Wide-field chandra X-ray observations of active galactic nuclei in Abell 85 and Abell 754

Gregory R. Sivakoff, Paul Martini, Ann I Zabludoff, Daniel D. Kelson, John S. Mulchaey

Research output: Contribution to journalArticle

24 Citations (Scopus)

Abstract

To better understand the mechanism or mechanisms that lead to AGN activity today, we measure the X-ray AGN fraction in a new sample of nearby clusters and examine how it varies with galaxy properties, projected clustercentric radius, and cluster velocity dispersion. We present new wide-field Chandra X-Ray Observatory observations of Abell 85, Abell 754, and the background cluster Abell 89B out to their virial radii. Out of 17 X-ray sources associated with galaxies in these clusters, we classify 7 as X-ray AGNs with LX,B > 1041 ergs s-1. Only 2 of these would be classified as AGNs based on their optical spectra. We combine these observations with archival data to create a sample of X-ray AGN from 6 z < 0.08 clusters and find that 3.4-0.8+1.1% of MR < -20 galaxies host X-ray AGNs with LX, B > 1041 ergs s_1. We find that more X-ray AGNs are detected in more luminous galaxies and attribute this to larger spheroids in more luminous galaxies and increased sensitivity to lower Eddington-rate accretion from black holes in those spheroids. At a given X-ray luminosity limit, more massive black holes can be accreting less efficiently, yet still be detected. If interactions between galaxies are the principal drivers of AGN activity, then the AGN fraction should be higher in lower velocity dispersion clusters and the outskirts of clusters. However, the tendency of the most massive and early-type galaxies to lie in the centers of the richest clusters could dilute such trends. While we find no variation in the AGN fraction with projected clustercentric radius, we do find that the AGN fraction increases significantly, from 2.6-0.8 +1.0% in rich clusters to 10.0-4.3+6.2% in those with lower velocity dispersions.

Original languageEnglish (US)
Pages (from-to)803-820
Number of pages18
JournalAstrophysical Journal
Volume682
Issue number2
DOIs
StatePublished - Aug 1 2008

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active galactic nuclei
galaxies
x rays
spheroids
erg
low speed
radii
observatory
optical spectrum
accretion
observatories
tendencies
luminosity
trends
sensitivity

Keywords

  • Galaxies: active
  • Galaxies: clusters: general
  • Galaxies: general
  • X-rays: galaxies
  • X-rays: galaxies: clusters
  • X-rays: general

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Wide-field chandra X-ray observations of active galactic nuclei in Abell 85 and Abell 754. / Sivakoff, Gregory R.; Martini, Paul; Zabludoff, Ann I; Kelson, Daniel D.; Mulchaey, John S.

In: Astrophysical Journal, Vol. 682, No. 2, 01.08.2008, p. 803-820.

Research output: Contribution to journalArticle

Sivakoff, Gregory R. ; Martini, Paul ; Zabludoff, Ann I ; Kelson, Daniel D. ; Mulchaey, John S. / Wide-field chandra X-ray observations of active galactic nuclei in Abell 85 and Abell 754. In: Astrophysical Journal. 2008 ; Vol. 682, No. 2. pp. 803-820.
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AB - To better understand the mechanism or mechanisms that lead to AGN activity today, we measure the X-ray AGN fraction in a new sample of nearby clusters and examine how it varies with galaxy properties, projected clustercentric radius, and cluster velocity dispersion. We present new wide-field Chandra X-Ray Observatory observations of Abell 85, Abell 754, and the background cluster Abell 89B out to their virial radii. Out of 17 X-ray sources associated with galaxies in these clusters, we classify 7 as X-ray AGNs with LX,B > 1041 ergs s-1. Only 2 of these would be classified as AGNs based on their optical spectra. We combine these observations with archival data to create a sample of X-ray AGN from 6 z < 0.08 clusters and find that 3.4-0.8+1.1% of MR < -20 galaxies host X-ray AGNs with LX, B > 1041 ergs s_1. We find that more X-ray AGNs are detected in more luminous galaxies and attribute this to larger spheroids in more luminous galaxies and increased sensitivity to lower Eddington-rate accretion from black holes in those spheroids. At a given X-ray luminosity limit, more massive black holes can be accreting less efficiently, yet still be detected. If interactions between galaxies are the principal drivers of AGN activity, then the AGN fraction should be higher in lower velocity dispersion clusters and the outskirts of clusters. However, the tendency of the most massive and early-type galaxies to lie in the centers of the richest clusters could dilute such trends. While we find no variation in the AGN fraction with projected clustercentric radius, we do find that the AGN fraction increases significantly, from 2.6-0.8 +1.0% in rich clusters to 10.0-4.3+6.2% in those with lower velocity dispersions.

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