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A Complete Bank of Optical Images of the ICRF QSOs

dc.contributor.authorHUMBERTO ANDREI, Alexandre,
dc.contributor.authorTARIS, Francois,
hal.structure.identifierRécepteurs et Canaux Ioniques Membranaires [RCIM]
dc.contributor.authorANTON, Sonia,
hal.structure.identifierM2A 2015
dc.contributor.authorBOURDA, G.
dc.contributor.authorDAMLJANOVIC, Goran,
hal.structure.identifierSystèmes de Référence Temps Espace [SYRTE]
dc.contributor.authorSOUCHAY, Jean,
dc.contributor.authorVIEIRA MARTINS, Roberto,
hal.structure.identifierNordic Optical Telescope [NOT]
dc.contributor.authorPURSIMO, Tapio,
hal.structure.identifierSystèmes de Référence Temps Espace [SYRTE]
dc.contributor.authorBARACHE, Christophe,
dc.contributor.authorNEPOMUCENO DA SILVA NETO, Dario,
dc.contributor.authorFERNANDES COELHO, Bruno David,
dc.date.issued2015-08
dc.date.conference2015-01-04
dc.description.abstractEnWe have been developing a systematic effort to collect good quality images of the optical counterpart of ICRF sources, in particular for those that have been regularly radio surveyed either for future implementation at high frequencies and/or those that will be the link sources between the ICRF and the Gaia CRF. Observations have been taken at the LNA/Brazil, CASLEO/Argentina, NOT/Spain, LFOA/Austria, Rozhen/Bulgária, and ASV/Serbia. In complement images were collected from the SDSS. As a step to implement such image data bank and make it publicly available through the IERS service we present its description, that comprises for each source the number of measurements, filter, pixel scale, size of field, and seeing at each observation. The photometry analysis is centered on the morphology, since there remain still cases in which the host galaxy is overwhelming, and many cases in which the host asks for a non-stellar PSF modeling. On basis of the neighbor stars we assign magnitudes and variability whenever possible. Finally, assisted by previous literature, the redshift and luminosity are used to derive astrophysical quantities, in special the absolute magnitude, SED and spectral index. Moreover, since Gaia will not obtain direct images of the observed sources, the morphology and magnitude becomes useful as templates onto which assembling and interpreting the one-dimensional and uncontinuous line spread function samplings that will be delivered by Gaia for each QSO.
dc.language.isoen
dc.title.enA Complete Bank of Optical Images of the ICRF QSOs
dc.typeCommunication dans un congrès
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]
bordeaux.page43437
bordeaux.volume22
bordeaux.conference.title2015IAUGA..2243437H - IAU General Assembly, Meeting #29, #2243437 - held 4-8 January 2015 in Seattle, USA
bordeaux.countryUS
bordeaux.conference.citySeattle
bordeaux.peerReviewedoui
hal.identifierhal-01197392
hal.version1
hal.invitednon
hal.proceedingsnon
hal.conference.end2015-01-08
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01197392v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.date=2015-08&rft.volume=22&rft.spage=43437&rft.epage=43437&rft.au=HUMBERTO%20ANDREI,%20Alexandre,&TARIS,%20Francois,&ANTON,%20Sonia,&BOURDA,%20G.&DAMLJANOVIC,%20Goran,&rft.genre=unknown


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