MUSEQuBES: The relation between Ly$alpha$ emitters and C IV absorbers at $z approx 3.3$. (arXiv:2304.04788v1 [astro-ph.GA])

MUSEQuBES: The relation between Ly$alpha$ emitters and C IV absorbers at $z approx 3.3$. (arXiv:2304.04788v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Banerjee_E/0/1/0/all/0/1">Eshita Banerjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muzahid_S/0/1/0/all/0/1">Sowgat Muzahid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaye_J/0/1/0/all/0/1">Joop Schaye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_S/0/1/0/all/0/1">Sean D. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cantalupo_S/0/1/0/all/0/1">Sebastiano Cantalupo</a>

We present a detailed study of the column density and covering fraction
profiles of C IV absorption around 86 redshift $z approx 3.3$ Ly$alpha$
emitters (LAEs) detected in 8 Multi-Unit Spectroscopic Explorer (MUSE) fields
of $1’times 1’$ centered on 8 bright background quasars as part of the
MUSEQuBES survey. Using Voigt profile fitting of all the C IV absorbers
detected along these 8 sightlines, we generated a “blind” absorbers’ catalog
consisting of 489 C IV absorption components. We cross-matched this blind C IV
catalog with the MUSE-detected LAE catalog and found a significant enhancement
of C IV components within $approx pm$400 $rm km, s^{-1}$ of the systemic
redshifts of the LAEs. Neither the C IV column density ($N$) nor the Doppler
parameter ($b$) of individual C IV components shows any significant
anti-correlation with impact parameter ($rho$) of the LAEs in the 68
percentile range of $90leq rho leq 230$ physical kpc (pkpc). We find a
covering fraction of $approx 60%$ for a threshold $N$(C IV) of $10^{12.5},
rm rm cm^{-2}$, which is roughly twice as high as in random regions. The C IV
covering fraction remains constant at $approx50%$ for impact parameters in
the range 150–250~pkpc ($approx 3-6 R_{200}$). Using the covering fraction
profile, we constrained the LAE–C IV absorber two-point correlation function,
and obtained $r_0 = 3.2~h^{-1}$ comoving Mpc (cMpc) and $gamma = 1.2$ for a
threshold $N$(C IV) of $10^{13.0}, rm cm^{-2}$. The C IV covering fraction is
found to be enhanced for the LAEs that are part of a “pair/group” compared to
the isolated ones.

We present a detailed study of the column density and covering fraction
profiles of C IV absorption around 86 redshift $z approx 3.3$ Ly$alpha$
emitters (LAEs) detected in 8 Multi-Unit Spectroscopic Explorer (MUSE) fields
of $1’times 1’$ centered on 8 bright background quasars as part of the
MUSEQuBES survey. Using Voigt profile fitting of all the C IV absorbers
detected along these 8 sightlines, we generated a “blind” absorbers’ catalog
consisting of 489 C IV absorption components. We cross-matched this blind C IV
catalog with the MUSE-detected LAE catalog and found a significant enhancement
of C IV components within $approx pm$400 $rm km, s^{-1}$ of the systemic
redshifts of the LAEs. Neither the C IV column density ($N$) nor the Doppler
parameter ($b$) of individual C IV components shows any significant
anti-correlation with impact parameter ($rho$) of the LAEs in the 68
percentile range of $90leq rho leq 230$ physical kpc (pkpc). We find a
covering fraction of $approx 60%$ for a threshold $N$(C IV) of $10^{12.5},
rm rm cm^{-2}$, which is roughly twice as high as in random regions. The C IV
covering fraction remains constant at $approx50%$ for impact parameters in
the range 150–250~pkpc ($approx 3-6 R_{200}$). Using the covering fraction
profile, we constrained the LAE–C IV absorber two-point correlation function,
and obtained $r_0 = 3.2~h^{-1}$ comoving Mpc (cMpc) and $gamma = 1.2$ for a
threshold $N$(C IV) of $10^{13.0}, rm cm^{-2}$. The C IV covering fraction is
found to be enhanced for the LAEs that are part of a “pair/group” compared to
the isolated ones.

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