Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733550h&link_type=abstract
American Astronomical Society, AAS Meeting #217, #335.50; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Searching high redshift galaxies is one of the most active fields of observational cosmology and is essential to the characterization and understanding of the formation and evolution of the galaxies. Galaxies at redshift 6 are routinely found. Detection of z 7 galaxies is however still rare. From z=6.5 to z=7 light dimming due to luminosity distance is 17% and the age of the Universe varies by 172 Myr. At these redshift, the Universe is thought to be undergoing re-ionization. One tracer of high z galaxies is the Ly-alpha line which can be detected through Narrow Band (NB) imaging surveys. The Luminosity Function (LF) of high z LAEs is one of the few observables of the re-ionization epoch accessible to date with 8-10m telescopes. The determination of the Ly-alpha LF at high z is actively pursued by several groups. The evolution of the Ly-alpha LF involves both the evolution of the re-ionization state of the Universe and of the Ly-alpha population which can also be traced by the evolution of the UVLF. This evolution with redshift allows us to constrain the evolution of LAEs and their role in re-ionizing the Universe at the end of the Dark Ages. Results on the evolution of both UVLF and LAEs LF at z 7 are still limited and occasionally contradictory. We have carried out a 28 hours NB (9680A) imaging program, targeting z 7 LAEs, using the IMACS/Magellan instrument. The data were taken over 2 years. We reached a detection limit of 8.9e-18 erg/s/cm2. From these observations, we have derived a photometric sample of z 7 LAEs candidates. After careful evaluation of possible sources of contamination, and accounting for cosmic variance, we inferred the LF at z 7 LAEs and constrain the LFs produced by different existing models. These results will need to be confirmed by spectroscopic follow-up.
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