A Chandra Study of the Complex Structure in the Core of 2A 0335+096

Details A Chandra Study of the Complex Structure in the Core of 2A 0335+096 A Chandra Study of the Complex Structure in the Core of 2A 0335+096

2003-03-13

arxiv.org/abs/astro-ph/0303314v1

Astrophys.J. 596 (2003) 190-203

Astronomy and Astrophysics

Astrophysics

Submitted for publication in ApJ; 14 pages, 2 color figures and 11 BW figures, emulateapj

Scientific paper

10.1086/377633

We present a Chandra observation of the central (r< 200kpc) region of the cluster of galaxies 2A 0335+096, rich in interesting phenomena. On large scales (r> 40kpc), the X-ray surface brightness is symmetric and slightly elliptical. The cluster has a cool dense core; the radial temperature gradient varies with position angle. The radial metallicity profile shows a pronounced central drop and an off-center peak. Similarly to many clusters with dense cores, 2A 0335+096 hosts a cold front at r\approx 40kpc south of the center. The gas pressure across the front is discontinuous by a factor A_P=1.6\pm 0.3, indicating that the cool core is moving with respect to the ambient gas with a Mach number M\approx 0.75\pm 0.2. The central dense region inside the cold front shows an unusual X-ray morphology, which consists of a number of X-ray blobs and/or filaments on scales \gtrsim 3kpc, along with two prominent X-ray cavities. The X-ray blobs are not correlated with either the optical line emission (H\alpha+[NII]), member galaxies or radio emission. Deprojected temperature of the dense blobs is consistent with that of the less dense ambient gas, so these gas phases do not appear to be in thermal pressure equilibrium. An interesting possibility is a significant, unseen non-thermal pressure component in the inter-blob gas, possibly arising from the activity of the central AGN. We discuss two models for the origin of the gas blobs -- hydrodynamic instabilities caused by the observed motion of the gas core, or ``bubbling'' of the core caused by multiple outbursts of the central AGN.

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