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IRIS
Context. We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Aims. A summary of the contents of Gaia EDR3 is presented, accompanied by a discussion on the differences with respect to Gaia DR2 and an overview of the main limitations which are present in the survey. Recommendations are made on the responsible use of Gaia EDR3 results. Methods. The raw data collected with the Gaia instruments during the first 34 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium and turned into this early third data release, which represents a major advance with respect to Gaia DR2 in terms of astrometric and photometric precision, accuracy, and homogeneity. Results. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motions, and the (GBP - GRP) colour are also available. The passbands for G, GBP, and GRP are provided as part of the release. For ease of use, the 7 million radial velocities from Gaia DR2 are included in this release, after the removal of a small number of spurious values. New radial velocities will appear as part of Gaia DR3. Finally, Gaia EDR3 represents an updated materialisation of the celestial reference frame (CRF) in the optical, the Gaia-CRF3, which is based solely on extragalactic sources. The creation of the source list for Gaia EDR3 includes enhancements that make it more robust with respect to high proper motion stars, and the disturbing effects of spurious and partially resolved sources. The source list is largely the same as that for Gaia DR2, but it does feature new sources and there are some notable changes. The source list will not change for Gaia DR3. Conclusions. Gaia EDR3 represents a significant advance over Gaia DR2, with parallax precisions increased by 30 per cent, proper motion precisions increased by a factor of 2, and the systematic errors in the astrometry suppressed by 30-40% for the parallaxes and by a factor ~2.5 for the proper motions. The photometry also features increased precision, but above all much better homogeneity across colour, magnitude, and celestial position. A single passband for G, GBP, and GRP is valid over the entire magnitude and colour range, with no systematics above the 1% level
Gaia Early Data Release 3: Summary of the contents and survey properties
Brown A. G. A.;Vallenari A.;Prusti T.;De Bruijne J. H. J.;Babusiaux C.;Biermann M.;Creevey O. L.;Evans D. W.;Eyer L.;Hutton A.;Jansen F.;Jordi C.;Klioner S. A.;Lammers U.;Lindegren L.;Luri X.;Mignard F.;Panem C.;Pourbaix D.;Randich S.;Sartoretti P.;Soubiran C.;Walton N. A.;Arenou F.;Bailer-Jones C. A. L.;Bastian U.;Cropper M.;Drimmel R.;Katz D.;Lattanzi M. G.;Van Leeuwen F.;Bakker J.;Cacciari C.;Castaneda J.;De Angeli F.;Ducourant C.;Fabricius C.;Fouesneau M.;Fremat Y.;Guerra R.;Guerrier A.;Guiraud J.;Jean-Antoine Piccolo A.;Masana E.;Messineo R.;Mowlavi N.;Nicolas C.;Nienartowicz K.;Pailler F.;Panuzzo P.;Riclet F.;Roux W.;Seabroke G. M.;Sordo R.;Tanga P.;Thevenin F.;Gracia-Abril G.;Portell J.;Teyssier D.;Altmann M.;Andrae R.;Bellas-Velidis I.;Benson K.;Berthier J.;Blomme R.;Brugaletta E.;Burgess P. W.;Busso G.;Carry B.;Cellino A.;Cheek N.;Clementini G.;Damerdji Y.;Davidson M.;Delchambre L.;Dell'Oro A.;Fernandez-Hernandez J.;Galluccio L.;Garcia-Lario P.;Garcia-Reinaldos M.;Gonzalez-Nunez J.;Gosset E.;Haigron R.;Halbwachs J. -L.;Hambly N. C.;Harrison D. L.;Hatzidimitriou D.;Heiter U.;Hernandez J.;Hestroffer D.;Hodgkin S. T.;Holl B.;Janssen K.;Jevardat De Fombelle G.;Jordan S.;Krone-Martins A.;Lanzafame A. C.;Loffler W.;Lorca A.;Manteiga M.;Marchal O.;Marrese P. M.;Moitinho A.;Mora A.;Muinonen K.;Osborne P.;Pancino E.;Pauwels T.;Petit J. -M.;Recio-Blanco A.;Richards P. J.;Riello M.;Rimoldini L.;Robin A. C.;Roegiers T.;Rybizki J.;Sarro L. M.;Siopis C.;Smith M.;Sozzetti A.;Ulla A.;Utrilla E.;Van Leeuwen M.;Van Reeven W.;Abbas U.;Abreu Aramburu A.;Accart S.;Aerts C.;Aguado J. J.;Ajaj M.;Altavilla G.;Alvarez M. A.;Alvarez Cid-Fuentes J.;Alves J.;Anderson R. I.;Anglada Varela E.;Antoja T.;Audard M.;Baines D.;Baker S. G.;Balaguer-Nunez L.;Balbinot E.;Balog Z.;Barache C.;Barbato D.;Barros M.;Barstow M. A.;Bartolome S.;Bassilana J. -L.;Bauchet N.;Baudesson-Stella A.;Becciani U.;Bellazzini M.;Bernet M.;Bertone S.;Bianchi L.;Blanco-Cuaresma S.;Boch T.;Bombrun A.;Bossini D.;Bouquillon S.;Bragaglia A.;Bramante L.;Breedt E.;Bressan A.;Brouillet N.;Bucciarelli B.;Burlacu A.;Busonero D.;Butkevich A. G.;Buzzi R.;Caffau E.;Cancelliere R.;Canovas H.;Cantat-Gaudin T.;Carballo R.;Carlucci T.;Carnerero M. I.;Carrasco J. M.;Casamiquela L.;Castellani M.;Castro-Ginard A.;Castro Sampol P.;Chaoul L.;Charlot P.;Chemin L.;Chiavassa A.;Cioni M. -R. L.;Comoretto G.;Cooper W. J.;Cornez T.;Cowell S.;Crifo F.;Crosta M.;Crowley C.;Dafonte C.;Dapergolas A.;David M.;David P.;De Laverny P.;De Luise F.;De March R.;De Ridder J.;De Souza R.;De Teodoro P.;De Torres A.;Del Peloso E. F.;Del Pozo E.;Delbo M.;Delgado A.;Delgado H. E.;Delisle J. -B.;Di Matteo P.;Diakite S.;Diener C.;Distefano E.;Dolding C.;Eappachen D.;Edvardsson B.;Enke H.;Esquej P.;Fabre C.;Fabrizio M.;Faigler S.;Fedorets G.;Fernique P.;Fienga A.;Figueras F.;Fouron C.;Fragkoudi F.;Fraile E.;Franke F.;Gai M.;Garabato D.;Garcia-Gutierrez A.;Garcia-Torres M.;Garofalo A.;Gavras P.;Gerlach E.;Geyer R.;Giacobbe P.;Gilmore G.;Girona S.;Giuffrida G.;Gomel R.;Gomez A.;Gonzalez-Santamaria I.;Gonzalez-Vidal J. J.;Granvik M.;Gutierrez-Sanchez R.;Guy L. P.;Hauser M.;Haywood M.;Helmi A.;Hidalgo S. L.;Hilger T.;Hladczuk N.;Hobbs D.;Holland G.;Huckle H. E.;Jasniewicz G.;Jonker P. G.;Juaristi Campillo J.;Julbe F.;Karbevska L.;Kervella P.;Khanna S.;Kochoska A.;Kontizas M.;Kordopatis G.;Korn A. J.;Kostrzewa-Rutkowska Z.;Kruszynska K.;Lambert S.;Lanza A. F.;Lasne Y.;Le Campion J. -F.;Le Fustec Y.;Lebreton Y.;Lebzelter T.;Leccia S.;Leclerc N.;Lecoeur-Taibi I.;Liao S.;Licata E.;Lindstrom E. P.;Lister T. A.;Livanou E.;Lobel A.;Madrero Pardo P.;Managau S.;Mann R. G.;Marchant J. M.;Marconi M.;Marcos Santos M. M. S.;Marinoni S.;Marocco F.;Marshall D. J.;Martin Polo L.;Martin-Fleitas J. M.;Masip A.;Massari D.;Mastrobuono-Battisti A.;Mazeh T.;McMillan P. J.;Messina S.;Michalik D.;Millar N. R.;Mints A.;Molina D.;Molinaro R.;Molnar L.;Montegriffo P.;Mor R.;Morbidelli R.;Morel T.;Morris D.;Mulone A. F.;Munoz D.;Muraveva T.;Murphy C. P.;Musella I.;Noval L.;Ordenovic C.;Orru G.;Osinde J.;Pagani C.;Pagano I.;Palaversa L.;Palicio P. A.;Panahi A.;Pawlak M.;Penalosa Esteller X.;Penttila A.;Piersimoni A. M.;Pineau F. -X.;Plachy E.;Plum G.;Poggio E.;Poretti E.;Poujoulet E.;Prsa A.;Pulone L.;Racero E.;Ragaini S.;Rainer M.;Raiteri C. M.;Rambaux N.;Ramos P.;Ramos-Lerate M.;Re Fiorentin P.;Regibo S.;Reyle C.;Ripepi V.;Riva A.;Rixon G.;Robichon N.;Robin C.;Roelens M.;Rohrbasser L.;Romero-Gomez M.;Rowell N.;Royer F.;Rybicki K. A.;Sadowski G.;Sagrista Selles A.;Sahlmann J.;Salgado J.;Salguero E.;Samaras N.;Sanchez Gimenez V.;Sanna N.;Santovena R.;Sarasso M.;Schultheis M.;Sciacca E.;Segol M.;Segovia J. C.;Segransan D.;Semeux D.;Shahaf S.;Siddiqui H. I.;Siebert A.;Siltala L.;Slezak E.;Smart R. L.;Solano E.;Solitro F.;Souami D.;Souchay J.;Spagna A.;Spoto F.;Steele I. A.;Steidelmuller H.;Stephenson C. A.;Suveges M.;Szabados L.;Szegedi-Elek E.;Taris F.;Tauran G.;Taylor M. B.;Teixeira R.;Thuillot W.;Tonello N.;Torra F.;Torra J.;Turon C.;Unger N.;Vaillant M.;Van Dillen E.;Vanel O.;Vecchiato A.;Viala Y.;Vicente D.;Voutsinas S.;Weiler M.;Wevers T.;Wyrzykowski L.;Yoldas A.;Yvard P.;Zhao H.;Zorec J.;Zucker S.;Zurbach C.;Zwitter T.
2021-01-01
Abstract
Context. We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Aims. A summary of the contents of Gaia EDR3 is presented, accompanied by a discussion on the differences with respect to Gaia DR2 and an overview of the main limitations which are present in the survey. Recommendations are made on the responsible use of Gaia EDR3 results. Methods. The raw data collected with the Gaia instruments during the first 34 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium and turned into this early third data release, which represents a major advance with respect to Gaia DR2 in terms of astrometric and photometric precision, accuracy, and homogeneity. Results. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motions, and the (GBP - GRP) colour are also available. The passbands for G, GBP, and GRP are provided as part of the release. For ease of use, the 7 million radial velocities from Gaia DR2 are included in this release, after the removal of a small number of spurious values. New radial velocities will appear as part of Gaia DR3. Finally, Gaia EDR3 represents an updated materialisation of the celestial reference frame (CRF) in the optical, the Gaia-CRF3, which is based solely on extragalactic sources. The creation of the source list for Gaia EDR3 includes enhancements that make it more robust with respect to high proper motion stars, and the disturbing effects of spurious and partially resolved sources. The source list is largely the same as that for Gaia DR2, but it does feature new sources and there are some notable changes. The source list will not change for Gaia DR3. Conclusions. Gaia EDR3 represents a significant advance over Gaia DR2, with parallax precisions increased by 30 per cent, proper motion precisions increased by a factor of 2, and the systematic errors in the astrometry suppressed by 30-40% for the parallaxes and by a factor ~2.5 for the proper motions. The photometry also features increased precision, but above all much better homogeneity across colour, magnitude, and celestial position. A single passband for G, GBP, and GRP is valid over the entire magnitude and colour range, with no systematics above the 1% level
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11769/523721
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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.
