Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996rftu.proc..587h&link_type=abstract
International Conference on X-ray Astronomy and Astrophysics: Röntgenstrahlung from the Universe, p. 587 - 588
Astronomy and Astrophysics
Astrophysics
Clusters Of Galaxies: Cooling Flows, Clusters Of Galaxies: Morphology, Clusters Of Galaxies: X Rays, Clusters Of Galaxies: Galaxy Distribution
Scientific paper
The cores of subclusters at z ≅ 0.1 are well suited to imaging with the ROSAT HRI. Analysis of a 26 ks observation of Abell 2384, a BM II-III with a cD galaxy, shows an interesting morphology. The cluster appears to be composed of a primary subcluster with a secondary peak which is probably due to a small subcluster, 0.8 Mpc away. The galaxy distribution suggests a secondary peak at the approximate location of the secondary X-ray peak confirming the bimodal morphology. It is particularily interesting because the primary and secondary peak are connected, with the X-ray emission elongated in the direction of the merger axis. This is indicative of an early, pre-merger stage. Resolution of the core of the primary cluster, not resolved in the Einstein IPC data, allows setting limits on the amount of gas in a possible cooling flow. The central particle density is quite high, 0.01 cm-3, but falls rapidly with radius so that the estimated accretion rate is 4 Msunyr-1. Based on the pre-merger morphology and low accretion rate, it is concluded that cooling flows must grow appreciably after a merger to equal the large accretion rates typical of rich clusters.
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