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CRIS Current Research Information System
Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims. A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Methods. The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. Results. Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330-680 nm) and GRP (630-1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions. Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.
Brown, A., Vallenari, A., Prusti, T., De Bruijne, J., Babusiaux, C., Bailer-Jones, C., et al. (2018). Summary of the contents and survey properties. ASTRONOMY & ASTROPHYSICS, 616, 1-22 [10.1051/0004-6361/201833051].
Summary of the contents and survey properties
Brown, A. G. A.;Vallenari, A.;Prusti, T.;De Bruijne, J. H. J.;Babusiaux, C.;Bailer-Jones, C. A. L.;Biermann, M.;Evans, D. W.;Eyer, L.;Jansen, F.;Jordi, C.;Klioner, S. A.;Lammers, U.;Lindegren, L.;Luri, X.;Mignard, F.;Panem, C.;Pourbaix, D.;Randich, S.;Sartoretti, P.;Siddiqui, H. I.;Soubiran, C.;Van Leeuwen, F.;Walton, N. A.;Arenou, F.;Bastian, U.;Cropper, M.;Drimmel, R.;Katz, D.;Lattanzi, M. G.;Bakker, J.;Cacciari, C.;Castañeda, J.;Chaoul, L.;Cheek, N.;De Angeli, F.;Fabricius, C.;Guerra, R.;Holl, B.;Masana, E.;Messineo, R.;Mowlavi, N.;Nienartowicz, K.;Panuzzo, P.;Portell, J.;Riello, M.;Seabroke, G. M.;Tanga, P.;Thévenin, F.;Gracia-Abril, G.;Comoretto, G.;Garcia-Reinaldos, M.;Teyssier, D.;Altmann, M.;Andrae, R.;Audard, M.;Bellas-Velidis, I.;Benson, K.;Berthier, J.;Blomme, R.;Burgess, P.;Busso, G.;Carry, B.;Cellino, A.;Clementini, G.;Clotet, M.;Creevey, O.;Davidson, M.;De Ridder, J.;Delchambre, L.;Dell'Oro, A.;Ducourant, C.;Fernández-Hernández, J.;Fouesneau, M.;Frémat, Y.;Galluccio, L.;García-Torres, M.;González-Núñez, J.;González-Vidal, J. J.;Gosset, E.;Guy, L. P.;Halbwachs, J. -L.;Hambly, N. C.;Harrison, D. L.;Hernández, J.;Hestroffer, D.;Hodgkin, S. T.;Hutton, A.;Jasniewicz, G.;Jean-Antoine-Piccolo, A.;Jordan, S.;Korn, A. J.;Krone-Martins, A.;Lanzafame, A. C.;Lebzelter, T.;Löffler, W.;Manteiga, M.;Marrese, P. M.;Martín-Fleitas, J. M.;Moitinho, A.;Mora, A.;Muinonen, K.;Osinde, J.;Pancino, E.;Pauwels, T.;Petit, J. -M.;Recio-Blanco, A.;Richards, P. J.;Rimoldini, L.;Robin, A. C.;Sarro, L. M.;Siopis, C.;Smith, M.;Sozzetti, A.;Süveges, M.;Torra, J.;Van Reeven, W.;Abbas, U.;Abreu Aramburu, A.;Accart, S.;Aerts, C.;Altavilla, G.;Álvarez, M. A.;Alvarez, R.;Alves, J.;Anderson, R. I.;Andrei, A. H.;Anglada Varela, E.;Antiche, E.;Antoja, T.;Arcay, B.;Astraatmadja, T. L.;Bach, N.;Baker, S. G.;Balaguer-Núñez, L.;Balm, P.;Barache, C.;Barata, C.;Barbato, D.;Barblan, F.;Barklem, P. S.;Barrado, D.;Barros, M.;Barstow, M. A.;Bartholomé Muñoz, S.;Bassilana, J. -L.;Becciani, U.;Bellazzini, M.;Berihuete, A.;Bertone, S.;Bianchi, L.;Bienaymé, O.;Blanco-Cuaresma, S.;Boch, T.;Boeche, C.;Bombrun, A.;Borrachero, R.;Bossini, D.;Bouquillon, S.;Bourda, G.;Bragaglia, A.;Bramante, L.;Breddels, M. A.;Bressan, A.;Brouillet, N.;Brüsemeister, T.;Brugaletta, E.;Bucciarelli, B.;Burlacu, A.;Busonero, D.;Butkevich, A. G.;Buzzi, R.;Caffau, E.;Cancelliere, R.;Cannizzaro, G.;Cantat-Gaudin, T.;Carballo, R.;Carlucci, T.;Carrasco, J. M.;Casamiquela, L.;Castellani, M.;Castro-Ginard, A.;Charlot, P.;Chemin, L.;Chiavassa, A.;Cocozza, G.;Costigan, G.;Cowell, S.;Crifo, F.;Crosta, M.;Crowley, C.;Cuypersy, J.;Dafonte, C.;Damerdji, Y.;Dapergolas, A.;David, P.;David, M.;De Laverny, P.;De Luise, F.;De March, R.;De Martino, D.;De Souza, R.;De Torres, A.;Debosscher, J.;Del Pozo, E.;Delbo, M.;Delgado, A.;Delgado, H. E.;Di Matteo, P.;Diakite, S.;Diener, C.;Distefano, E.;Dolding, C.;Drazinos, P.;Durán, J.;Edvardsson, B.;Enke, H.;Eriksson, K.;Esquej, P.;Eynard Bontemps, G.;Fabre, C.;Fabrizio, M.;Faigler, S.;Falcão, A. J.;Farràs Casas, M.;Federici, L.;Fedorets, G.;Fernique, P.;Figueras, F.;Filippi, F.;Findeisen, K.;Fonti, A.;Fraile, E.;Fraser, M.;Frézouls, B.;Gai, M.;Galleti, S.;Garabato, D.;García-Sedano, F.;Garofalo, A.;Garralda, N.;Gavel, A.;Gavras, P.;Gerssen, J.;Geyer, R.;Giacobbe, P.;Gilmore, G.;Girona, S.;Giuffrida, G.;Glass, F.;Gomes, M.;Granvik, M.;Gueguen, A.;Guerrier, A.;Guiraud, J.;Gutiérrez-Sánchez, R.;Haigron, R.;Hatzidimitriou, D.;Hauser, M.;Haywood, M.;Heiter, U.;Helmi, A.;Heu, J.;Hilger, T.;Hobbs, D.;Hofmann, W.;Holland, G.;Huckle, H. E.;Hypki, A.;Icardi, V.;Janßen, K.;De Fombelle, G. Jevardat;Jonker, P. G.;Juhász, Ã. L.;Julbe, F.;Karampelas, A.;Kewley, A.;Klar, J.;Kochoska, A.;Kohley, R.;Kolenberg, K.;Kontizas, M.;Kontizas, E.;Koposov, S. E.;Kordopatis, G.;Kostrzewa-Rutkowska, Z.;Koubsky, P.;Lambert, S.;Lanza, A. F.;Lasne, Y.;Lavigne, J. -B.;Le Fustec, Y.;Le Poncin-Lafitte, C.;Lebreton, Y.;Leccia, S.;Leclerc, N.;Lecoeur-Taibi, I.;Lenhardt, H.;Leroux, F.;Liao, S.;Licata, E.;Lindstrøm, H. E. P.;Lister, T. A.;Livanou, E.;Lobel, A.;López, M.;Managau, S.;Mann, R. G.;Mantelet, G.;Marchal, O.;Marchant, J. M.;Marconi, M.;Marinoni, S.;Marschalkó, G.;Marshall, D. J.;Martino, M.;Marton, G.;Mary, N.;Massari, D.;Matijević, G.;Mazeh, T.;McMillan, P. J.;Messina, S.;Michalik, D.;Millar, N. R.;Molina, D.;Molinaro, R.;Molnár, L.;Montegriffo, P.;Mor, R.;Morbidelli, R.;Morel, T.;Morris, D.;Mulone, A. F.;Muraveva, T.;Musella, I.;Nelemans, G.;Nicastro, L.;Noval, L.;O'Mullane, W.;Ordénovic, C.;Ordóñez-Blanco, D.;Osborne, P.;Pagani, C.;Pagano, I.;Pailler, F.;Palacin, H.;Palaversa, L.;Panahi, A.;Pawlak, M.;Piersimoni, A. M.;Pineau, F. -X.;Plachy, E.;Plum, G.;Poggio, E.;Poujoulet, E.;Prša, A.;Pulone, L.;Racero, E.;Ragaini, S.;Rambaux, N.;Ramos-Lerate, M.;Regibo, S.;Reylé, C.;Riclet, F.;Ripepi, V.;Riva, A.;Rivard, A.;Rixon, G.;Roegiers, T.;Roelens, M.;Romero-Gómez, M.;Rowell, N.;Royer, F.;Ruiz-Dern, L.;Sadowski, G.;Sagristà Sellés, T.;Sahlmann, J.;Salgado, J.;Salguero, E.;Sanna, N.;Santana-Ros, T.;Sarasso, M.;Savietto, H.;Schultheis, M.;Sciacca, E.;Segol, M.;Segovia, J. C.;Ségransan, D.;Shih, I. -C.;Siltala, L.;Silva, A. F.;Smart, R. L.;Smith, K. W.;Solano, E.;Solitro, F.;Sordo, R.;Soria Nieto, S.;Souchay, J.;Spagna, A.;Spoto, F.;Stampa, U.;Steele, I. A.;Steidelmüller, H.;Stephenson, C. A.;Stoev, H.;Suess, F. F.;Surdej, J.;Szabados, L.;Szegedi-Elek, E.;Tapiador, D.;Taris, F.;Tauran, G.;Taylor, M. B.;Teixeira, R.;Terrett, D.;Teyssandier, P.;Thuillot, W.;Titarenko, A.;Torra Clotet, F.;Turon, C.;Ulla, A.;Utrilla, E.;Uzzi, S.;Vaillant, M.;Valentini, G.;Valette, V.;Van Elteren, A.;Van Hemelryck, E.;Van Leeuwen, M.;Vaschetto, M.;Vecchiato, A.;Veljanoski, J.;Viala, Y.;Vicente, D.;Vogt, S.;Von Essen, C.;Voss, H.;Votruba, V.;Voutsinas, S.;Walmsley, G.;Weiler, M.;Wertz, O.;Wevers, T.;Wyrzykowski, Å.;Yoldas, A.;Žerjal, M.;Ziaeepour, H.;Zorec, J.;Zschocke, S.;Zucker, S.;Zurbach, C.;Zwitter, T.
2018
Abstract
Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims. A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Methods. The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. Results. Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330-680 nm) and GRP (630-1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions. Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy.
Brown, A., Vallenari, A., Prusti, T., De Bruijne, J., Babusiaux, C., Bailer-Jones, C., et al. (2018). Summary of the contents and survey properties. ASTRONOMY & ASTROPHYSICS, 616, 1-22 [10.1051/0004-6361/201833051].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/660016
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.
