Star Formation Rates in Cooling Flow Clusters: A UV Pilot Study with Archival XMM-Newton Optical Monitor Data

Details Star Formation Rates in Cooling Flow Clusters: A UV Pilot Study with Archival XMM-Newton Optical Monitor Data Star Formation Rates in Cooling Flow Clusters: A UV Pilot Study with Archival XMM-Newton Optical Monitor Data

2005-08-04

arxiv.org/abs/astro-ph/0508143v1

Astrophys.J.635:L9-L12,2005

Astronomy and Astrophysics

Astrophysics

16 pages, 5 figures. A slightly shorter version has been accepted for publication in Astrophysical Journal Letters

Scientific paper

10.1086/499123

We have analyzed XMM-Newton Optical Monitor (OM) UV (180-400 nm) data for a sample of 33 galaxies, of which 30 are cluster members. Nine of these are central cluster galaxies (CCGs) in cooling flow clusters, having mass deposition rates which span a range of 8 to 525 solar masses per year. Using the ratio of UV to 2MASS J band flux, we find a significant UV excess in many, but not all, cooling flow CCGs. This UV excess is a direct indication of the presence of young massive stars, and therefore recent star formation, in these galaxies. Using the Starburst99 spectral energy distribution (SED) model of continuous star formation over a 900 Myr period, we derive star formation rates of 0.2 to 219 solar masses per year for the cooling flow sample. For 2/3 of this sample it is possible to equate Chandra/XMM cooling flow mass deposition rates with UV inferred star formation rates, for a combination of starburst lifetime and IMF slope. This is a pilot study of the well populated XMM UV cluster archive and a more extensive follow up study is currently underway.

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