Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19916110b&link_type=abstract
American Astronomical Society, 199th AAS Meeting, #161.10; Bulletin of the American Astronomical Society, Vol. 34, p.573
Other
Scientific paper
Recent Chandra observations of cooling flow clusters containing central radio sources reveal an anti-correlation between radio and X-ray emission. Abell 2052 is a dramatic example of a cluster that exhibits this morphology. The cD galaxy at the center of Abell 2052 is host to the powerful radio source 3C 317. "Holes" in the X-ray emission are coincident with the radio lobes which are surrounded by bright "shells" of X-ray emission. Heating by central radio sources has been proposed as one solution to the "missing gas" in cooling flows -- there is a lack of gas detected in the X-ray at temperatures below approximately 1-2 keV. However, the gas surrounding the radio source in Abell 2052 is cool, with no evidence of heating from the radio source. The data are consistent with the radio source displacing and compressing, and at the same time being confined by, the X-ray gas. The compression of the X-ray shells appears to have been relatively gentle and, at most, slightly transonic. The pressure in the X-ray gas (the shells and surrounding cooler gas) is approximately an order of magnitude higher than the minimum pressure derived for the radio source, suggesting that an additional source of pressure is needed to support the radio plasma. The compression of the X-ray shells has speeded up the cooling of the shells, and optical emission line filaments are found coincident with the brightest regions of the shells. From spectral fitting, we find an abundance gradient that increases from the outer parts of the cluster inward and then drops again within the central 40 kpc. This profile is consistent with what is expected from an inhomogeneous (on 1 kpc scales) abundance distribution, composed of clumps of high-metallicity gas surrounded by very low-metallicity gas. Inhomogeneous abundances are another possible explanation for the lack of 1-2 keV gas detected in cooling flow clusters. In addition to Abell 2052, we will present initial results from a recent Chandra observation of a similar system, Abell 262.
Blanton Elizabeth L.
McNamara Brian R.
Sarazin Craig L.
Wise Michael Wayne
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