Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/0510476)
· On-line Data
· References in the article
· Citations to the Article (163) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (3)
· NED Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction
Authors:
Fabian, A. C.; Sanders, J. S.; Taylor, G. B.; Allen, S. W.; Crawford, C. S.; Johnstone, R. M.; Iwasawa, K.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4060, USA; National Radio Astronomy Observatory, Socorro, NM 87801, USA; University of New Mexico, Department of Physics & Astronomy, Albuquerque, NM 87131, USA), AD(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA; Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4060, USA), AE(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AF(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AG(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 366, Issue 2, pp. 417-428. (MNRAS Homepage)
Publication Date:
02/2006
Origin:
MNRAS
MNRAS Keywords:
galaxies: clusters: individual: Perseus, intergalactic medium, X-rays: galaxies
DOI:
10.1111/j.1365-2966.2005.09896.x
Bibliographic Code:
2006MNRAS.366..417F

Abstract

We present the first results from a very deep Chandra X-ray observation of the core of the Perseus cluster of galaxies. A pressure map reveals a clear thick band of high pressure around the inner radio bubbles. The gas in the band must be expanding outwards and the sharp front to it is identified as a shock front, yet we see no temperature jump across it; indeed, there is more soft emission behind the shock than in front of it. We conclude that in this inner region either thermal conduction operates efficiently or the co-existing relativistic plasma seen as the radio mini-halo is mediating the shock. If common, isothermal shocks in cluster cores mean that we cannot diagnose the expansion speed of radio bubbles from temperature measurements alone. They can at times expand more rapidly than currently assumed without producing significant regions of hot gas. Bubbles may also be significantly more energetic. The pressure ripples found in earlier images are identified as isothermal sound waves. A simple estimate based on their amplitude confirms that they can be an effective distributed heat source able to balance radiative cooling. We see multiphase gas with about 109Msolar at a temperature of about 0.5 keV. Much, but not all, of this X-ray emitting cooler gas is spatially associated with the optical filamentary nebula around the central galaxy, NGC1275. A residual cooling flow of about 50Msolaryr-1 may be taking place. A channel is found in the pressure map along the path of the bubbles, with indications found of outer bubbles. The channel connects in the south (S) with a curious cold front.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints