Статья

The VIMOS VLT deep survey

O. Le FèvreLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]G. VettolaniIstituto di Radio-Astronomia – INAF, 40129 Bologna, ItalyB. GarilliIASF – INAF, 20133 Milano, ItalyL. TresseLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]D. BottiniIASF – INAF, 20133 Milano, ItalyV. Le BrunLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]D. MaccagniIASF – INAF, 20133 Milano, ItalyJ. P. PicatLaboratoire d'Astrophysique – Observatoire Midi-Pyrénées, 31400 Toulouse, FranceR. ScaramellaIstituto di Radio-Astronomia – INAF, 40129 Bologna, ItalyM. ScodeggioIASF – INAF, 20133 Milano, ItalyA. ZanichelliIstituto di Radio-Astronomia – INAF, 40129 Bologna, ItalyC. AdamiLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]M. ArnaboldiOsservatorio Astronomico di Capodimonte – INAF, via Moiariello 16, 80131 Napoli, ItalyS. ArnoutsLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]S. BardelliOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyM. BolzonellaUniversity of BolognaA. CappiOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyS. CharlotInstitut d'Astrophysique de Paris, UMR 7095, 98bis Bd. Arago, 75014 Paris, FranceP. CiliegiOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyT. ContiniLaboratoire d'Astrophysique – Observatoire Midi-Pyrénées, 31400 Toulouse, FranceS. FoucaudIASF – INAF, 20133 Milano, ItalyP. FranzettiIASF – INAF, 20133 Milano, ItalyI. GavignaudEuropean Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, GermanyL. GuzzoOsservatorio Astronomico di Brera – INAF, via Brera 28, 20121 Milan, ItalyO. IlbertLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]A. IovinoOsservatorio Astronomico di Brera – INAF, via Brera 28, 20121 Milan, ItalyH. J. McCrackenInstitut d'Astrophysique de Paris, UMR 7095, 98bis Bd. Arago, 75014 Paris, FranceB. MaranoUniversità di Bologna, Dipartimento di Astronomia, via Ranzani, 1, 40127 Bologna, ItalyC. MarinoniLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]G. MathezLaboratoire d'Astrophysique – Observatoire Midi-Pyrénées, 31400 Toulouse, FranceA. MazureLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]B. MeneuxLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]R. MerighiOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyS. PaltaniLaboratoire d'Astrophysique de Marseille, OAMP, Université de Provence, UMR 6110, Traverse du Siphon-Les trois Lucs, 13012 Marseille, France, e-mail: [email protected]R. PellóLaboratoire d'Astrophysique – Observatoire Midi-Pyrénées, 31400 Toulouse, FranceA. PolloOsservatorio Astronomico di Brera – INAF, via Brera 28, 20121 Milan, ItalyL. PozzettiOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyM. RadovichOsservatorio Astronomico di Capodimonte – INAF, via Moiariello 16, 80131 Napoli, ItalyG. ZamoraniOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyE. ZuccaOsservatorio Astronomico di Bologna – INAF, via Ranzani 1, 40127 Bologna, ItalyM. BondiIstituto di Radio-Astronomia – INAF, 40129 Bologna, ItalyA. BongiornoUniversità di Bologna, Dipartimento di Astronomia, via Ranzani, 1, 40127 Bologna, ItalyG. BusarelloOsservatorio Astronomico di Capodimonte – INAF, via Moiariello 16, 80131 Napoli, ItalyFabrice LamareilleLaboratoire d'Astrophysique – Observatoire Midi-Pyrénées, 31400 Toulouse, FranceY. MellierInstitut d'Astrophysique de Paris, UMR 7095, 98bis Bd. Arago, 75014 Paris, FranceP. MerluzziOsservatorio Astronomico di Capodimonte – INAF, via Moiariello 16, 80131 Napoli, ItalyV. RipepiOsservatorio Astronomico di Capodimonte – INAF, via Moiariello 16, 80131 Napoli, ItalyD. RizzoLaboratoire d'Astrophysique – Observatoire Midi-Pyrénées, 31400 Toulouse, France

2005en

ABI

Аннотация

This paper presents the “First Epoch” sample from the VIMOS VLT Deep Survey (VVDS). The VVDS goals, observations, data reduction with the VIPGI pipeline and redshift measurement scheme with KBRED are discussed. Data have been obtained with the VIsible Multi Object Spectrograph (VIMOS) on the ESO-VLT UT3, allowing us to observe 600 slits simultaneously at a spectral resolution . A total of 11 564 objects have been observed in the VVDS-02h and VVDS-CDFS “Deep” fields over a total area of deg2, selected solely on the basis of apparent magnitude . The VVDS efficiently covers the redshift range . It is successfully going through the “redshift desert” , while the range remains of difficult access because of the VVDS wavelength coverage. A total of 9677 galaxies have a redshift measurement, 836 objects are stars, 90 objects are AGN, and a redshift could not be measured for 961 objects. There are 1065 galaxies with a measured redshift . When considering only the primary spectroscopic targets, the survey reaches a redshift measurement completeness of 78% overall (93% including less reliable flag 1 objects), with a spatial sampling of the population of galaxies of ~25% and ~30% in the VVDS-02h and VVDS-CDFS respectively. The redshift accuracy measured from repeated observations with VIMOS and comparison to other surveys is ~276 km s-1. From this sample we are able to present for the first time the redshift distribution of a magnitude-limited spectroscopic sample down to . The redshift distribution has a median of , , , and , for magnitude-limited samples with , 23.0, 23.5 and 24.0 respectively. A high redshift tail above redshift 2 and up to redshift 5 becomes readily apparent for , probing the bright star-forming population of galaxies. This sample provides an unprecedented dataset to study galaxy evolution over ~90% of the life of the universe.

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Идентификаторы

DOI: 10.1051/0004-6361:20041960

Цитирования и источники

Цитирований: 3Использованных источников: 0

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