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

Angie Veronica; Yuanyuan Su; Veronica Biffi; Thomas H. Reiprich; Florian Pacaud; Paul E.J. Nulsen; Ralph P. Kraft; Jeremy S. Sanders; Akos Bogdan; Melih Kara; Klaus Dolag; Jürgen Kerp; Bärbel S. Koribalski; Thomas Erben; Esra Bulbul; Efrain Gatuzz; Vittorio Ghirardini; Andrew M. Hopkins; Ang Liu; Konstantinos Migkas; Tessa Vernstrom

doi:10.1051/0004-6361/202141415

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

Angie Veronica, Yuanyuan Su, Veronica Biffi, Thomas H. Reiprich, Florian Pacaud, Paul E.J. Nulsen, Ralph P. Kraft, Jeremy S. Sanders, Akos Bogdan, Melih Kara, Klaus Dolag, Jürgen Kerp, Bärbel S. Koribalski, Thomas Erben, Esra Bulbul, Efrain Gatuzz, Vittorio Ghirardini, Andrew M. Hopkins, Ang Liu, Konstantinos MigkasTessa Vernstrom

Research output: Contribution to journal › Article › peer-review

12 Scopus citations

Abstract

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 ÃÂ-R200) 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 (R200). 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 0.2-0.5R500 is kBT500 = 1.99 ± 0.04 keV. We employed the mass-temperature (M -T) scaling relation and obtained a mass estimate of M500 = (7.68 ± 0.43) ÃÂ-1013 M and R500 = (63 6 ± 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 ~R500, 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 ~318 kpc, plausibly the result of ram pressure stripping. Through a two-temperature fit, we identify a cooler component in the Northern Filament with kBT = 0.68- 0.64+ 0.38 keV kBT=0.68 0.64+0.38keV and ne = 1.99-1.24+0.88 ÃÂ-10-5cm-3, ne1.99 1.24+0.88ÃÂ-*10 5cm 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.

Original language	English
Article number	A46
Journal	Astronomy and Astrophysics
Volume	661
DOIs	https://doi.org/10.1051/0004-6361/202141415
State	Published - May 1 2022

Bibliographical note

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Funding

aboard SRG, a joint Russian-German science mission supported by the Russian Space Agency (Roskosmos), in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI), and the Deutsches Zentrum für Luft-und Raumfahrt (DLR). The SRG spacecraft was built by Lavochkin Association (NPOL) and its subcontractors, and is operated by NPOL with support from the Max Planck Institute for Extraterrestrial Physics (MPE). The development and construction of the eROSITA X-ray instrument was led by MPE, with contributions from the Dr. Karl Remeis Observatory Bamberg and ECAP (FAU Erlangen-Nuernberg), the University of Hamburg Observatory, the Leibniz Institute for Astrophysics Potsdam (AIP), and the Institute for Astronomy and Astrophysics of the University of Tübingen, with the support of DLR and the Max Planck Society. The Argelander Institute for Astronomy of the University of Bonn and the Ludwig Maximilians Universität Munich also participated in the science preparation for eROSITA. The eROSITA data shown here were processed using the eSASS/NRTA software system developed by the German eROSITA consortium. Partly based on observations obtained with XMMNewton , an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We acknowledge the Wajarri Yamatji people as the traditional owners of the Murchison Radio-astronomy Observatory, where ASKAP is located. cA knowledgements. We would like to thank the anonymous referee for their valuable feedback that helped improve the manuscript. We thank Kaustuv moni Basu for discussion about the Planck y-map. Funded by the Deutsche Forschungs-gemeinschaft (DFG, German Research Foundation) – 450861021. This research was supported by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC-2094 – 390783311. V.B. acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – 415510302. Y.S. acknowledges support from Chandra grants AR8-19020A and GO1-22126X. A.V. is a member of the Max-Planck International School for Astronomy and Astrophysics (IMPRS) and of the Bonn-Cologne Graduate School for Physics and Astronomy (BCGS), and thanks for their support. This work is based on data from eROSITA, the soft X-ray instrument We would like to thank the anonymous referee for their valuable feedback that helped improve the manuscript. We thank Kaustuv moni Basu for discussion about the Planck y-map. Funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)-450861021. This research was supported by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy-EXC-2094-390783311. V.B. acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)-415510302. Y.S. acknowledges support from Chandra grants AR8-19020A and GO1-22126X. A.V. is a member of the Max-Planck International School for Astronomy and Astrophysics (IMPRS) and of the Bonn-Cologne Graduate School for Physics and Astronomy (BCGS), and thanks for their support. This work is based on data from eROSITA, the soft X-ray instrument aboard SRG, a joint Russian-German science mission supported by the Russian Space Agency (Roskosmos), in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI), and the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). The SRG spacecraft was built by Lavochkin Association (NPOL) and its subcontractors, and is operated by NPOL with support from the Max Planck Institute for Extraterrestrial Physics (MPE). The development and construction of the eROSITA X-ray instrument was led by MPE, with contributions from the Dr. Karl Remeis Observatory Bamberg and ECAP (FAU Erlangen-Nuernberg), the University of Hamburg Observatory, the Leibniz Institute for Astrophysics Potsdam (AIP), and the Institute for Astronomy and Astrophysics of the University of Tubingen, with the support of DLR and the Max Planck Society. The Argelander Institute for Astronomy of the University of Bonn and the Ludwig Maximilians Universitat Munich also participated in the science preparation for eROSITA. The eROSITA data shown here were processed using the eSASS/NRTA software system developed by the German eROSITA consortium. Partly based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We acknowledge the Wajarri Yamatji people as the traditional owners of the Murchison Radio-astronomy Observatory, where ASKAP is located

Funders	Funder number
Bonn-Cologne Graduate School for Physics and Astronomy
FAU Erlangen-Nuernberg
Lavochkin Association
Max Planck Institute for Extraterrestrial Physics
Max-Planck International School for Astronomy and Astrophysics
NPOL
Russian Space Agency
University of Hamburg Observatory
National Aeronautics and Space Administration
European Space Agency
Deutsche Forschungsgemeinschaft	AR8-19020A, EXC-2094 – 390783311, 450861021, 415510302, GO1-22126X
Deutsche Forschungsgemeinschaft
Eberhard Karls Universität Tübingen
Deutsches Zentrum für Luft- und Raumfahrt
Fritz-Haber-Institut der Max-Planck-Gesellschaft
Ludwig–Maximilians–Universität München
Rheinische Friedrich-Wilhelms-Universität Bonn
International Max Planck Research School for Advanced Methods in Process and Systems Engineering
Leibniz-Institut für Astrophysik Potsdam

Keywords

Galaxies: clusters: individual: A3391
Galaxies: clusters: individual: MCXCJ0621.7-5242
Galaxies: clusters: individual: Northern Clump
Galaxies: clusters: intracluster medium
X-rays: galaxies: clusters

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/202141415

Cite this

Veronica, A., Su, Y., Biffi, V., Reiprich, T. H., Pacaud, F., Nulsen, P. E. J., Kraft, R. P., Sanders, J. S., Bogdan, A., Kara, M., Dolag, K., Kerp, J., Koribalski, B. S., Erben, T., Bulbul, E., Gatuzz, E., Ghirardini, V., Hopkins, A. M., Liu, A., ... Vernstrom, T. (2022). 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. Astronomy and Astrophysics, 661, Article A46. https://doi.org/10.1051/0004-6361/202141415

@article{92c3a305c4a348feb9d77e40832043f4,

title = "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",

abstract = "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 {\~A}{\^A}-R200) 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 (R200). 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 0.2-0.5R500 is kBT500 = 1.99 ± 0.04 keV. We employed the mass-temperature (M -T) scaling relation and obtained a mass estimate of M500 = (7.68 ± 0.43) {\~A}{\^A}-1013 M and R500 = (63 6 ± 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 ~R500, 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 ~318 kpc, plausibly the result of ram pressure stripping. Through a two-temperature fit, we identify a cooler component in the Northern Filament with kBT = 0.68- 0.64+ 0.38 keV kBT=0.68 0.64+0.38keV and ne = 1.99-1.24+0.88 {\~A}{\^A}-10-5cm-3, ne1.99 1.24+0.88{\~A}{\^A}-*10 5cm 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.",

keywords = "Galaxies: clusters: individual: A3391, Galaxies: clusters: individual: MCXCJ0621.7-5242, Galaxies: clusters: individual: Northern Clump, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters",

author = "Angie Veronica and Yuanyuan Su and Veronica Biffi and Reiprich, {Thomas H.} and Florian Pacaud and Nulsen, {Paul E.J.} and Kraft, {Ralph P.} and Sanders, {Jeremy S.} and Akos Bogdan and Melih Kara and Klaus Dolag and J{\"u}rgen Kerp and Koribalski, {B{\"a}rbel S.} and Thomas Erben and Esra Bulbul and Efrain Gatuzz and Vittorio Ghirardini and Hopkins, {Andrew M.} and Ang Liu and Konstantinos Migkas and Tessa Vernstrom",

year = "2022",

month = may,

day = "1",

doi = "10.1051/0004-6361/202141415",

language = "English",

volume = "661",

}

Veronica, A, Su, Y, Biffi, V, Reiprich, TH, Pacaud, F, Nulsen, PEJ, Kraft, RP, Sanders, JS, Bogdan, A, Kara, M, Dolag, K, Kerp, J, Koribalski, BS, Erben, T, Bulbul, E, Gatuzz, E, Ghirardini, V, Hopkins, AM, Liu, A, Migkas, K & Vernstrom, T 2022, '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', Astronomy and Astrophysics, vol. 661, A46. https://doi.org/10.1051/0004-6361/202141415

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, Jürgen

AU - Koribalski, Bärbel S.

AU - Erben, Thomas

AU - Bulbul, Esra

AU - Gatuzz, Efrain

AU - Ghirardini, Vittorio

AU - Hopkins, Andrew M.

AU - Liu, Ang

AU - Migkas, Konstantinos

AU - Vernstrom, Tessa

PY - 2022/5/1

Y1 - 2022/5/1

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 ÃÂ-R200) 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 (R200). 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 0.2-0.5R500 is kBT500 = 1.99 ± 0.04 keV. We employed the mass-temperature (M -T) scaling relation and obtained a mass estimate of M500 = (7.68 ± 0.43) ÃÂ-1013 M and R500 = (63 6 ± 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 ~R500, 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 ~318 kpc, plausibly the result of ram pressure stripping. Through a two-temperature fit, we identify a cooler component in the Northern Filament with kBT = 0.68- 0.64+ 0.38 keV kBT=0.68 0.64+0.38keV and ne = 1.99-1.24+0.88 ÃÂ-10-5cm-3, ne1.99 1.24+0.88ÃÂ-*10 5cm 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 ÃÂ-R200) 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 (R200). 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 0.2-0.5R500 is kBT500 = 1.99 ± 0.04 keV. We employed the mass-temperature (M -T) scaling relation and obtained a mass estimate of M500 = (7.68 ± 0.43) ÃÂ-1013 M and R500 = (63 6 ± 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 ~R500, 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 ~318 kpc, plausibly the result of ram pressure stripping. Through a two-temperature fit, we identify a cooler component in the Northern Filament with kBT = 0.68- 0.64+ 0.38 keV kBT=0.68 0.64+0.38keV and ne = 1.99-1.24+0.88 ÃÂ-10-5cm-3, ne1.99 1.24+0.88ÃÂ-*10 5cm 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: A3391

KW - Galaxies: clusters: individual: MCXCJ0621.7-5242

KW - Galaxies: clusters: individual: Northern Clump

KW - Galaxies: clusters: intracluster medium

KW - X-rays: galaxies: clusters

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UR - http://www.scopus.com/inward/citedby.url?scp=85130643221&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202141415

DO - 10.1051/0004-6361/202141415

M3 - Article

AN - SCOPUS:85130643221

SN - 0004-6361

VL - 661

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A46

ER -

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

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