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)
· arXiv e-print (arXiv:0810.1272)
· On-line Data
· References in the article
· Citations to the Article (7) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (16)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The Enrichment of the Intracluster Medium
Authors:
Sivanandam, Suresh; Zabludoff, Ann I.; Zaritsky, Dennis; Gonzalez, Anthony H.; Kelson, Dan D.
Affiliation:
AA(Steward Observatory, University of Arizona, 933 North Cherry Ave, Tucson, AZ 85721, USA ), AB(Steward Observatory, University of Arizona, 933 North Cherry Ave, Tucson, AZ 85721, USA ), AC(Steward Observatory, University of Arizona, 933 North Cherry Ave, Tucson, AZ 85721, USA ), AD(Department of Astronomy, University of Florida, P.O. Box 112055, 211 Bryant Space Science Center, Gainesville, FL 32611, USA ), AE(The Observatories, Carnegie Institution of Washington, 813 Santa Barbara St, Pasadena, CA 91101, USA )
Publication:
The Astrophysical Journal, Volume 691, Issue 2, pp. 1787-1806 (2009). (ApJ Homepage)
Publication Date:
02/2009
Origin:
IOP
ApJ Keywords:
galaxies: clusters: general, intergalactic medium, supernovae: general, X-rays: galaxies: clusters
DOI:
10.1088/0004-637X/691/2/1787
Bibliographic Code:
2009ApJ...691.1787S

Abstract

To determine the relative contributions of galactic and intracluster stars to the enrichment of the intracluster medium (ICM), we present X-ray surface brightness, temperature, and Fe abundance profiles for a set of 12 galaxy clusters4Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. for which we have extensive optical photometry. Assuming a standard initial mass function and simple chemical evolution model scaled to match the present-day cluster early-type SN Ia rate, the stars in the brightest cluster galaxy (BCG) plus the intracluster stars (ICS) generate 31+11 -9%, on average, of the observed ICM Fe within r 500 (~0.6 times r 200, the virial radius). An alternate, two-component SN Ia model (including both prompt and delayed detonations) produces a similar BCG+ICS contribution of 22+9 -9%. Because the ICS typically contribute 80% of the BCG+ICS Fe, we conclude that the ICS are significant, yet often neglected, contributors to the ICM Fe within r 500. However, the BCG+ICS fall short of producing all the Fe, so metal loss from stars in other cluster galaxies must also contribute. By combining the enrichment from intracluster and galactic stars, we can account for all the observed Fe. These models require a galactic metal-loss fraction (0.84+0.11 -0.14) that, while large, is consistent with the metal mass not retained by galactic stars. The SN Ia rates, especially as a function of galaxy environment and redshift, remain a significant source of uncertainty in further constraining the metal-loss fraction. For example, increasing the SN Ia rate by a factor of 1.8—to just within the 2σ uncertainty for present-day cluster early-type galaxies—allows the combined BCG + ICS + cluster galaxy model to generate all the ICM Fe with a much lower galactic metal-loss fraction (~0.35).
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