Volume 511, February 2010
|Number of page(s)||16|
|Section||Cosmology (including clusters of galaxies)|
|Published online||24 February 2010|
Evidence of a fast evolution of the UV luminosity function beyond redshift 6 from a deep HAWK-I survey of the GOODS-S field
INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy e-mail: email@example.com
2 Lick Observatory, University of California, Santa Cruz, CA 95064, USA
3 NOAO, 950 N. Cherry Avenue, Tucson, AZ 85719, USA
4 Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA
5 INAF - Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy
6 INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
7 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
8 INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
Accepted: 10 November 2009
Aims. We perform a deep search for galaxies in the redshift range , to measure the evolution of the number density of luminous galaxies in this redshift range and derive useful constraints on the evolution of their luminosity function.
Methods. We present here the first results of an ESO Large Programme, which exploits the unique combination of area and sensitivity provided in the near-IR by the camera Hawk-I at the VLT. We have obtained two Hawk-I pointings on the GOODS South field for a total of observing hours, covering . The images reach Y=26.7 mag for the two fields. We used public ACS images in the z band to select z-dropout galaxies with the colour criteria , , and . The other public data in the UBVRIJK bands are used to reject possible low redshift interlopers. The output has been compared with extensive Monte Carlo simulations to quantify the observational effects of our selection criteria, as well as the effects of photometric errors.
Results. We detect 7 high-quality candidates in the magnitude range . This interval samples the critical range for at z>6 ( to -21.5). After accounting for the expected incompleteness, we rule out a luminosity function constant from z=6 to z=7 at a 99% confidence level, even including the effects of cosmic variance. For galaxies brighter than , we derive a luminosity density , implying a decrease by a factor 3.5 from z=6 to . On the basis of our findings, we make predictions for the surface densities expected in future surveys, based on ULTRA-VISTA, HST-WFC3, or JWST-NIRCam, evaluating the best observational strategy to maximise their impact.
Key words: galaxies: distances and redshifts / galaxies: high-redshift / galaxies: luminosity function, mass function / galaxies: evolution
© ESO, 2010
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