The eROSITA view of the Abell 3391/95 field: The Northern Clump. The largest infalling structure in the longest known gas filament observed with eROSITA, XMM-Newton, and Chandra. (arXiv:2106.14543v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Veronica_A/0/1/0/all/0/1">Angie Veronica</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Su_Y/0/1/0/all/0/1">Yuanyuan Su</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biffi_V/0/1/0/all/0/1">Veronica Biffi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiprich_T/0/1/0/all/0/1">Thomas H. Reiprich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pacaud_F/0/1/0/all/0/1">Florian Pacaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nulsen_P/0/1/0/all/0/1">Paul E. J. Nulsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">Ralph P. Kraft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanders_J/0/1/0/all/0/1">Jeremy S. Sanders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bogdan_A/0/1/0/all/0/1">Akos Bogdan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kara_M/0/1/0/all/0/1">Melih Kara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolag_K/0/1/0/all/0/1">Klaus Dolag</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kerp_J/0/1/0/all/0/1">Jürgen Kerp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koribalski_B/0/1/0/all/0/1">Bärbel S. Koribalski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erben_T/0/1/0/all/0/1">Thomas Erben</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulbul_E/0/1/0/all/0/1">Esra Bulbul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gatuzz_E/0/1/0/all/0/1">Efrain Gatuzz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghirardini_V/0/1/0/all/0/1">Vittorio Ghirardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hopkins_A/0/1/0/all/0/1">Andrew M. Hopkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_A/0/1/0/all/0/1">Ang Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Migkas_K/0/1/0/all/0/1">Konstantinos Migkas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vernstrom_T/0/1/0/all/0/1">Tessa Vernstrom</a>
SRG/eROSITA PV observations revealed the A3391/95 cluster system and the
Northern Clump (MCXC J0621.7-5242 galaxy cluster) are aligning along a cosmic
filament in soft X-rays, similarly to what has been seen in simulations before.
We aim to understand the dynamical state of the Northern Clump as it enters the
atmosphere ($3times R_{200}$) of A3391. We analyzed joint eROSITA, XMM-Newton,
and Chandra observations to probe the morphological, thermal, and chemical
properties of the Northern Clump from its center out to a radius of 988 kpc
($R_{200}$). We utilized the ASKAP/EMU radio data, DECam optical image, and
Planck y-map to study the influence of the WAT radio source on the Northern
Clump central ICM. From the Magneticum simulation, we identified an analog of
the A3391/95 system along with an infalling group resembling the Northern
Clump. The Northern Clump is a WCC cluster centered on a WAT radio galaxy. The
gas temperature over $0.2-0.5R_{500}$ is $k_BT_{500}=1.99pm0.04$ keV. We
employed the $M-T$ scaling relation and obtained a mass estimate of
$M_{500}=(7.68pm0.43)times10^{13}M_{odot}$ and $R_{500}=(636pm12)$ kpc. Its
atmosphere has a boxy shape and deviates from spherical symmetry. We identify a
southern surface brightness edge, likely caused by subsonic motion relative to
the filament gas. At $sim! R_{500}$, the southern atmosphere appears to be
42% hotter than its northern atmosphere. We detect a downstream tail pointing
toward the north with a projected length of $sim318$ kpc, plausibly the result
of ram pressure stripping. The analog group in the Magneticum simulation is
experiencing changes in its gas properties and a shift between the position of
the halo center and that of the bound gas, while approaching the main cluster
pair.
SRG/eROSITA PV observations revealed the A3391/95 cluster system and the
Northern Clump (MCXC J0621.7-5242 galaxy cluster) are aligning along a cosmic
filament in soft X-rays, similarly to what has been seen in simulations before.
We aim to understand the dynamical state of the Northern Clump as it enters the
atmosphere ($3times R_{200}$) of A3391. We analyzed joint eROSITA, XMM-Newton,
and Chandra observations to probe the morphological, thermal, and chemical
properties of the Northern Clump from its center out to a radius of 988 kpc
($R_{200}$). We utilized the ASKAP/EMU radio data, DECam optical image, and
Planck y-map to study the influence of the WAT radio source on the Northern
Clump central ICM. From the Magneticum simulation, we identified an analog of
the A3391/95 system along with an infalling group resembling the Northern
Clump. The Northern Clump is a WCC cluster centered on a WAT radio galaxy. The
gas temperature over $0.2-0.5R_{500}$ is $k_BT_{500}=1.99pm0.04$ keV. We
employed the $M-T$ scaling relation and obtained a mass estimate of
$M_{500}=(7.68pm0.43)times10^{13}M_{odot}$ and $R_{500}=(636pm12)$ kpc. Its
atmosphere has a boxy shape and deviates from spherical symmetry. We identify a
southern surface brightness edge, likely caused by subsonic motion relative to
the filament gas. At $sim! R_{500}$, the southern atmosphere appears to be
42% hotter than its northern atmosphere. We detect a downstream tail pointing
toward the north with a projected length of $sim318$ kpc, plausibly the result
of ram pressure stripping. The analog group in the Magneticum simulation is
experiencing changes in its gas properties and a shift between the position of
the halo center and that of the bound gas, while approaching the main cluster
pair.
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