2019
DOI: 10.3847/1538-4357/ab4808
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A BCG with Offset Cooling: Is the AGN Feedback Cycle Broken in A2495?

Abstract: We present a combined radio/X-ray analysis of the poorly studied galaxy cluster Abell 2495 (z=0.07923) based on new EVLA and Chandra data. We also analyze and discuss Hα emission and optical continuum data retrieved from the literature. We find an offset of ∼ 6 kpc between the cluster BCG (MCG+02-58-021) and the peak of the X-ray emission, suggesting that the cooling process is not taking place on the central galaxy nucleus. We propose that sloshing of the ICM could be responsible for this separation. Furtherm… Show more

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Cited by 19 publications
(38 citation statements)
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“…This observed variability has been corroborated by numerical simulations (e.g., Li et al 2015;Prasad et al 2015), providing an explanation for the lobe structure in the Phoenix cluster. It is possible that the sloshing in the ICM contributes in part to this AGN variability by displacing the accretion material of the AGN, similar to as observed in A2495 by Pasini et al (2019). However, whereas the BCG in A2495 appears to be oscillating back and forth through the cool core, the BCG in the Phoenix cluster is stationary at the center of the cool core.…”
Section: The Extreme Feedback In the Phoenix Clustermentioning
confidence: 81%
“…This observed variability has been corroborated by numerical simulations (e.g., Li et al 2015;Prasad et al 2015), providing an explanation for the lobe structure in the Phoenix cluster. It is possible that the sloshing in the ICM contributes in part to this AGN variability by displacing the accretion material of the AGN, similar to as observed in A2495 by Pasini et al (2019). However, whereas the BCG in A2495 appears to be oscillating back and forth through the cool core, the BCG in the Phoenix cluster is stationary at the center of the cool core.…”
Section: The Extreme Feedback In the Phoenix Clustermentioning
confidence: 81%
“…Indeed, the observed offset between the BCG and the peak H α emission was at most ≈10kpc versus ≈25 kpc in SpARCS1049. The authors argued that such displacements may be caused by a large event such as a major merger (see also Pasini et al 2019 andVantyghem et al 2019). Nonetheless, it is important to remember that SpARCS1049 is located at the epoch in which the most massive structures (such as SpARCS1049) are still forming and have not yet settled into equilibrium.…”
Section: A Cool Core Offset From Its Central Galaxymentioning
confidence: 99%
“…Small offsets (<50 kpc) are expected and found in most relaxed clusters since even a minor merger can induce sloshing and displace the X-ray emission peak from the BCG (e.g., Hamer et al 2016;Pasini et al 2019;Ubertosi et al 2021;Pasini et al 2021b). Large offsets (100-1000 kpc) are often an indication of a strongly disturbed cluster environment (Rossetti et al 2016;De Propris et al 2021, and references therein).…”
Section: Bcg Offsetsmentioning
confidence: 98%