AAS 205th Meeting, 9-13 January 2005
Session 147 Groups and Clusters of Galaxies
Poster, Thursday, January 13, 2005, 9:20am-4:00pm, Exhibit Hall

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[147.08] Nebular Emission in X-ray Selected Brightest Cluster Galaxies

R. Samuele, B.R. McNamara (Ohio U.), C.R. Mullis (U. Michigan), A. Vikhlinin, W. Forman (CfA), I.M. Gioia (Institutio di Radioastronomia del CNR, Italy), J.P. Henry (U. Hawaii), A. Hornstrup (DSRI), C. Jones (CfA), H. Quintana (U. Catolica de Chile)

Optical spectra of brightest cluster galaxies selected from the 160 Square Degree ROSAT cluster survey (Vikhlinin et al. 1999) are used to measure the equivalent widths of \rm\,[OII]\lambda3727\, and \rm\,H\alpha\, nebular emission lines. This line emission is used to trace warm ionized gas in the interstellar media of 77 brightest cluster galaxies. Their redshifts lie between z=0.066-0.7, while their X-ray luminosities range between \rm LX =0.04-4.27\times1044\,erg\,s-1\,[0.5-2\,keV]. We find no \rm\,[OII]\lambda 3727\, or \rm\,H\alpha\, emission stronger than -15\,Å\, or -5\,Å\, respectively. A comparison between our sample and the frequency of brightest cluster galaxies with strong line emission from the Brightest Cluster Survey (Crawford et al. 1999) suggests that we could have detected nearly a dozen emission-line galaxies. We discuss several interpretations of this apparent dearth of emission line galaxies detected in our survey.

The author(s) of this abstract have provided an email address for comments about the abstract: samuele@helios.phy.ohiou.edu

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© 2004. The American Astronomical Society.