Riding the wake of a merging galaxy cluster
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Riding the wake of a merging galaxy cluster. / Canning, R. E. A.; Russell, H. R.; Hatch, N. A.; Fabian, A. C.; Zabludoff, A. I.; Crawford, C. S.; King, L. J.; McNamara, B. R.; Okamoto, S.; Raimundo, S. I.
In: Monthly Notices of the Royal Astronomical Society, Vol. 420, No. 4, 01.03.2012, p. 2956-2968.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - Riding the wake of a merging galaxy cluster
AU - Canning, R. E. A.
AU - Russell, H. R.
AU - Hatch, N. A.
AU - Fabian, A. C.
AU - Zabludoff, A. I.
AU - Crawford, C. S.
AU - King, L. J.
AU - McNamara, B. R.
AU - Okamoto, S.
AU - Raimundo, S. I.
PY - 2012/3/1
Y1 - 2012/3/1
N2 - Using William Herschel Telescope (WHT) Optically Adaptive System for Imaging Spectroscopy (OASIS) integral field unit observations, we report the discovery of a thin plume of ionized gas extending from the brightest cluster galaxy (BCG) in Abell 2146 to the subcluster X-ray cool core which is offset from the BCG by ˜37 kpc. The plume is greater than 15 kpc long and less than 3 kpc wide. This plume is unique in that the cluster it is situated in is currently undergoing a major galaxy cluster merger. The BCG is unusually located behind the X-ray shock front and in the wake of the ram-pressure-stripped X-ray cool core, and evidence for recent disruption to the BCG is observed. We examine the gas and stellar morphology, the gas kinematics of the BCG and their relation to the X-ray gas. We propose that a causal link between the ionized gas plume and the offset X-ray cool core provides the simplest explanation for the formation of the plume. An interaction or merger between the BCG and another cluster galaxy is probably the cause of the offset.
AB - Using William Herschel Telescope (WHT) Optically Adaptive System for Imaging Spectroscopy (OASIS) integral field unit observations, we report the discovery of a thin plume of ionized gas extending from the brightest cluster galaxy (BCG) in Abell 2146 to the subcluster X-ray cool core which is offset from the BCG by ˜37 kpc. The plume is greater than 15 kpc long and less than 3 kpc wide. This plume is unique in that the cluster it is situated in is currently undergoing a major galaxy cluster merger. The BCG is unusually located behind the X-ray shock front and in the wake of the ram-pressure-stripped X-ray cool core, and evidence for recent disruption to the BCG is observed. We examine the gas and stellar morphology, the gas kinematics of the BCG and their relation to the X-ray gas. We propose that a causal link between the ionized gas plume and the offset X-ray cool core provides the simplest explanation for the formation of the plume. An interaction or merger between the BCG and another cluster galaxy is probably the cause of the offset.
KW - ISM: kinematics and dynamics
KW - galaxies: clusters: individual: Abell 2146
KW - galaxies: clusters: intracluster medium
KW - galaxies: kinematics and dynamics
U2 - 10.1111/j.1365-2966.2011.20116.x
DO - 10.1111/j.1365-2966.2011.20116.x
M3 - Journal article
VL - 420
SP - 2956
EP - 2968
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 4
ER -
ID: 230475661