UV Luminosity Functions at redshifts z\textasciitilde4 to z\textasciitilde10: 10000 Galaxies from HST Legacy Fields. Bouwens, R. J., Illingworth, G. D., Oesch, P. A., Trenti, M., Labbe', I., Bradley, L., Carollo, M., van Dokkum, P. G., Gonzalez, V., Holwerda, B., Franx, M., Spitler, L., Smit, R., & Magee, D. The Astrophysical Journal, 803(1):34, April, 2015. arXiv: 1403.4295![UV Luminosity Functions at redshifts z\textasciitilde4 to z\textasciitilde10: 10000 Galaxies from HST Legacy Fields [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex The remarkable HST datasets from the CANDELS, HUDF09, HUDF12, ERS, and BoRG/HIPPIES programs have allowed us to map out the evolution of the UV LF from z\textasciitilde10 to z\textasciitilde4. We have identified 5859, 3001, 857, 481, 217, and 6 galaxy candidates at z\textasciitilde4, z\textasciitilde5, z\textasciitilde6, z\textasciitilde7, z\textasciitilde8, and z\textasciitilde10, respectively from the \textasciitilde1000 arcmin**2 area probed. The selection of z\textasciitilde4-8 galaxies over the five CANDELS fields allows us to assess the cosmic variance; the largest variations are apparent at z\textgreater=7. Our new LF determinations at z\textasciitilde4 and z\textasciitilde5 span a 6-mag baseline (-22.5 to -16 AB mag). These determinations agree well with previous estimates, but the larger samples and volumes probed here result in a more reliable sampling of \textgreaterL* galaxies and allow us to reassess the form of the UV LFs. Our new LF results strengthen our earlier findings to 3.4 sigma significance for a steeper faint-end slope to the UV LF at z\textgreater4, with alpha evolving from alpha=-1.64+/-0.04 at z\textasciitilde4 to alpha=-2.06+/-0.13 at z\textasciitilde7 (and alpha = -2.02+/-0.23 at z\textasciitilde8), consistent with that expected from the evolution of the halo mass function. With our improved constraints at the bright end, we find less evolution in the characteristic luminosity M* over the redshift range z\textasciitilde4 to z\textasciitilde7; the observed evolution in the LF is now largely represented by changes in phi*. No evidence for a non-Schechter-like form to the z\textasciitilde4-8 LFs is found. A simple conditional LF model based on halo growth and evolution in the M/L ratio of halos ((1+z)**-1.5) provides a good representation of the observed evolution.
@article{bouwens_uv_2015,
title = {{UV} {Luminosity} {Functions} at redshifts z{\textasciitilde}4 to z{\textasciitilde}10: 10000 {Galaxies} from {HST} {Legacy} {Fields}},
volume = {803},
issn = {1538-4357},
shorttitle = {{UV} {Luminosity} {Functions} at redshifts z{\textasciitilde}4 to z{\textasciitilde}10},
url = {http://arxiv.org/abs/1403.4295},
doi = {10.1088/0004-637X/803/1/34},
abstract = {The remarkable HST datasets from the CANDELS, HUDF09, HUDF12, ERS, and BoRG/HIPPIES programs have allowed us to map out the evolution of the UV LF from z{\textasciitilde}10 to z{\textasciitilde}4. We have identified 5859, 3001, 857, 481, 217, and 6 galaxy candidates at z{\textasciitilde}4, z{\textasciitilde}5, z{\textasciitilde}6, z{\textasciitilde}7, z{\textasciitilde}8, and z{\textasciitilde}10, respectively from the {\textasciitilde}1000 arcmin**2 area probed. The selection of z{\textasciitilde}4-8 galaxies over the five CANDELS fields allows us to assess the cosmic variance; the largest variations are apparent at z{\textgreater}=7. Our new LF determinations at z{\textasciitilde}4 and z{\textasciitilde}5 span a 6-mag baseline (-22.5 to -16 AB mag). These determinations agree well with previous estimates, but the larger samples and volumes probed here result in a more reliable sampling of {\textgreater}L* galaxies and allow us to reassess the form of the UV LFs. Our new LF results strengthen our earlier findings to 3.4 sigma significance for a steeper faint-end slope to the UV LF at z{\textgreater}4, with alpha evolving from alpha=-1.64+/-0.04 at z{\textasciitilde}4 to alpha=-2.06+/-0.13 at z{\textasciitilde}7 (and alpha = -2.02+/-0.23 at z{\textasciitilde}8), consistent with that expected from the evolution of the halo mass function. With our improved constraints at the bright end, we find less evolution in the characteristic luminosity M* over the redshift range z{\textasciitilde}4 to z{\textasciitilde}7; the observed evolution in the LF is now largely represented by changes in phi*. No evidence for a non-Schechter-like form to the z{\textasciitilde}4-8 LFs is found. A simple conditional LF model based on halo growth and evolution in the M/L ratio of halos ((1+z)**-1.5) provides a good representation of the observed evolution.},
number = {1},
urldate = {2016-07-11},
journal = {The Astrophysical Journal},
author = {Bouwens, R. J. and Illingworth, G. D. and Oesch, P. A. and Trenti, M. and Labbe', I. and Bradley, L. and Carollo, M. and van Dokkum, P. G. and Gonzalez, V. and Holwerda, B. and Franx, M. and Spitler, L. and Smit, R. and Magee, D.},
month = apr,
year = {2015},
note = {arXiv: 1403.4295},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {34},
}
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G.","Gonzalez, V.","Holwerda, B.","Franx, M.","Spitler, L.","Smit, R.","Magee, D."],"bibdata":{"bibtype":"article","type":"article","title":"UV Luminosity Functions at redshifts z\\textasciitilde4 to z\\textasciitilde10: 10000 Galaxies from HST Legacy Fields","volume":"803","issn":"1538-4357","shorttitle":"UV Luminosity Functions at redshifts z\\textasciitilde4 to z\\textasciitilde10","url":"http://arxiv.org/abs/1403.4295","doi":"10.1088/0004-637X/803/1/34","abstract":"The remarkable HST datasets from the CANDELS, HUDF09, HUDF12, ERS, and BoRG/HIPPIES programs have allowed us to map out the evolution of the UV LF from z\\textasciitilde10 to z\\textasciitilde4. We have identified 5859, 3001, 857, 481, 217, and 6 galaxy candidates at z\\textasciitilde4, z\\textasciitilde5, z\\textasciitilde6, z\\textasciitilde7, z\\textasciitilde8, and z\\textasciitilde10, respectively from the \\textasciitilde1000 arcmin**2 area probed. The selection of z\\textasciitilde4-8 galaxies over the five CANDELS fields allows us to assess the cosmic variance; the largest variations are apparent at z\\textgreater=7. Our new LF determinations at z\\textasciitilde4 and z\\textasciitilde5 span a 6-mag baseline (-22.5 to -16 AB mag). These determinations agree well with previous estimates, but the larger samples and volumes probed here result in a more reliable sampling of \\textgreaterL* galaxies and allow us to reassess the form of the UV LFs. Our new LF results strengthen our earlier findings to 3.4 sigma significance for a steeper faint-end slope to the UV LF at z\\textgreater4, with alpha evolving from alpha=-1.64+/-0.04 at z\\textasciitilde4 to alpha=-2.06+/-0.13 at z\\textasciitilde7 (and alpha = -2.02+/-0.23 at z\\textasciitilde8), consistent with that expected from the evolution of the halo mass function. With our improved constraints at the bright end, we find less evolution in the characteristic luminosity M* over the redshift range z\\textasciitilde4 to z\\textasciitilde7; the observed evolution in the LF is now largely represented by changes in phi*. No evidence for a non-Schechter-like form to the z\\textasciitilde4-8 LFs is found. 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Our new LF results strengthen our earlier findings to 3.4 sigma significance for a steeper faint-end slope to the UV LF at z{\\textgreater}4, with alpha evolving from alpha=-1.64+/-0.04 at z{\\textasciitilde}4 to alpha=-2.06+/-0.13 at z{\\textasciitilde}7 (and alpha = -2.02+/-0.23 at z{\\textasciitilde}8), consistent with that expected from the evolution of the halo mass function. With our improved constraints at the bright end, we find less evolution in the characteristic luminosity M* over the redshift range z{\\textasciitilde}4 to z{\\textasciitilde}7; the observed evolution in the LF is now largely represented by changes in phi*. No evidence for a non-Schechter-like form to the z{\\textasciitilde}4-8 LFs is found. 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