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The Gaia astrophysical parameters inference system (Apsis). Pre-launch description

dc.contributor.authorBAILER-JONES, C. A. L.
dc.contributor.authorANDRAE, R.
dc.contributor.authorARCAY, B.
dc.contributor.authorASTRAATMADJA, T.
dc.contributor.authorBELLAS-VELIDIS, I.
dc.contributor.authorBERIHUETE, A.
hal.structure.identifierJoseph Louis LAGRANGE [LAGRANGE]
dc.contributor.authorBIJAOUI, A.
dc.contributor.authorCARRIÓN, C.
dc.contributor.authorDAFONTE, C.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierObservatoire de Haute-Provence [OHP]
dc.contributor.authorDAMERDJI, Y.
dc.contributor.authorDAPERGOLAS, A.
dc.contributor.authorDE LAVERNY, P.
dc.contributor.authorDELCHAMBRE, L.
dc.contributor.authorDRAZINOS, P.
dc.contributor.authorDRIMMEL, R.
hal.structure.identifierRoyal Observatory of Belgium = Observatoire Royal de Belgique [ROB]
dc.contributor.authorFRÉMAT, Y.
dc.contributor.authorFUSTES, D.
dc.contributor.authorGARCÍA-TORRES, M.
hal.structure.identifierGalaxies, Etoiles, Physique, Instrumentation [GEPI]
dc.contributor.authorGUÉDÉ, C.
dc.contributor.authorHEITER, U.
dc.contributor.authorJANOTTO, A. -M.
dc.contributor.authorKARAMPELAS, A.
dc.contributor.authorKIM, D. -W.
dc.contributor.authorKNUDE, J.
dc.contributor.authorKOLKA, I.
dc.contributor.authorKONTIZAS, E.
dc.contributor.authorKONTIZAS, M.
hal.structure.identifierDepartment of Astronomy and Space Physics [Uppsala]
dc.contributor.authorKORN, A. J.
hal.structure.identifierINAF - Osservatorio Astrofisico di Catania [OACT]
dc.contributor.authorLANZAFAME, A. C.
hal.structure.identifierGalaxies, Etoiles, Physique, Instrumentation [GEPI]
dc.contributor.authorLEBRETON, Y.
dc.contributor.authorLINDSTRØM, H.
dc.contributor.authorLIU, C.
dc.contributor.authorLIVANOU, E.
dc.contributor.authorLOBEL, A.
dc.contributor.authorMANTEIGA, M.
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorMARTAYAN, C.
dc.contributor.authorORDENOVIC, Ch.
hal.structure.identifierJoseph Louis LAGRANGE [LAGRANGE]
dc.contributor.authorPICHON, B.
dc.contributor.authorRECIO-BLANCO, A.
dc.contributor.authorROCCA-VOLMERANGE, B.
dc.contributor.authorSARRO, L. M.
dc.contributor.authorSMITH, K.
dc.contributor.authorSORDO, R.
hal.structure.identifierM2A 2013
dc.contributor.authorSOUBIRAN, C.
hal.structure.identifierJoseph Louis LAGRANGE [LAGRANGE]
dc.contributor.authorSURDEJ, J.
dc.contributor.authorTHÉVENIN, F.
dc.contributor.authorTSALMANTZA, P.
dc.contributor.authorVALLENARI, A.
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorZOREC, J.
dc.date.created2013-09-09
dc.date.issued2013
dc.identifier.issn0004-6361
dc.description.abstractEnThe Gaia satellite will survey the entire celestial sphere down to 20th magnitude, obtaining astrometry, photometry, and low resolution spectrophotometry on one billion astronomical sources, plus radial velocities for over one hundred million stars. Its main objective is to take a census of the stellar content of our Galaxy, with the goal of revealing its formation and evolution. Gaia's unique feature is the measurement of parallaxes and proper motions with hitherto unparalleled accuracy for many objects. As a survey, the physical properties of most of these objects are unknown. Here we describe the data analysis system put together by the Gaia consortium to classify these objects and to infer their astrophysical properties using the satellite's data. This system covers single stars, (unresolved) binary stars, quasars, and galaxies, all covering a wide parameter space. Multiple methods are used for many types of stars, producing multiple results for the end user according to different models and assumptions. Prior to its application to real Gaia data the accuracy of these methods cannot be assessed definitively. But as an example of the current performance, we can attain internal accuracies (RMS residuals) on F,G,K,M dwarfs and giants at G=15 (V=15-17) for a wide range of metallicites and interstellar extinctions of around 100K in effective temperature (Teff), 0.1mag in extinction (A0), 0.2dex in metallicity ([Fe/H]), and 0.25dex in surface gravity (logg). The accuracy is a strong function of the parameters themselves, varying by a factor of more than two up or down over this parameter range. After its launch in November 2013, Gaia will nominally observe for five years, during which the system we describe will continue to evolve in light of experience with the real data.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enThe Gaia astrophysical parameters inference system (Apsis). Pre-launch description
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201322344
dc.subject.halPhysique [physics]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1309.2157
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A74
bordeaux.volume559
bordeaux.peerReviewedoui
hal.identifierhal-00860253
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00860253v1
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