The Role of Quasar Radiative Feedback on Galaxy Formation during Cosmic Reionization. (arXiv:1911.09113v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chen_H/0/1/0/all/0/1">Huanqing Chen</a>

Recent observations have found that many $zsim 6$ quasar fields lack
galaxies. This unexpected lack of galaxies may potentially be explained by
quasar radiation feedback. In this paper I present a suite of 3D radiative
transfer cosmological simulations of quasar fields. I find that quasar
radiation suppresses star formation in low mass galaxies, mainly by
photo-dissociating their molecular hydrogen. Photo-heating also plays a role,
but only after $sim$100 Myr. However, galaxies which already have stellar mass
above $10^5 M_odot$ when the quasar turns on will not be suppressed
significantly. Quasar radiative feedback suppresses the faint end of the galaxy
luminosity function (LF) within $1$ pMpc, but to a far lesser degree than the
field-to-field variation of the LF. My study also suggests that by using the
number of bright galaxies ($M_{1500}<-16$) around quasars, we can potentially recover the underlying mass overdensity, which allows us to put reliable constraints on quasar environments.

Recent observations have found that many $zsim 6$ quasar fields lack
galaxies. This unexpected lack of galaxies may potentially be explained by
quasar radiation feedback. In this paper I present a suite of 3D radiative
transfer cosmological simulations of quasar fields. I find that quasar
radiation suppresses star formation in low mass galaxies, mainly by
photo-dissociating their molecular hydrogen. Photo-heating also plays a role,
but only after $sim$100 Myr. However, galaxies which already have stellar mass
above $10^5 M_odot$ when the quasar turns on will not be suppressed
significantly. Quasar radiative feedback suppresses the faint end of the galaxy
luminosity function (LF) within $1$ pMpc, but to a far lesser degree than the
field-to-field variation of the LF. My study also suggests that by using the
number of bright galaxies ($M_{1500}<-16$) around quasars, we can potentially
recover the underlying mass overdensity, which allows us to put reliable
constraints on quasar environments.

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