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Context. The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was derived from measurements obtained by means of the Blue and Red photometers (BP/RP), which were binned in 16 discrete wavelength bands. For every spectrum, the DR3 also contains additional information about the data quality for each band. Aims. We describe the processing of the Gaia spectral data of SSOs, explaining both the criteria used to select the subset of asteroid spectra published in Gaia DR3, and the different steps of our internal validation procedures. In order to further assess the quality of Gaia SSO reflectance spectra, we carried out external validation against SSO reflectance spectra obtained from ground-based and space-borne telescopes and available in the literature; we present our validation approach. Methods. For each selected SSO, an epoch reflectance was computed by dividing the calibrated spectrum observed by the BP/RP at each transit on the focal plane by the mean spectrum of a solar analogue. The latter was obtained by averaging the Gaia spectral measurements of a selected sample of stars known to have very similar spectra to that of the Sun. Finally, a mean of the epoch reflectance spectra was calculated in 16 spectral bands for each SSO. Results.Gaia SSO reflectance spectra are in general agreement with those obtained from a ground-based spectroscopic campaign specifically designed to cover the same spectral interval as Gaia and mimic the illumination and observing geometry characterising Gaia SSO observations. In addition, the agreement between Gaia mean reflectance spectra and those available in the literature is good for bright SSOs, regardless of their taxonomic spectral class. We identify an increase in the spectral slope of S-type SSOs with increasing phase angle. Moreover, we show that the spectral slope increases and the depth of the 1 μm absorption band decreases for increasing ages of S-type asteroid families. The latter can be interpreted as proof of progressive ageing of S-type asteroid surfaces due to their exposure to space weathering effects.
Gaia Data Release 3: Reflectance spectra of Solar System small bodies
Galluccio L.;Delbo M.;De Angeli F.;Pauwels T.;Tanga P.;Mignard F.;Cellino A.;Brown A. G. A.;Muinonen K.;Penttila A.;Jordan S.;Vallenari A.;Prusti T.;de Bruijne J. H. J.;Arenou F.;Babusiaux C.;Biermann M.;Creevey O. L.;Ducourant C.;Evans D. W.;Eyer L.;Guerra R.;Hutton A.;Jordi C.;Klioner S. A.;Lammers U. L.;Lindegren L.;Luri X.;Panem C.;Pourbaix D.;Randich S.;Sartoretti P.;Soubiran C.;Walton N. A.;Bailer-Jones C. A. L.;Bastian U.;Drimmel R.;Jansen F.;Katz D.;Lattanzi M. G.;van Leeuwen F.;Bakker J.;Cacciari C.;Castaneda J.;Fabricius C.;Fouesneau M.;Fremat Y.;Guerrier A.;Heiter U.;Masana E.;Messineo R.;Mowlavi N.;Nicolas C.;Nienartowicz K.;Pailler F.;Panuzzo P.;Riclet F.;Roux W.;Seabroke G. M.;Sordo R.;Thevenin F.;Gracia-Abril G.;Portell J.;Teyssier D.;Altmann M.;Andrae R.;Audard M.;Bellas-Velidis I.;Benson K.;Berthier J.;Blomme R.;Burgess P. W.;Busonero D.;Busso G.;Canovas H.;Carry B.;Cheek N.;Clementini G.;Damerdji Y.;Davidson M.;de Teodoro P.;Nunez Campos M.;Delchambre L.;Dell'Oro A.;Esquej P.;Fernandez-Hernandez J.;Fraile E.;Garabato D.;Garcia-Lario P.;Gosset E.;Haigron R.;Halbwachs J. -L.;Hambly N. C.;Harrison D. L.;Hernandez J.;Hestroffer D.;Hodgkin S. T.;Holl B.;Jansen K.;de Fombelle G. J.;Krone-Martins A.;Lanzafame A. C.;Loer W.;Marchal O.;Marrese P. M.;Moitinho A.;Osborne P.;Pancino E.;Recio-Blanco A.;Reyle C.;Riello M.;Rimoldini L.;Roegiers T.;Rybizki J.;Sarro L. M.;Siopis C.;Smith M.;Sozzetti A.;Utrilla E.;van Leeuwen M.;Abbas U.;Abraham P.;Aramburu A. A.;Aerts C.;Aguado J. J.;Ajaj M.;Aldea-Montero F.;Altavilla G.;Alvarez M. A.;Alves J.;Anderson R. I.;Varela E. A.;Antoja T.;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.;Becciani U.;Bellazzini M.;Berihuete A.;Bernet M.;Bertone S.;Bianchi L.;Binnenfeld A.;Blanco-Cuaresma S.;Boch T.;Bombrun A.;Bossini D.;Bouquillon S.;Bragaglia A.;Bramante L.;Breedt E.;Bressan A.;Brouillet N.;Brugaletta E.;Bucciarelli B.;Burlacu A.;Butkevich A. G.;Buzzi R.;Caffau E.;Cancelliere R.;Cantat-Gaudin T.;Carballo R.;Carlucci T.;Carnerero M. I.;Carrasco J. M.;Casamiquela L.;Castellani M.;Castro-Ginard A.;Chaoul L.;Charlot P.;Chemin L.;Chiaramida V.;Chiavassa A.;Chornay N.;Comoretto G.;Contursi G.;Cooper W. J.;Cornez T.;Cowell S.;Crifo F.;Cropper M.;Crosta M.;Crowley C.;Dafonte C.;Dapergolas A.;David P.;de Laverny P.;De Luise F.;De March R.;De Ridder J.;de Souza R.;de Torres A.;del Peloso E. F.;del Pozo E.;Delgado A.;Delisle J. -B.;Demouchy C.;Dharmawardena T. E.;Diakite S.;Diener C.;Distefano E.;Dolding C.;Enke H.;Fabre C.;Fabrizio M.;Faigler S.;Fedorets G.;Fernique P.;Figueras F.;Fournier Y.;Fouron C.;Fragkoudi F.;Gai M.;Garcia-Gutierrez A.;Garcia-Reinaldos M.;Garcia-Torres M.;Garofalo A.;Gavel A.;Gavras P.;Gerlach E.;Geyer R.;Giacobbe P.;Gilmore G.;Girona S.;Giuffrida G.;Gomel R.;Gomez A.;Gonzalez-Nunez J.;Gonzalez-Santamaria I.;Gonzalez-Vidal J. J.;Granvik M.;Guillout P.;Guiraud J.;Gutierrez-Sanchez R.;Guy L. P.;Hatzidimitriou D.;Hauser M.;Haywood M.;Helmer A.;Helmi A.;Sarmiento M. H.;Hidalgo S. L.;Hladczuk N.;Hobbs D.;Holland G.;Huckle H. E.;Jardine K.;Jasniewicz G.;Piccolo A. J. -A.;Jimenez-Arranz O.;Campillo J. J.;Julbe F.;Karbevska L.;Kervella P.;Khanna S.;Kordopatis G.;Korn A. J.;Kospal A.;Kostrzewa-Rutkowska Z.;Kruszynska K.;Kun M.;Laizeau P.;Lambert S.;Lanza A. F.;Lasne Y.;Le Campion J. -F.;Lebreton Y.;Lebzelter T.;Leccia S.;Leclerc N.;Lecoeur-Taibi I.;Liao S.;Licata E. L.;Lindstrom H. E. P.;Lister T. A.;Livanou E.;Lobel A.;Lorca A.;Loup C.;Pardo P. M.;Romeo A. M.;Managau S.;Mann R. G.;Manteiga M.;Marchant J. M.;Marconi M.;Marcos J.;Santos M. M. S. M.;Pina D. M.;Marinoni S.;Marocco F.;Marshall D. J.;Polo L. M.;Martin-Fleitas J. M.;Marton G.;Mary N.;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.;Monari G.;Monguio M.;Montegriffo P.;Montero A.;Mor R.;Mora A.;Morbidelli R.;Morel T.;Morris D.;Muraveva T.;Murphy C. P.;Musella I.;Nagy Z.;Noval L.;Ocana F.;Ogden A.;Ordenovic C.;Osinde J. O.;Pagani C.;Pagano I.;Palaversa L.;Palicio P. A.;Pallas-Quintela L.;Panahi A.;Payne-Wardenaar S.;Esteller X. P.;Petit J. -M.;Pichon B.;Piersimoni A. M.;Pineau F. -X.;Plachy E.;Plum G.;Poggio E.;Prsa A.;Pulone L.;Racero E.;Ragaini S.;Rainer M.;Raiteri C. M.;Ramos P.;Ramos-Lerate M.;Re Fiorentin P.;Regibo S.;Richards P. J.;Diaz C. R.;Ripepi V.;Riva A.;Rix H. -W.;Rixon G.;Robichon N.;Robin A. C.;Robin C.;Roelens M.;Rogues H. R. O.;Rohrbasser L.;Romero-Gomez M.;Rowell N.;Royer F.;Mieres D. R.;Rybicki K. A.;Sadowski G.;Nunez A. S.;Selles A. S.;Sahlmann J.;Salguero E.;Samaras N.;Gimenez V. S.;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.;Silvelo A.;Slezak E.;Slezak I.;Smart R. L.;Snaith O. N.;Solano E.;Solitro F.;Souami D.;Souchay J.;Spagna A.;Spina L.;Spoto F.;Steele I. A.;Steidelmuller H.;Stephenson C. A.;Suveges M.;Surdej J.;Szabados L.;Szegedi-Elek E.;Taris F.;Taylor M. B.;Teixeira R.;Tolomei L.;Tonello N.;Torra F.;Torra J.;Elipe G. T.;Trabucchi M.;Tsounis A. T.;Turon C.;Ulla A.;Unger N.;Vaillant M. V.;van Dillen E.;van Reeven W.;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.;Zwitter T.
2023
Abstract
Context. The Gaia mission of the European Space Agency (ESA) has been routinely observing Solar System objects (SSOs) since the beginning of its operations in August 2014. The Gaia data release three (DR3) includes, for the first time, the mean reflectance spectra of a selected sample of 60 518 SSOs, primarily asteroids, observed between August 5, 2014, and May 28, 2017. Each reflectance spectrum was derived from measurements obtained by means of the Blue and Red photometers (BP/RP), which were binned in 16 discrete wavelength bands. For every spectrum, the DR3 also contains additional information about the data quality for each band. Aims. We describe the processing of the Gaia spectral data of SSOs, explaining both the criteria used to select the subset of asteroid spectra published in Gaia DR3, and the different steps of our internal validation procedures. In order to further assess the quality of Gaia SSO reflectance spectra, we carried out external validation against SSO reflectance spectra obtained from ground-based and space-borne telescopes and available in the literature; we present our validation approach. Methods. For each selected SSO, an epoch reflectance was computed by dividing the calibrated spectrum observed by the BP/RP at each transit on the focal plane by the mean spectrum of a solar analogue. The latter was obtained by averaging the Gaia spectral measurements of a selected sample of stars known to have very similar spectra to that of the Sun. Finally, a mean of the epoch reflectance spectra was calculated in 16 spectral bands for each SSO. Results.Gaia SSO reflectance spectra are in general agreement with those obtained from a ground-based spectroscopic campaign specifically designed to cover the same spectral interval as Gaia and mimic the illumination and observing geometry characterising Gaia SSO observations. In addition, the agreement between Gaia mean reflectance spectra and those available in the literature is good for bright SSOs, regardless of their taxonomic spectral class. We identify an increase in the spectral slope of S-type SSOs with increasing phase angle. Moreover, we show that the spectral slope increases and the depth of the 1 μm absorption band decreases for increasing ages of S-type asteroid families. The latter can be interpreted as proof of progressive ageing of S-type asteroid surfaces due to their exposure to space weathering effects.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/3538022
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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.
