TY - JOUR
T1 - The eROSITA view of the Abell 3391/95 field
T2 - The Northern Clump The largest infalling structure in the longest known gas filament observed with eROSITA, XMM-Newton, and Chandra
AU - Veronica, Angie
AU - Su, Yuanyuan
AU - Biffi, Veronica
AU - Reiprich, Thomas H.
AU - Pacaud, Florian
AU - Nulsen, Paul E. J.
AU - Kraft, Ralph P.
AU - Sanders, Jeremy S.
AU - Bogdan, Akos
AU - Kara, Melih
AU - Dolag, Klaus
AU - Kerp, Juergen
AU - Koribalski, Barbel S.
AU - Bulbul, Esra
AU - Gatuzz, Efrain
AU - Ghirardini, Vittorio
AU - Hopkins, Andrew M.
AU - Liu, Ang
AU - Vernstrom, Tessa
PY - 2022/5
Y1 - 2022/5
N2 - Context. Galaxy clusters grow through mergers and the accretion of substructures along large-scale filaments. Many of the missing baryons in the local Universe may reside in such filaments as the warm-hot intergalactic medium (WHIM).Aims. SRG/eROSITA performance verification observations revealed that the binary cluster Abell 3391/3395 and the Northern Clump (the 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 (3 x R-200) of Abell 3391.Methods. 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, the DECam optical image, and the Planck y-map to study the influence of the wide-angle tail (WAT) radio source on the Northern Clump's central intracluster medium. Using eROSITA data, we also analyzed the gas properties of the Northern Filament, the region between the virial radii of the Northern Clump and the A3391 cluster. From the Magneticum simulation, we identified an analog of the A3391/95 system along with an infalling group resembling the Northern Clump.Results. The Northern Clump is a weak cool-core cluster centered on a WAT radio galaxy. The gas temperature over 0.2-0.5R(500) is k(B)T(500 )= 1.99 +/- 0.04 keV. We employed the mass-temperature (M - T) scaling relation and obtained a mass estimate of M-500 = (7.68 +/- 0.43) x 10(13) M circle dot and R-500 = (636 +/- 12) kpc. Its X-ray 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 in the southern direction. At similar to R-500, the southern atmosphere (infalling head) appears to be 42% hotter than its northern atmosphere. We detect a downstream tail pointing toward the north with a projected length of similar to 318 kpc, plausibly the result of ram pressure stripping. Through a two-temperature fit, we identify a cooler component in the Northern Filament with k(B)T = 0.68(-0.64)(+0.38) keV and n(e) = 1.991(-1.24)(+0.88) 10(-5 )cm(-3), which are consistent within the expected ranges of WHIM properties. 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.Conclusions. The Northern Clump is a dynamically active system and far from being relaxed. Its atmosphere is affected by an interaction with the WAT and by gas sloshing or its infall toward Abell 3391 along the filament, consistent with the analog group-size halo in the Magneticum simulation.
AB - Context. Galaxy clusters grow through mergers and the accretion of substructures along large-scale filaments. Many of the missing baryons in the local Universe may reside in such filaments as the warm-hot intergalactic medium (WHIM).Aims. SRG/eROSITA performance verification observations revealed that the binary cluster Abell 3391/3395 and the Northern Clump (the 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 (3 x R-200) of Abell 3391.Methods. 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, the DECam optical image, and the Planck y-map to study the influence of the wide-angle tail (WAT) radio source on the Northern Clump's central intracluster medium. Using eROSITA data, we also analyzed the gas properties of the Northern Filament, the region between the virial radii of the Northern Clump and the A3391 cluster. From the Magneticum simulation, we identified an analog of the A3391/95 system along with an infalling group resembling the Northern Clump.Results. The Northern Clump is a weak cool-core cluster centered on a WAT radio galaxy. The gas temperature over 0.2-0.5R(500) is k(B)T(500 )= 1.99 +/- 0.04 keV. We employed the mass-temperature (M - T) scaling relation and obtained a mass estimate of M-500 = (7.68 +/- 0.43) x 10(13) M circle dot and R-500 = (636 +/- 12) kpc. Its X-ray 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 in the southern direction. At similar to R-500, the southern atmosphere (infalling head) appears to be 42% hotter than its northern atmosphere. We detect a downstream tail pointing toward the north with a projected length of similar to 318 kpc, plausibly the result of ram pressure stripping. Through a two-temperature fit, we identify a cooler component in the Northern Filament with k(B)T = 0.68(-0.64)(+0.38) keV and n(e) = 1.991(-1.24)(+0.88) 10(-5 )cm(-3), which are consistent within the expected ranges of WHIM properties. 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.Conclusions. The Northern Clump is a dynamically active system and far from being relaxed. Its atmosphere is affected by an interaction with the WAT and by gas sloshing or its infall toward Abell 3391 along the filament, consistent with the analog group-size halo in the Magneticum simulation.
KW - galaxies: clusters: individual: Northern Clump
KW - galaxies: clusters: individual: MCXCJ0621.7-5242
KW - galaxies: clusters: individual: A3391
KW - galaxies: clusters: intracluster medium
KW - X-rays: galaxies: clusters
KW - LARGE-SCALE STRUCTURE
KW - X-RAY
KW - GALAXY CLUSTERS
KW - CENTAURUS CLUSTER
KW - MISSING BARYONS
KW - RADIO GALAXIES
KW - OUTSKIRTS
KW - CATALOG
KW - PLASMA
KW - CORE
U2 - 10.1051/0004-6361/202141415
DO - 10.1051/0004-6361/202141415
M3 - Article
SN - 0004-6361
VL - 661
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
M1 - A46
ER -