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/0311502)
· On-line Data
· References in the article
· Citations to the Article (85) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (6)
· NED Objects (10)
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
Mapping small-scale temperature and abundance structures in the core of the Perseus cluster
Authors:
Sanders, J. S.; Fabian, A. C.; Allen, S. W.; Schmidt, R. W.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AC(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AD(Institut für Physik, Universität Potsdam, Am neuen Palais 10, D-14469 Potsdam, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 349, Issue 3, pp. 952-972. (MNRAS Homepage)
Publication Date:
04/2004
Origin:
MNRAS
MNRAS Keywords:
galaxies: clusters: individual: Perseus, cooling flows, intergalactic medium, X-rays: galaxies: clusters
DOI:
10.1111/j.1365-2966.2004.07576.x
Bibliographic Code:
2004MNRAS.349..952S

Abstract

We report further results from a 191-ks Chandra observation of the core of the Perseus cluster, Abell 426. The emission-weighted temperature and abundance structures are mapped in detail. There are temperature variations down to ~1 kpc in the brightest regions. Globally, the strongest X-ray surface brightness features appear to be caused by temperature changes. Density and temperature changes conspire to give approximate azimuthal balance in pressure showing that the gas is in hydrostatic equilibrium. Si, S, Ar, Ca, Fe and Ni abundance profiles rise inwards from about 100 kpc, peaking at about 30-40 kpc. Most of these abundances drop inwards of the peak, but Ne shows a central peak, all of which may be explained by resonance scattering. There is no evidence for a widespread additional cooler temperature component in the cluster with a temperature greater than a factor of 2 from the local temperature. There is, however, evidence for a widespread hard component which may be non-thermal. The temperature and abundance of gas in the cluster are observed to be correlated in a manner similar to that found between clusters.

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