Chandra Observations of the AS0295 Cluster

Aurelia Pascut, John P. Hughes

Research output: Contribution to journalArticle

Abstract

We present deep (205 ks) Chandra ,Fobservations of the AS0295 binary merging cluster (z ,F= ,F0.30). In the X-ray image, the secondary component is clearly visible as a surface brightness peak, while the primary cluster has a flatter distribution. We found cool gas (∼6 keV) associated with the secondary, while the central temperature of the primary does not deviate significantly from the mean temperature of the cluster of ∼9.5 keV. In the vicinity of the primary's core we found the hottest region in the cluster accompanied by a surface brightness discontinuity. We propose that this region corresponds to a shock, for which we estimate a Mach number of . We found other merger signatures such as a plume of cool gas emerging from the primary cluster and a cold front and a possible bow shock (Mach number of ) leading the secondary cluster. Based on the observed properties in comparison to binary merger simulations from the literature we propose for AS0295 a low-mass ratio, off-axis merging scenario, with the secondary close to the first apocenter. Comparison of our results with strong-lensing observations of AS0295 from Cibirka et al. shows an offset between the total mass peak and the bulk of the gas distribution in the primary cluster. The properties of the merger and the existence of the offset between mass peak and gas make AS0295 a promising candidate for the study of mergers involving non-cool core clusters and the nature of dark matter.

Original languageEnglish (US)
Article number71
JournalAstrophysical Journal
Volume874
Issue number1
DOIs
StatePublished - Mar 20 2019

Fingerprint

merger
gas
cold front
gases
Mach number
discontinuity
brightness
plume
temperature
shock
cold fronts
bows
mass ratios
plumes
simulation
emerging
dark matter
signatures
distribution
comparison

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • X-rays: galaxies: clusters
  • galaxies: clusters: individual (AS0295)

Cite this

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title = "Chandra Observations of the AS0295 Cluster",
abstract = "We present deep (205 ks) Chandra ,Fobservations of the AS0295 binary merging cluster (z ,F= ,F0.30). In the X-ray image, the secondary component is clearly visible as a surface brightness peak, while the primary cluster has a flatter distribution. We found cool gas (∼6 keV) associated with the secondary, while the central temperature of the primary does not deviate significantly from the mean temperature of the cluster of ∼9.5 keV. In the vicinity of the primary's core we found the hottest region in the cluster accompanied by a surface brightness discontinuity. We propose that this region corresponds to a shock, for which we estimate a Mach number of . We found other merger signatures such as a plume of cool gas emerging from the primary cluster and a cold front and a possible bow shock (Mach number of ) leading the secondary cluster. Based on the observed properties in comparison to binary merger simulations from the literature we propose for AS0295 a low-mass ratio, off-axis merging scenario, with the secondary close to the first apocenter. Comparison of our results with strong-lensing observations of AS0295 from Cibirka et al. shows an offset between the total mass peak and the bulk of the gas distribution in the primary cluster. The properties of the merger and the existence of the offset between mass peak and gas make AS0295 a promising candidate for the study of mergers involving non-cool core clusters and the nature of dark matter.",
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Chandra Observations of the AS0295 Cluster. / Pascut, Aurelia; Hughes, John P.

In: Astrophysical Journal, Vol. 874, No. 1, 71, 20.03.2019.

Research output: Contribution to journalArticle

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AU - Hughes, John P.

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AB - We present deep (205 ks) Chandra ,Fobservations of the AS0295 binary merging cluster (z ,F= ,F0.30). In the X-ray image, the secondary component is clearly visible as a surface brightness peak, while the primary cluster has a flatter distribution. We found cool gas (∼6 keV) associated with the secondary, while the central temperature of the primary does not deviate significantly from the mean temperature of the cluster of ∼9.5 keV. In the vicinity of the primary's core we found the hottest region in the cluster accompanied by a surface brightness discontinuity. We propose that this region corresponds to a shock, for which we estimate a Mach number of . We found other merger signatures such as a plume of cool gas emerging from the primary cluster and a cold front and a possible bow shock (Mach number of ) leading the secondary cluster. Based on the observed properties in comparison to binary merger simulations from the literature we propose for AS0295 a low-mass ratio, off-axis merging scenario, with the secondary close to the first apocenter. Comparison of our results with strong-lensing observations of AS0295 from Cibirka et al. shows an offset between the total mass peak and the bulk of the gas distribution in the primary cluster. The properties of the merger and the existence of the offset between mass peak and gas make AS0295 a promising candidate for the study of mergers involving non-cool core clusters and the nature of dark matter.

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