Ionized and atomic interstellar medium in the z = 6.003 quasar SDSS J2310+1855. (arXiv:2007.12339v2 [astro-ph.GA] UPDATED)

Ionized and atomic interstellar medium in the z = 6.003 quasar SDSS J2310+1855. (arXiv:2007.12339v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Jianan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_R/0/1/0/all/0/1">Ran Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cox_P/0/1/0/all/0/1">Pierre Cox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_Y/0/1/0/all/0/1">Yu Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walter_F/0/1/0/all/0/1">Fabian Walter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wagg_J/0/1/0/all/0/1">Jeff Wagg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">Karl M. Menten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertoldi_F/0/1/0/all/0/1">Frank Bertoldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shao_Y/0/1/0/all/0/1">Yali Shao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venemans_B/0/1/0/all/0/1">Bram P. Venemans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decarli_R/0/1/0/all/0/1">Roberto Decarli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">Dominik Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neri_R/0/1/0/all/0/1">Roberto Neri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_X/0/1/0/all/0/1">Xiaohui Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omont_A/0/1/0/all/0/1">Alain Omont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayanan_D/0/1/0/all/0/1">Desika Narayanan</a>

Observing the interstellar medium (ISM) in $z gtrsim 6$ quasars host
galaxies is essential for understanding the co-evolution between the
supermassive black holes and their hosts. To probe the gas physical conditions
and search for imprints of Active Galactic Nuclei (AGN) on the ISM, we report
ALMA observations of the $rm [N II]_{122 mu m}$ and $rm [O I]_{146 mu m}$
lines and the underlying continuum from the $z=6.003$ quasar SDSS
J231038.88+185519.7. Together with previous $rm [C II]_{158 mu m}$ and $rm
[O III]_{88 mu m}$ observations, we use the ratios of these fine-structure
lines to probe the ISM properties. Similar to other high-$z$ systems, this
object exhibits a $rm [C II]_{158 mu m}$/$rm [O I]_{146 mu m}$ ratio
comparable to the lowest values found in local (Ultra) luminous infrared
galaxies, suggesting a “warmer” and “denser” gas component compared to typical
local systems. The $rm [O III]_{88 mu m}$/$rm [O I]_{146 mu m}$ ratio is
lower than that of other local and high-$z$ systems, indicating a smaller
ionized gas fraction in this quasar. The $rm [O III]_{88 mu m}$/$rm [N
II]_{122 mu m}$ ratio is comparable to that of local systems, and suggests a
metallicity of $Z/Z_{odot}$=1.5$-$2.1. Based on the $rm [N II]_{122 mu m}$
detection, we estimate that $17%$ of the $rm [C II]_{158 mu m}$ emission is
associated with ionized gas. The $rm [N II]_{122 mu m}$ line shows a “flux
deficit” comparable to local systems. The $rm [O I]_{146 mu m}$ line, with a
$rm [O I]_{146 mu m}$/FIR ratio $ge 2times$ than expected from the local
relation, indicates no $rm [O I]_{rm 146 mu m}$ deficit. The low $rm [C
II]_{158 mu m}$/$rm [O I]_{146 mu m}$ ratio, together with the high $rm
[O I]_{146 mu m}$/FIR ratio in J2310+1855, reveals that the warm and dense
gas is likely a result of AGN heating to the ISM.

http://arxiv.org/icons/sfx.gif