500 ± 100, 4595 ± 45, 4640 ± 65 K respectively). These are the coolest stars (except for WASP-80) for which the RM effect has been observed so far. We find λ = 3.5 ± 6.8 deg for WASP-43 b and λ = -8.0 ± 6.9 deg for HAT-P-20 b, while for Qatar-2, our faintest target, the RM effect is only marginally detected, though our best-fit value λ = 15 ± 20 deg is in agreement with a previous determination. In combination with stellar rotational periods derived photometrically, we estimate the true spin-orbit angle, finding that WASP-43 b is aligned while the orbit of HAT-P-20 b presents a small but significant obliquity ( deg). By analyzing the CaII H&K chromospheric emission lines for HAT-P-20 and WASP-43, we find evidence for an enhanced level of stellar activity that is possibly induced by star-planet interactions. Based on observations collected at the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica (INAF) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the frame of the programme Global Architecture of Planetary Systems (GAPS).Also based on observations collected at the 0.82 m IAC80 Telescope, operated on the island of Tenerife by the Instituto de Astrofísica de Canarias in the Spanish Observatorio del Teide.
- Published
- 2017
28. SN 2009ip à la PESSTO: no evidence for core collapse yet★
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Assaf Sternberg, S. Benetti, Stephen Smartt, Mark Sullivan, Daniel Bayliss, Franz E. Bauer, K. Takats, S. Marchi, J. P. Moore, K. W. Smith, Paolo A. Mazzali, Morgan Fraser, J. B. Haislip, Daniel E. Reichart, Marco Molinaro, Riccardo Smareglia, Stefano Valenti, Francisco Forster Buron, F. Bufano, Andrea Pastorello, Laurent Le Guillou, Seppo Mattila, Maria Teresa Botticella, O. Yaron, Fang Yuan, George Zhou, David Young, Massimo Turatto, T. W. Chen, Anders Jerkstrand, Giuliano Pignata, Cosimo Inserra, Joseph P. Anderson, M. J. Childress, Brad E. Tucker, Cristina Knapic, Rubina Kotak, and Avishay Gal-Yam
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Physics ,astro-ph.SR ,ta115 ,010308 nuclear & particles physics ,Star (game theory) ,Astronomy ,Balmer series ,Astronomy and Astrophysics ,Astrophysics ,16. Peace & justice ,Kinetic energy ,01 natural sciences ,Spectral line ,Luminosity ,symbols.namesake ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,symbols ,Emission spectrum ,Absorption (logic) ,Ejecta ,010303 astronomy & astrophysics - Abstract
We present observations of the interacting transient SN 2009ip, from the start of the outburst in October 2012 until the end of the 2012 observing season. The transient reached a peak of $M_V$=-17.7 mag before fading rapidly, with a total integrated luminosity of 1.9$\times10^{49}$ erg over the period of August-December 2012. The optical and near infrared spectra are dominated by narrow emission lines, signaling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities between 0.5-1.2$\times10^4$ km s$^{-1}$\. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudo-nebular spectra. We set a limit of $, Comment: 28 pages, submitted to MNRAS. Abstract abridged for arXiv
- Published
- 2013
29. Monitoring and controlling the SKA telescope manager: a peculiar LMC system in the framework of the SKA LMCs
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Matteo Canzari, Riccardo Smareglia, Matteo Di Carlo, Mauro Dolci, Simone Riggi, and ITA
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Aperture array ,business.industry ,Computer science ,02 engineering and technology ,021001 nanoscience & nanotechnology ,01 natural sciences ,law.invention ,010309 optics ,Telescope ,law ,Control system ,0103 physical sciences ,0210 nano-technology ,business ,Simulation ,Computer hardware - Abstract
The SKA Telescope Manager (TM) is the core package of the SKA Telescope: it is aimed at scheduling observations, controlling their execution, monitoring the telescope health status, diagnosing and fixing its faults and so on. To do that, TM directly interfaces with the Local Monitoring and Control systems (LMCs) of the various SKA Elements (e.g. Dishes, Low-Frequency Aperture Array, etc.), exchanging commands and data with each of them. TM in turn needs to be monitored and controlled, in order its continuous and proper operation - and therefore that of the whole SKA Telescope - is ensured. It appears indeed that, while the unavailability of one or more instances of any other SKA element should result only in a degraded operation for the whole telescope, a problem in TM could cause a complete stop of any operation. In addition to this higher responsibility, a local monitoring and control system for TM has to collect and display logging data directly to operators, perform lifecycle management of TM applications and directly deal - when possible - with management of TM faults (which also includes a direct handling of TM status and performance data). In this paper, the peculiarities presented by the TM monitoring and control and the consequences they have on the design of a related LMC system are addressed and discussed.
- Published
- 2016
30. Aided generation of search interfaces to astronomical archives
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Cristina Knapic, Francesco Cepparo, Andrea Bignamini, Sonia Zorba, Marco Molinaro, and Riccardo Smareglia
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Java ,Computer science ,business.industry ,Data management ,Virtual observatory ,World Wide Web ,Data access ,Software deployment ,Schema (psychology) ,Web application ,business ,computer ,Graphical user interface ,computer.programming_language - Abstract
Astrophysical data provider organizations that host web based interfaces to provide access to data resources have to cope with possible changes in data management that imply partial rewrites of web applications. To avoid doing this manually it was decided to develop a dynamically configurable Java EE web application that can set itself up reading needed information from configuration files. Specification of what information the astronomical archive database has to expose is managed using the TAP SCHEMA schema from the IVOA TAP recommendation, that can be edited using a graphical interface. When configuration steps are done the tool will build a war file to allow easy deployment of the application.
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- 2016
31. Radio data archiving system
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Cristina Knapic, Matteo Stagni, E. Dovgan, A. Zanichelli, Andrea Orlati, M. Sponza, Simona Righini, Mauro Nanni, F. Bedosti, and Riccardo Smareglia
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Metadata ,Radio telescope ,World Wide Web ,Data sharing ,Open Archival Information System ,Computer science ,computer.internet_protocol ,Virtual observatory ,computer ,XML ,Data modeling - Abstract
Radio Astronomical Data models are becoming very complex since the huge possible range of instrumental configurations available with the modern Radio Telescopes. What in the past was the last frontiers of data formats in terms of efficiency and flexibility is now evolving with new strategies and methodologies enabling the persistence of a very complex, hierarchical and multi-purpose information. Such an evolution of data models and data formats require new data archiving techniques in order to guarantee data preservation following the directives of Open Archival Information System and the International Virtual Observatory Alliance for data sharing and publication. Currently, various formats (FITS, MBFITS, VLBI's XML description files and ancillary files) of data acquired with the Medicina and Noto Radio Telescopes can be stored and handled by a common Radio Archive, that is planned to be released to the (inter)national community by the end of 2016. This state-of-the-art archiving system for radio astronomical data aims at delegating as much as possible to the software setting how and where the descriptors (metadata) are saved, while the users perform user-friendly queries translated by the web interface into complex interrogations on the database to retrieve data. In such a way, the Archive is ready to be Virtual Observatory compliant and as much as possible user-friendly.
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- 2016
32. Ska telescope manager (tm): status and architecture overview
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Mark Nicol, Swaminathan Natarajan, Alan Bridger, Mangesh Patil, Roger Thompson, Lize van den Heever, Domingos Barbosa, Stewart Williams, Gerhard Le Roux, Paul Swart, Mauro Dolci, Yashwant Gupta, Subhrojyoti Roy Choudhury, Matteo Di Carlo, Riccardo Smareglia, Sonja Vrcic, J. C. Guzman, João Paulo Barraca, ITA, GBR, IND, and ZAF
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Engineering ,Scope (project management) ,business.industry ,02 engineering and technology ,021001 nanoscience & nanotechnology ,01 natural sciences ,Monitoring and control ,law.invention ,010309 optics ,Telescope ,Design phase ,Radio telescope ,Work (electrical) ,law ,0103 physical sciences ,Systems engineering ,Architecture ,0210 nano-technology ,business ,Telecommunications - Abstract
The SKA radio telescope project is building two telescopes, SKA-Low in Australia and SKA-Mid in South Africa respectively. The Telescope Manager is responsible for the observations lifecycle and for monitoring and control of each instrument, and is being developed by an international consortium. The project is currently in the design phase, with the Preliminary Design Review having been successfully completed, along with re-baselining to match project scope to available budget. This report presents the status of the Telescope Manager work, key architectural challenges and our approach to addressing them.
- Published
- 2016
33. The GAPS Programme with HARPS-N@TNG XII: Characterization of the planetary system around HD108874
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P. Giacobbe, Silvano Desidera, E. Covino, Giuseppina Micela, A. Bignamini, Roberto Silvotti, K. Biazzo, Mario Damasso, A. S. Bonomo, A. Maggio, Cristina Knapic, Francesco Marzari, S. Masiero, Gloria Andreuzzi, M. Rainer, M. Pedani, S. Messina, G. Scandariato, I. Pagano, A. F. Martinez Fiorenzano, L. Di Fabrizio, Riccardo Smareglia, A. F. Lanza, V. Nascimbeni, Alessandro Sozzetti, Rosario Cosentino, C. Boccato, E. Poretti, Elisa Molinari, Ararat Harutyunyan, Riccardo Claudi, M. Esposito, S. Benatti, R. G. Gratton, Francesco Borsa, L. Malavolta, Laura Affer, G. Piotto, J. Maldonado, and ITA
- Subjects
Rotation period ,Physics ,Stars: activity ,Earth and Planetary Astrophysics (astro-ph.EP) ,Outer planets ,010308 nuclear & particles physics ,Giant planet ,Exomoon ,Planetary systems ,Stars: individual: HD 108874 ,Techniques: radial velocities ,Astronomy and Astrophysics ,Space and Planetary Science ,Astronomy ,FOS: Physical sciences ,Planetary system ,01 natural sciences ,Radial velocity ,Planet ,0103 physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Circumstellar habitable zone ,Astrophysics - Earth and Planetary Astrophysics - Abstract
In order to understand the observed physical and orbital diversity of extrasolar planetary systems, a full investigation of these objects and of their host stars is necessary. Within this field, one of the main purposes of the GAPS observing project with HARPS-N@TNG is to provide a more detailed characterisation of already known systems. In this framework we monitored the star, hosting two giant planets, HD108874, with HARPS-N for three years in order to refine the orbits, to improve the dynamical study and to search for additional low-mass planets in close orbits. We subtracted the radial velocity (RV) signal due to the known outer planets, finding a clear modulation of 40.2 d period. We analysed the correlation between RV residuals and the activity indicators and modelled the magnetic activity with a dedicated code. Our analysis suggests that the 40.2 d periodicity is a signature of the rotation period of the star. A refined orbital solution is provided, revealing that the system is close to a mean motion resonance of about 9:2, in a stable configuration over 1 Gyr. Stable orbits for low-mass planets are limited to regions very close to the star or far from it. Our data exclude super-Earths with Msin i \gtrsim 5 M_Earth within 0.4 AU and objects with Msin i \gtrsim 2 M_Earth with orbital periods of a few days. Finally we put constraints on the habitable zone of the system, assuming the presence of an exomoon orbiting the inner giant planet., Comment: 10 pages; 11 figures; A&A Accepted
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- 2016
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34. VIALACTEA knowledge base homogenizing access to Milky Way data
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Marilena Bandieramonte, Alessandro Costa, Marco Molinaro, Ugo Becciani, Massimo Brescia, Stefano Cavuoti, S. J. Liu, Davide Elia, Anna Maria Di Giorgio, Fabio Vitello, Ákos Hajnal, Sergio Molinari, Eugenio Schisano, Giuseppe Riccio, Hermann Gabor, Riccardo Smareglia, Péter Kacsuk, Robert Butora, Eva Sciacca, ITA, HUN, Gianluca Chiozzi, Juan C. Guzman, Molinaro, M., Butora, R., Bandieramonte, M., Becciani, U., Brescia, M., Cavuoti, S., Costa, A., Di Giorgio, A. M., Elia, D., Hajnal, A., Gabor, H., Kacsuk, P., Liu, S. J., Molinari, S., Riccio, G., Schisano, E., Sciacca, E., Smareglia, R., and Vitello, F.
- Subjects
business.industry ,Computer science ,Relational database ,Data discovery ,FOS: Physical sciences ,020206 networking & telecommunications ,02 engineering and technology ,Virtual observatory ,computer.software_genre ,01 natural sciences ,Task (project management) ,Metadata ,World Wide Web ,Knowledge base ,0103 physical sciences ,0202 electrical engineering, electronic engineering, information engineering ,Data access, Databases, Milky way, VO ,Web service ,Astrophysics - Instrumentation and Methods for Astrophysics ,business ,010303 astronomy & astrophysics ,computer ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Data integration - Abstract
The VIALACTEA project has a work package dedicated to Tools and Infrastructure and, inside it, a task for the Database and Virtual Observatory Infrastructure. This task aims at providing an infrastructure to store all the resources needed by the, more purposely, scientific work packages of the project itself. This infrastructure includes a combination of: storage facilities, relational databases and web services on top of them, and has taken, as a whole, the name of VIALACTEA Knowledge Base (VLKB). This contribution illustrates the current status of this VLKB. It details the set of data resources put together; describes the database that allows data discovery through VO inspired metadata maintenance; illustrates the discovery, cutout and access services built on top of the former two for the users to exploit the data content., Comment: 11 pages, 1 figure, SPIE Astronomical Telescopes + Instrumentation 2016, Software and Cyberifrastructure for Astronomy IV, Conference Proceedings
- Published
- 2016
35. The AstroBID: preserving and sharing the Italian astronomical heritage
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Valeria Zanini, Riccardo Smareglia, Emilia Olostro Cirella, Mauro Gargano, Antonella Gasperini, and ITA
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World Wide Web ,Cultural heritage ,History of astronomy ,Computer science ,Library science - Abstract
The cultural heritage of the National Institute for Astrophysics (INAF), made of rare and modern Books, Instruments and archival Documents, the AstroBID, marks the milestones in the history of astronomy in Italy. INAF, in collaboration with the Department of Physics and Astronomy of the University of Bologna, has developed a project to preserve, digitize, and valorize its patrimony by creating a web portal Polvere di Stelle. It shows the cultural heritage of 12 libraries and historical archives, and 13 instrument collections, and allows both academics and a wider audience to search simultaneously the AstroBID materials.
- Published
- 2016
36. A distributed infrastructure for publishing VO services: an implementation
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Francesco Cepparo, Ivan Scagnetto, Riccardo Smareglia, Marco Molinaro, and ITA
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Multiple instances ,Interface (Java) ,Computer science ,Distributed computing ,02 engineering and technology ,VO services ,High availability ,01 natural sciences ,010309 optics ,High performance ,Multiprocess ,Scalable architecture ,0103 physical sciences ,Electronic ,Optical and Magnetic Materials ,Multithreaded ,Electrical and Electronic Engineering ,Message driven ,business.industry ,Astrophysical publishing environment ,Distributed system ,Modular architecture ,Electronic, Optical and Magnetic Materials ,Condensed Matter Physics ,Computer Science Applications1707 Computer Vision and Pattern Recognition ,Applied Mathematics ,Message passing ,Modular design ,021001 nanoscience & nanotechnology ,Data access ,Publishing ,Scalability ,Message broker ,0210 nano-technology ,business ,Computer network - Abstract
This contribution describes both the design and the implementation details of a new solution for publishing VO services, enlightening its maintainable, distributed, modular and scalable architecture. Indeed, the new publisher is multithreaded and multiprocess. Multiple instances of the modules can run on different machines to ensure high performance and high availability, and this will be true both for the interface modules of the services and the back end data access ones. The system uses message passing to let its components communicate through an AMQP message broker that can itself be distributed to provide better scalability and availability.
- Published
- 2016
37. The GAPS Programme with HARPS-N at TNG
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Jesus Maldonado, Luca Malavolta, A. F. Lanza, Emilio Molinari, Riccardo Claudi, E. Covino, Gaetano Scandariato, C. Boccato, Walter Boschin, Pedro Figueira, Giuseppe Leto, Cristina Knapic, S. Masiero, Giuseppina Micela, M. Esposito, Marco Pedani, A. F. Martinez Fiorenzano, Aldo S. Bonomo, Serena Benatti, Alessandro Sozzetti, P. Giacobbe, Isabella Pagano, Silvano Desidera, Luigi Mancini, Raffaele Gratton, Antonio Maggio, K. Biazzo, Laura Affer, Riccardo Smareglia, Monica Rainer, Valerio Nascimbeni, E. Poretti, Giampaolo Piotto, F. Borsa, Sergio Messina, Mario Damasso, R. Cosentino, Andrea Bignamini, and ITA
- Subjects
Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010504 meteorology & atmospheric sciences ,Starspot ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Planetary system ,01 natural sciences ,Standard deviation ,Radial velocity ,Stars ,Settore FIS/05 - Astronomia e Astrofisica ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Planet ,0103 physical sciences ,Spectral resolution ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics ,0105 earth and related environmental sciences ,Line (formation) - Abstract
Stellar activity is the ultimate source of radial-velocity (RV) noise in the search for Earth-mass planets orbiting late-type main-sequence stars. We analyse the performance of four different indicators and the chromospheric index $\log R'_{\rm HK}$ in detecting RV variations induced by stellar activity in 15 slowly rotating ($v\sin i \leq 5$ km/s), weakly active ($\log R'_{\rm HK} \leq -4.95$) solar-like stars observed with the high-resolution spectrograph HARPS-N. We consider indicators of the asymmetry of the cross-correlation function (CCF) between the stellar spectrum and the binary weighted line mask used to compute the RV, that is the bisector inverse span (BIS), $\Delta V$, and a new indicator $V_{\rm asy(mod)}$ together with the full width at half maximum (FWHM) of the CCF. We present methods to evaluate the uncertainties of the CCF indicators and apply a kernel regression (KR) between the RV, the time, and each of the indicators to study their capability of reproducing the RV variations induced by stellar activity. The considered indicators together with the KR prove to be useful to detect activity-induced RV variations in $47 \pm 18$ percent of the stars over a two-year time span when a significance (two-sided p-value) threshold of one percent is adopted. In those cases, KR reduces the standard deviation of the RV time series by a factor of approximately two. The BIS, the FWHM, and the newly introduced $V_{\rm asy(mod)}$ are the best indicators, being useful in $27 \pm 13$, $13 \pm 9$, and $13 \pm 9$ percent of the cases, respectively. The relatively limited performances of the activity indicators are related to the very low activity level and $v\sin i$ of the considered stars. For the application of our approach to sun-like stars, a spectral resolution of at least $10^5$ and highly stabilized spectrographs are recommended., Comment: 15 pages, 6 figures, 5 tables, one Appendix, accepted to Astronomy and Astrophysics
- Published
- 2018
38. Wide and deep near-UV (360 nm) galaxy counts and the extragalactic background light with the Large Binocular Camera
- Author
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Emiliano Diolaiti, A. Di Paola, F. Gasparo, R. M. Wagner, Nicola Menci, Richard F. Green, Fabio Fontanot, Fernando Pedichini, Andrea Baruffolo, D. Thompson, Andrea Grazian, Riccardo Smareglia, Vincenzo Testa, G. Gentile, O. Kuhn, Stefano Gallozzi, Emanuele Giallongo, John M. Hill, Roberto Ragazzoni, Jacopo Farinato, Fabio Pasian, Roberto Speziali, Giacomo Beccari, Adriano Fontana, and Mario Radovich
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Star formation ,media_common.quotation_subject ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Large Binocular Telescope ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Cosmic variance ,Galaxy ,Photometry (optics) ,Extragalactic background light ,Space and Planetary Science ,Sky ,Galaxy formation and evolution ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,media_common - Abstract
Deep multicolour surveys are the main tool to explore the formation and evolution of the faint galaxies which are beyond the spectroscopic limit with the present technology. The photometric properties of these faint galaxies are usually compared with current renditions of semianalytical models to provide constraints on the fundamental physical processes involved in galaxy formation and evolution, namely the mass assembly and the star formation. Galaxy counts over large sky areas in the near-UV band are important because they are difficult to obtain given the low efficiency of near-UV instrumentation, even at 8m class telescopes. A large instrumental field of view helps in minimizing the biases due to the cosmic variance. We have obtained deep images in the 360nm U band provided by the blue channel of the Large Binocular Camera at the prime focus of the Large Binocular Telescope. We have derived over an area of ~0.4 sq. deg. the galaxy number counts down to U=27 in the Vega system (corresponding to U=27.86 in the AB system) at a completeness level of 30% reaching the faintest current limit for this wavelength and sky area. The shape of the galaxy counts in the U band can be described by a double power-law, the bright side being consistent with the shape of shallower surveys of comparable or greater areas. The slope bends over significantly at U>23.5 ensuring the convergence of the contribution by star forming galaxies to the EBL in the near-UV band to a value which is more than 70% of the most recent upper limits derived for this band. We have jointly compared our near-UV and K band counts collected from the literature with few selected hierarchical CDM models emphasizing critical issues in the physical description of the galaxy formation and evolution., Accepted for publication in A&A. Uses aa.cls, 9 pages, 4 figures. Citations updated
- Published
- 2009
39. The Blue Straggler Population in the Globular Cluster M53 (NGC 5024): A CombinedHST, LBT, and CFHT Study1
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C. De Santis, A. Di Paola, R. T. Rood, E. Diolaiti, Roberto Speziali, J. Farinato, F. Gasparo, F. Fusi Pecci, Nicolas Bouché, A. Grazian, Peter Buschkamp, Barbara Lanzoni, Fernando Pedichini, G. Gentile, Riccardo Smareglia, Vincenzo Testa, Fabio Pasian, M. Bellazzini, F. R. Ferraro, E. Giallongo, L. Pulone, Stefano Gallozzi, Andrea Baruffolo, Adriano Fontana, E. Vernet, Giacomo Beccari, and Roberto Ragazzoni
- Subjects
Physics ,education.field_of_study ,Population ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Star count ,Radius ,Blue straggler ,Stars ,Space and Planetary Science ,Globular cluster ,Cluster (physics) ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Tidal tail ,education ,Astrophysics::Galaxy Astrophysics - Abstract
We used a proper combination of multiband high-resolution and wide field multi-wavelength observations collected at three different telescopes (HST, LBT and CFHT) to probe Blue Straggler Star (BSS) populations in the globular cluster M53. Almost 200 BSS have been identified over the entire cluster extension. The radial distribution of these stars has been found to be bimodal (similarly to that of several other clusters) with a prominent dip at ~60'' (~2 r_c) from the cluster center. This value turns out to be a factor of two smaller than the radius of avoidance (r_avoid, the radius within which all the stars of ~1.2 M_sun have sunk to the core because of dynamical friction effects in an Hubble time). While in most of the clusters with a bimodal BSS radial distribution, r_avoid has been found to be located in the region of the observed minimum, this is the second case (after NGC6388) where this discrepancy is noted. This evidence suggests that in a few clusters the dynamical friction seems to be somehow less efficient than expected. We have also used this data base to construct the radial star density profile of the cluster: this is the most extended and accurate radial profile ever published for this cluster, including detailed star counts in the very inner region. The star density profile is reproduced by a standard King Model with an extended core (~25'') and a modest value of the concentration parameter (c=1.58). A deviation from the model is noted in the most external region of the cluster (at r>6.5' from the center). This feature needs to be further investigated in order to address the possible presence of a tidal tail in this cluster.
- Published
- 2008
40. The performance of the blue prime focus large binocular camera at the large binocular telescope
- Author
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O. Kuhn, Richard F. Green, Gianfranco Gentile, Jacopo Farinato, Roberto Speziali, Andrea Baruffolo, Andrea Grazian, Fernando Pedichini, Emiliano Diolaiti, C. De Santis, S. Gallozzi, R. M. Wagner, David Thompson, Emanuele Giallongo, Riccardo Smareglia, E. Vernet, Vincenzo Testa, Piero Salinari, Giacomo Beccari, A. Di Paola, Fabio Pasian, Adriano Fontana, John M. Hill, Roberto Ragazzoni, F. Gasparo, and Mario Radovich
- Subjects
Physics ,business.industry ,media_common.quotation_subject ,Astrophysics (astro-ph) ,Vega ,FOS: Physical sciences ,Astronomy and Astrophysics ,Large Binocular Telescope ,Astrophysics ,Chip ,Galaxy ,Redshift ,law.invention ,Telescope ,Optics ,Space and Planetary Science ,law ,Sky ,business ,Data reduction ,media_common - Abstract
We present the characteristics and some early scientific results of the first instrument at the Large Binocular Telescope (LBT), the Large Binocular Camera (LBC). Each LBT telescope unit will be equipped with similar prime focus cameras. The blue channel is optimized for imaging in the UV-B bands and the red channel for imaging in the VRIz bands. The corrected field-of-view of each camera is approximately 30 arcminutes in diameter, and the chip area is equivalent to a 23x23 arcmin2 field. In this paper we also present the commissioning results of the blue channel. The scientific and technical performance of the blue channel was assessed by measurement of the astrometric distortion, flat fielding, ghosts, and photometric calibrations. These measurements were then used as input to a data reduction pipeline applied to science commissioning data. The measurements completed during commissioning show that the technical performance of the blue channel is in agreement with original expectations. Since the red camera is very similar to the blue one we expect similar performance from the commissioning that will be performed in the following months in binocular configuration. Using deep UV image, acquired during the commissioning of the blue camera, we derived faint UV galaxy-counts in a ~500 sq. arcmin. sky area to U(Vega)=26.5. These galaxy counts imply that the blue camera is the most powerful UV imager presently available and in the near future in terms of depth and extent of the field-of-view. We emphasize the potential of the blue camera to increase the robustness of the UGR multicolour selection of Lyman break galaxies at redshift z~3., Comment: Accepted for publication in A&A. Uses aa.cls, 10 pages, 10 figures. Zero points changed in Table 2
- Published
- 2008
41. The Elongated Structure of the Hercules Dwarf Spheroidal Galaxy from Deep Large Binocular Telescope Imaging
- Author
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David Thompson, Roberto Ragazzoni, Nicolas F. Martin, Jill Bechtold, Matthew G. Coleman, Richard F. Green, Richard W. Pogge, David J. Sand, Vincenzo Testa, Hans Hippelein, Peter M. Garnavich, A. DiPaola, Riccardo Smareglia, Emanuele Giallongo, Hans-Walter Rix, Jacopo Farinato, Eric F. Bell, Jelte T. A. de Jong, and John M. Hill
- Subjects
Physics ,Milky Way ,Astronomy ,Astronomy and Astrophysics ,Large Binocular Telescope ,Field of view ,Orbital eccentricity ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Dwarf spheroidal galaxy ,Photometry (optics) ,Stars ,Space and Planetary Science ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Sagittarius ,Astrophysics::Galaxy Astrophysics - Abstract
We present a deep, wide-field photometric survey of the newly discovered Hercules dwarf spheroidal galaxy (dSph), based on data from the Large Binocular Telescope. Images in B, V, and r were obtained with the Large Binocular Camera covering a 23' × 23' field of view to a magnitude of ~25.5 (5 σ). This permitted the construction of color-magnitude diagrams that reach approximately 1.5 mag below the Hercules main-sequence turnoff. Three-filter photometry allowed us to preferentially select probable Hercules member stars and to examine the structure of this system at a previously unattained level. We find that the Hercules dwarf is highly elongated (3 : 1), considerably more so than any other dSph satellite of the Milky Way, except the disrupting Sagittarius dwarf. Although we cannot rule out that the unusual structure is intrinsic to Hercules as an equilibrium system, our results suggest tidal disruption as a likely cause of this highly elliptical structure. Given the relatively large galactocentric distance of this system (132 ± 12 kpc), signs of tidal disruption would require the Hercules dwarf to be on a highly eccentric orbit around the Milky Way.
- Published
- 2007
42. Enabling Grid technologies for Planck space mission
- Author
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Fabio Pasian, Claudio Vuerli, Andrea Zacchei, Giuliano Castelli, Riccardo Smareglia, Davide Maino, and Giuliano Taffoni
- Subjects
Computer Networks and Communications ,Computer science ,business.industry ,media_common.quotation_subject ,Astrophysics::Instrumentation and Methods for Astrophysics ,computer.software_genre ,Grid ,Simulation software ,Data sharing ,symbols.namesake ,Grid computing ,Hardware and Architecture ,Sky ,Computer data storage ,Systems engineering ,symbols ,Satellite ,Planck ,business ,computer ,Software ,Simulation ,media_common - Abstract
PLANCK, the ESA satellite aimed at mapping the microwave sky through two complete sky surveys, will fly in 2007. It is an extremely demanding space mission in terms of computing power and data storage. PLANCK simulations mimic the whole mission starting from a virtual sky (ideal or contaminated by introducing several noise sources). Their main goal is the validation of the acquisition and reduction procedure that will be used to build the final scientific data during the operative phase of the mission. The GRID technology seems to be a promising answer to data storage and processing needs of the satellite. In the framework of the EGEE grid infrastructure, we managed to run a number of experiments aimed at designing and defining an application specific environment for the simulation software and data sharing. Our successful experiments demonstrate that the "gridification" of Planck pipelines is not only possible but even extremely convenient in terms of data processing speed and data sharing.
- Published
- 2007
43. The GAPS Programme with HARPS-N at TNG VIII. Observations of the Rossiter-McLaughlin effect and characterisation of the transiting planetary systems HAT-P-36 and WASP-11/HAT-P-10
- Author
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Isabella Pagano, Antonio Maggio, Massimiliano Esposito, F. Borsa, Riccardo Claudi, Gaetano Scandariato, C. Boccato, J. Tregloan-Reed, Th. Henning, E. Poretti, L. Affer, John Southworth, Giampaolo Piotto, R. Zanmar Sanchez, Alessandro Sozzetti, Andrea Bignamini, Aldo S. Bonomo, Monica Rainer, V. Lorenzi, I. Bruni, Emilio Molinari, Luigi R. Bedin, Silvano Desidera, G. Raia, Giuseppina Micela, Francesco Marzari, Gracjan Maciejewski, Giuseppe Lodato, Simona Ciceri, Luigi Mancini, Mario Damasso, S. Murabito, Katia Biazzo, Riccardo Smareglia, A. F. Lanza, Elvira Covino, A. F. Martinez Fiorenzano, Raffaele Gratton, Rosario Cosentino, ITA, USA, GBR, DEU, ESP, and POL
- Subjects
Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Stellar rotation ,Starspot ,Rossiter–McLaughlin effect ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Planetary system ,Effective temperature ,Light curve ,Stars ,Settore FIS/05 - Astronomia e Astrofisica ,Space and Planetary Science ,Planet ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,QB - Abstract
We determine the true and the projected obliquity of HAT-P-36 and WASP-11/HAT-P-10 systems, respectively, which are both composed of a relatively cool star and a hot-Jupiter planet. Thanks to the high-resolution spectrograph HARPS-N, we observed the Rossiter-McLaughlin effect for both the systems by acquiring precise radial-velocity measurements during planetary transit events. We also present photometric observations comprising six light curves covering five transit events, obtained using three medium-class telescopes and the telescope-defocussing technique. One transit of WASP-11/HAT-P-10 was followed simultaneously from two observatories. The three transit light curves of HAT-P-36b show anomalies that are attributable to starspot complexes on the surface of the parent star, in agreement with the analysis of its spectra that indicate a moderate activity. By analysing the complete HATNet data set of HAT-P-36, we estimated the stellar rotation period by detecting a periodic photometric modulation in the light curve caused by star spots, obtaining Prot=15.3 days, which implies that the inclination of the stellar rotational axis with respect to the line of sight is 65 degree. We used the new spectroscopic and photometric data to revise the main physical parameters and measure the sky-projected misalignment angle of the two systems. We found \lambda=-14 degree for HAT-P-36 and \lambda=7 degree for WASP-11/HAT-P-10, indicating in both cases a good spin-orbit alignment. In the case of HAT-P-36, we also measured its real obliquity, which turned out to be 25 degrees., Comment: 18 pages, 14 figures
- Published
- 2015
44. The GAPS programme with HARPS-N at TNG: IX. The multi-planet system KELT-6: Detection of the planet KELT-6c and measurement of the Rossiter-McLaughlin effect for KELT-6 b
- Author
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Paolo Giacobbe, Luigi R. Bedin, Jesus Maldonado, Silvano Desidera, Giampaolo Piotto, Emilio Molinari, Riccardo Claudi, David W. Latham, F. Borsa, Serena Benatti, Alessandro Sozzetti, L. Di Fabrizio, Davide Gandolfi, Antonio Maggio, S. Murabito, Laura Affer, M. Gomez-Jimenez, Isabella Pagano, Giuseppina Micela, Riccardo Smareglia, Marco Molinaro, Luca Malavolta, Rosario Cosentino, Allyson Bieryla, Karen A. Collins, R. Zanmar Sanchez, Aldo S. Bonomo, Monica Rainer, M. Esposito, Cristobal Petrovich, Katia Biazzo, John Southworth, A. F. Lanza, Gaetano Scandariato, C. Boccato, R. G. Gratton, Elvira Covino, Mario Damasso, M. Barbieri, Luigi Mancini, Valerio Nascimbeni, E. Poretti, ITA, USA, GBR, DEU, ESP, and CHL
- Subjects
photometry ,Rossiter–McLaughlin effect ,FOS: Physical sciences ,Orbital eccentricity ,Astrophysics ,Ephemeris ,Stars, KELT-6, planetary systems, radial velocities, photometry ,law.invention ,Photometry (optics) ,Telescope ,Settore FIS/05 - Astronomia e Astrofisica ,law ,Planet ,KELT-6 ,planetary systems ,Solar and Stellar Astrophysics (astro-ph.SR) ,QC ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Astronomy and Astrophysics ,Planetary system ,Stars ,Radial velocity ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,radial velocities ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Aims. For more than 1.5 years we monitored spectroscopically the star KELT-6 (BD+312447), known to host the transiting hot Saturn KELT-6b, because a previously observed long-term trend in radial velocity time series suggested the existence of an outer companion. Methods. We collected a total of 93 new spectra with the HARPS-N and TRES spectrographs. A spectroscopic transit of KELT-6b was observed with HARPS-N, and simultaneous photometry was obtained with the IAC-80 telescope. Results. We proved the existence of an outer planet with a mininum mass M$_{\rm p}$sini=3.71$\pm$0.21 M$_{\rm Jup}$ and a moderately eccentric orbit ($e=0.21_{-0.036}^{+0.039}$) of period P$\sim$3.5 years. We improved the orbital solution of KELT-6b and obtained the first measurement of the Rossiter-McLaughlin effect, showing that the planet has a likely circular, prograde, and slightly misaligned orbit, with a projected spin-orbit angle $\lambda$=$-$36$\pm$11 degrees. We improved the KELT-6b transit ephemeris from photometry, and we provided new measurements of the stellar parameters. KELT-6 appears as an interesting case to study the formation and evolution of multi-planet systems., Comment: Letter, 4 figures, accepted for publication in A&A. Some language editing and numbering of the paper series changed (from X to IX)
- Published
- 2015
45. The GAPS programme with HARPS-N at TNG: VII. Putting exoplanets in the stellar context: Magnetic activity and asteroseismology of τ Bootis A ∗ ∗ ∗
- Author
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Aldo S. Bonomo, Evgenya L. Shkolnik, M. Barbieri, Isabella Pagano, M. P. Di Mauro, John Southworth, M. Esposito, Monica Rainer, Ignazio Pillitteri, Beate Stelzer, Aldo F. M. Fiorenzano, Giuseppina Micela, Laura Affer, Roberto Silvotti, Mario Damasso, Avet Harutyunyan, Andrea Bignamini, Francesco Borsa, Jesus Maldonado, Davide Gandolfi, Paolo Molaro, Riccardo Claudi, Silvano Desidera, Giampaolo Piotto, Ennio Poretti, Elvira Covino, Katia Biazzo, Emilio Molinari, Antonio Maggio, Serena Benatti, Alessandro Sozzetti, Rosario Cosentino, Riccardo Smareglia, A. F. Lanza, Gaetano Scandariato, C. Boccato, and R. G. Gratton
- Subjects
Physics ,Asteroseismology ,Planetary systems ,Stars: activity ,Stars: individual:τBoo ,Techniques: spectroscopic ,Astronomy and Astrophysics ,Space and Planetary Science ,Stellar mass ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Planetary system ,Ephemeris ,Exoplanet ,Radial velocity ,Astrophysics - Solar and Stellar Astrophysics ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Spectrograph ,Astrophysics::Galaxy Astrophysics ,QB - Abstract
Aims. We observed the $\tau$ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the CaII H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of $0.9\pm0.5$ Gyr for $\tau$ Boo and further constrains the value of the stellar mass to $1.38\pm0.05$ M$_\odot$., Comment: 14 pages, accepted for publication in Astronomy and Astrophysics
- Published
- 2015
46. SN 2012ec: mass of the progenitor from PESSTO follow-up of the photospheric phase
- Author
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P. Ochner, O. Yaron, M. T. Botticella, A. Riffeser, S. Benetti, Daniel E. Reichart, Aaron P. LaCluyze, L. Tomasella, Avishay Gal-Yam, Justyn R. Maund, Mario Hamuy, C. Ries, Maria Letizia Pumo, Stefano Valenti, Marco Molinaro, Nancy Elias-Rosa, Morgan Fraser, M. Della Valle, David Young, Jesper Sollerman, Massimo Dall'Ora, A. Pastorello, Cristina Knapic, Michael Schmidt, Anders Jerkstrand, Massimo Turatto, Cosimo Inserra, Giuliano Pignata, Brian P. Schmidt, Stephen J. Smartt, C. Barbarino, Luca Zampieri, Mark Sullivan, Riccardo Smareglia, and K. W. Smith
- Subjects
Supernovae: general ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Luminosity ,Wolf–Rayet star ,supernovae: individual: SN 2012ec ,0103 physical sciences ,Ejecta ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Physics ,Spiral galaxy ,010308 nuclear & particles physics ,supernovae: individual: SN 2012A ,supernovae: individual: NGC 1084 ,Astronomy ,Astronomy and Astrophysics ,Radius ,supernovae: individual: SN 2012aw ,Light curve ,Supernova ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Circumstellar dust ,supernovae: individual: SN 2012ec, supernovae: individual: SN 2012aw, supernovae: individual: SN 2012A, supernovae: individual: NGC 1084 - Abstract
We present the results of a photometric and spectroscopic monitoring campaign of SN 2012ec, which exploded in the spiral galaxy NGC 1084, during the photospheric phase. The photometric light curve exhibits a plateau with luminosity L= 0.9 x 10^{42} erg/s and duration ~90 days, which is somewhat shorter than standard Type II-P supernovae. We estimate the nickel mass as 0.040 +/- 0.015 Msun from the luminosity at the beginning of the radioactive tail of the light curve. The explosion parameters of SN 2012ec were estimated from the comparison of the bolometric light curve and the observed temperature and velocity evolution of the ejecta with predictions from hydrodynamical models. We derived an envelope mass of 12.6 Msun, an initial progenitor radius of 1.6 x 10^{13} cm and an explosion energy of 1.2 foe. These estimates agree with an independent study of the progenitor star identified in pre-explosion images, for which an initial mass of M=14-22 Msun was determined. We have applied the same analysis to two other type II-P supernovae (SNe 2012aw and 2012A), and carried out a comparison with the properties of SN 2012ec derived in this paper. We find a reasonable agreement between the masses of the progenitors obtained from pre-explosion images and masses derived from hydrodynamical models. We estimate the distance to SN 2012ec with the Standardized Candle Method (SCM) and compare it with other estimates based on other primary and secondary indicators. SNe 2012A, 2012aw and 2012ec all follow the standard relations for the SCM for the use of Type II-P SNe as distance indicators., Comment: Accepted for publication in MRAS on Jan. 14, 2015
- Published
- 2015
47. The GAPS Programme with HARPS-N at TNG
- Author
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Gaetano Scandariato, Giampaolo Piotto, Giuseppe Lodato, P. Giacobbe, C. Boccato, Isabella Pagano, S. Crespi, Luigi Mancini, Rosario Cosentino, S. Masiero, Mario Damasso, Aldo S. Bonomo, A. F. Martinez Fiorenzano, Laura Affer, F. Borsa, Guillaume Hébrard, Marco Pedani, Andrea Bignamini, Valerio Nascimbeni, E. Poretti, Jesus Maldonado, Antonio Maggio, Giuseppina Micela, Emilio Molinari, Riccardo Claudi, E. Covino, A. F. Lanza, Francesco Marzari, Serena Benatti, Alessandro Sozzetti, Luca Malavolta, Monica Rainer, Silvano Desidera, M. Esposito, K. Biazzo, Raffaele Gratton, and Riccardo Smareglia
- Subjects
Planet-star interactions ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Settore FIS/05 - Astronomia e Astrofisica ,Planet ,0103 physical sciences ,Hot Jupiter ,010303 astronomy & astrophysics ,Stars: fundamental parameters ,Solar and Stellar Astrophysics (astro-ph.SR) ,Planetary migration ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Orbital elements ,010308 nuclear & particles physics ,Giant planet ,Astronomy and Astrophysics ,Planetary system ,Exoplanet ,Planetary systems ,Techniques: radial velocities ,Space and Planetary Science ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Roche limit ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We carried out a Bayesian homogeneous determination of the orbital parameters of 231 transiting giant planets (TGPs) that are alone or have distant companions; we employed DE-MCMC methods to analyse radial-velocity (RV) data from the literature and 782 new high-accuracy RVs obtained with the HARPS-N spectrograph for 45 systems over 3 years. Our work yields the largest sample of systems with a transiting giant exoplanet and coherently determined orbital, planetary, and stellar parameters. We found that the orbital parameters of TGPs in non-compact planetary systems are clearly shaped by tides raised by their host stars. Indeed, the most eccentric planets have relatively large orbital separations and/or high mass ratios, as expected from the equilibrium tide theory. This feature would be the outcome of high-eccentricity migration (HEM). The distribution of $��=a/a_R$, where $a$ and $a_R$ are the semi-major axis and the Roche limit, for well-determined circular orbits peaks at 2.5; this also agrees with expectations from the HEM. The few planets of our sample with circular orbits and $��>5$ values may have migrated through disc-planet interactions instead of HEM. By comparing circularisation times with stellar ages, we found that hot Jupiters with $a < 0.05$ au have modified tidal quality factors $10^{5} < Q'_p < 10^{9}$, and that stellar $Q'_s > 10^{6}-10^{7}$ are required to explain the presence of eccentric planets at the same orbital distance. As a by-product of our analysis, we detected a non-zero eccentricity for HAT-P-29; we determined that five planets that were previously regarded to have hints of non-zero eccentricity have circular orbits or undetermined eccentricities; we unveiled curvatures caused by distant companions in the RV time series of HAT-P-2, HAT-P-22, and HAT-P-29; and we revised the planetary parameters of CoRoT-1b., 44 pages (16 pages of main text and figures), 11 figures, 5 longtables, published in Astronomy and Astrophysics, Volume 602, A107 (2017). Tables with new HARPS-N and TRES radial-velocity data (Tables 1 and 2), stellar parameters (Table 7), orbital parameters and RV jitter (Table 8), and planet physical parameters (Table 9) are available as ancillary files (sidebar on the right)
- Published
- 2017
48. Modular VO oriented Java EE service deployer
- Author
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Cristina Knapic, Marco De Marco, Francesco Cepparo, Pietro Apollo, Riccardo Smareglia, and Marco Molinaro
- Subjects
Service layer ,Database ,Java ,business.industry ,Interface (Java) ,Computer science ,strictfp ,Virtual observatory ,computer.software_genre ,Java Naming and Directory Interface ,Java concurrency ,Enterprise Java Bean ,Real time Java ,Java API for XML-based RPC ,Observatory ,Systems architecture ,Software engineering ,business ,computer ,computer.programming_language - Abstract
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 development of the new system using Java Enterprise technologies can better benefit from existing libraries to build up the single tokens implementing the IVOA standards. Each component can be built from single standards and each deployed service (i.e. service components instantiations) can consume the other components' exposed methods and services without the need of homogenizing them in dedicated libraries. Scalability can be achieved in an easier way by deploying components or sets of services on a distributed environment and using JNDI (Java Naming and Directory Interface) and RMI (Remote Method Invocation) technologies. Single service configuration will not be significantly different from the VO-Dance solution given that Java class instantiation that benefited from Java Reflection will only be moved to Java EJB pooling (and not, e.g. embedded in bundles for subsequent deployment).
- Published
- 2014
49. The GAPS Programme with HARPS-N at TNG. III: The retrograde orbit of HAT-P-18b
- Author
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Rosario Cosentino, Antonio Maggio, Isabella Pagano, Silvano Desidera, Aldo S. Bonomo, Valerio Nascimbeni, Riccardo Smareglia, F. Borsa, E. Poretti, John Southworth, Luigi Mancini, Emilio Molinari, Giampaolo Piotto, A. F. Lanza, C. Boccato, Massimiliano Esposito, Alessandro Sozzetti, Riccardo Claudi, Avet Harutyunyan, Elvira Covino, Davide Gandolfi, Giuseppina Micela, Raffaele Gratton, Mauro Barbieri, and Katia Biazzo
- Subjects
stars: individual: HAT-P-18 ,FOS: Physical sciences ,planetary systems ,techniques: spectroscopic ,techniques: radial velocities ,stars: fundamental parameters ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Settore FIS/05 - Astronomia e Astrofisica ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Retrograde motion ,Astronomy and Astrophysics ,Planetary system ,Surface gravity ,Orbital period ,Exoplanet ,Radial velocity ,Stars ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The measurement of the Rossiter-McLaughlin effect for transiting exoplanets places constraints on the orientation of the orbital axis with respect to the stellar spin axis, which can shed light on the mechanisms shaping the orbital configuration of planetary systems. Here we present the interesting case of the Saturn-mass planet HAT-P-18b, which orbits one of the coolest stars for which the Rossiter-McLaughlin effect has been measured so far. We acquired a spectroscopic time-series, spanning a full transit, with the HARPS-N spectrograph mounted at the TNG telescope. The very precise radial velocity measurements delivered by the HARPS-N pipeline were used to measure the Rossiter-McLaughlin effect. Complementary new photometric observations of another full transit were also analysed to obtain an independent determination of the star and planet parameters. We find that HAT-P-18b lies on a counter-rotating orbit, the sky-projected angle between the stellar spin axis and the planet orbital axis being lambda=132 +/- 15 deg. By joint modelling of the radial velocity and photometric data we obtain new determinations of the star (M_star = 0.770 +/- 0.027 M_Sun; R_star= 0.717 +/- 0.026 R_Sun; Vsin(I_star) = 1.58 +/- 0.18 km/s) and planet (M_pl = 0.196 +/- 0.008 M_J; R_pl = 0.947 +/- 0.044 R_J) parameters. Our spectra provide for the host star an effective temperature T_eff = 4870 +/- 50 K, a surface gravity of log(g_star) = 4.57 +/- 0.07 cm/s, and an iron abundance of [Fe/H] = 0.10 +/- 0.06. HAT-P-18b is one of the few planets known to transit a star with T_eff < 6250 K on a retrograde orbit. Objects such as HAT-P-18b (low planet mass and/or relatively long orbital period) most likely have a weak tidal coupling with their parent stars, therefore their orbits preserve any original misalignment. As such, they are ideal targets to study the causes of orbital evolution in cool main-sequence stars., 5 pages, 2 figures
- Published
- 2014
50. WINGS Data Release: a database of galaxies in nearby clusters
- Author
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Alan Dressler, Mauro D'Onofrio, Riccardo Smareglia, Mariano Moles, Alessia Moretti, Daniela Bettoni, A. Omizzolo, Marco Molinaro, Warrick J. Couch, Benedetta Vulcani, G. Fasano, Marco Gullieuszik, T. Valentinuzzi, Bianca M. Poggianti, J. Varela, Jacopo Fritz, Per Kjaergaard, and Antonio Cava
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,SAMPLE ,FOS: Physical sciences ,virtual observatory tools ,MORPHOLOGICAL CLASSIFICATIONS ,Astrophysics ,Virtual observatory ,computer.software_genre ,Photometry (optics) ,surveys ,Galaxy formation and evolution ,Cluster (physics) ,fundamental parameters [galaxies] ,clusters: general [galaxies] ,PHOTOMETRY ,Surface brightness ,Physics ,Database ,Star formation ,DIGITAL-SKY-SURVEY ,FORMATION HISTORIES ,RICH CLUSTERS ,Astronomy and Astrophysics ,CATALOG ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,EVOLUTION ,Physics and Astronomy ,Space and Planetary Science ,LUMINOSITY FUNCTION ,Astrophysics of Galaxies (astro-ph.GA) ,photometry [galaxies] ,STELLAR MASS ,computer ,catalogs ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
[Abridged] To effectively investigate galaxy formation and evolution, it is of paramount importance to exploit homogeneous data for large samples of galaxies in different environments. The WINGS (WIde-field Nearby Galaxy-cluster Survey) project aim is to evaluate physical properties of galaxies in a complete sample of low redshift clusters to be used as reference sample for evolutionary studies. The WINGS survey is still ongoing and the original dataset will soon be enlarged with new observations. This paper presents the entire collection of WINGS measurements obtained so far. We decided to make use of the Virtual Observatory (VO) tools to share the WINGS database (that will be regularly updated) with the community. In the database each object has one unique identification (WINGSID). Each subset of estimated properties is accessible using a simple cone search (including wide-field images). We provide the scientific community the entire set of wide-field images. Furthermore, the published database contains photometry of 759,024 objects and surface brightness analysis for 42,275 and 41,463 galaxies in the V and B band, respectively. The completeness depends on the image quality, and on the cluster redshift, reaching on average 90% at V, 11 pages, 3 Figures. Accepted for publication in A & A
- Published
- 2014
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