Astrophys. J., 855, 105-105 (2018/March-2)
The dearth of z ∼ 10 galaxies in all HST legacy fields-the rapid evolution of the galaxy population in the first 500 Myr.
OESCH P.A., BOUWENS R.J., ILLINGWORTH G.D., LABBE I. and STEFANON M.
Abstract (from CDS):
We present an analysis of all prime HST legacy fields spanning >800 arcmin2 in the search for z ∼ 10 galaxy candidates and the study of their UV luminosity function (LF). In particular, we present new z ∼ 10 candidates selected from the full Hubble Frontier Field (HFF) data set. Despite the addition of these new fields, we find a low abundance of z ∼ 10 candidates with only nine reliable sources identified in all prime HST data sets that include the HUDF09/12, the HUDF/XDF, all of the CANDELS fields, and now the HFF survey. Based on this comprehensive search, we find that the UV luminosity function decreases by one order of magnitude from z ∼ 8 to z ∼ 10 over a four-magnitude range. This also implies a decrease of the cosmic star formation rate density by an order of magnitude within 170 Myr from z ∼ 8 to z ∼ 10. We show that this accelerated evolution compared to lower redshift can entirely be explained by the fast build up of the dark matter halo mass function at z > 8. Consequently, the predicted UV LFs from several models of galaxy formation are in good agreement with this observed trend, even though the measured UV LF lies at the low end of model predictions. The difference is generally still consistent within the Poisson and cosmic variance uncertainties. We discuss the implications of these results in light of the upcoming James Webb Space Telescope mission, which is poised to find much larger samples of z ∼ 10 galaxies as well as their progenitors at less than 400 Myr after the big bang.
© 2018. The American Astronomical Society. All rights reserved.
galaxies: evolution - galaxies: formation - galaxies: high-redshift - galaxies: luminosity function, mass function - gravitational lensing: strong
Fig. 1, Table 2: [OBI2018] A370par-JDN (Nos JD1-JD2). Table 6: [OBI2018] MHHMM-NNNN (Nos M0416-874, M1149-3689), [OBI2018] M1149par-NNNN (Nos 2407, 2491), <%M [OBI2018] As1063par-2572) N=1.
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