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To understand the evolution of galaxies, we need to know as accurately as possible how many galaxies were present in the Universe at different epochs. Galaxies in the young Universe have hitherto mainly been identified using their expected optical colours, but this leaves open the possibility that a significant population remains undetected because their(More)
Observations of distant supernovae indicate that the Universe is now in a phase of accelerated expansion the physical cause of which is a mystery. Formally, this requires the inclusion of a term acting as a negative pressure in the equations of cosmic expansion, accounting for about 75 per cent of the total energy density in the Universe. The simplest(More)
Context. Understanding the relationship between the formation and evolution of galaxies and their central super massive black holes (SMBH) is one of the main topics in extragalactic astrophysics. Links and feedback may reciprocally affect both black hole and galaxy growth. Aims. Observations of the CO line at redshifts of 2-4 are crucial to investigate the(More)
(Affiliations can be found after the references) Received – – —-; accepted – – —-ABSTRACT Aims. The availability of wide angle and deep surveys , both in the optical and the radio band , allows us to explore the evolution of radio sources with optical counterparts up to redshift z ∼ 1. 1 in an unbiased way , using not only large numbers of radio sources but(More)
In this paper we present the optical and near-infrared identifications of the 1054 radio sources detected in the 20cm deep radio survey down to a 5σ flux limit of ∼80µJy obtained with the VLA in the VIMOS VLT Deep Survey VVDS-02h deep field. (50% completeness) we identified 718 radio sources (∼74% of the whole sample). The photometric redshift analysis(More)
In a previous paper (Gavignaud et al. 2006), we presented the type–1 Active Galactic Nuclei (AGN) sample obtained from the first epoch data of the VIMOS-VLT Deep Survey (VVDS). The sample consists of 130 faint, broad-line AGN with redshift up to z = 5 and 17.5 < I AB < 24.0, selected on the basis of their spectra. In this paper we present the measurement of(More)
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