Star formation in the outer filaments of NGC 1275

Type Journal Article
Names R. E. A. Canning, A. C. Fabian, R. M. Johnstone, J. S. Sanders, C. J. Conselice, C. S. Crawford, J. S. Gallagher, E. Zweibel
Publication Monthly Notices of the Royal Astronomical Society
Volume 405
Issue 1
Pages 115-128
Date June 1, 2010
Library Catalog NASA ADS
Abstract We present photometry of the outer star clusters in NGC 1275, the brightest galaxy in the Perseus cluster. The observations were taken using the Hubble Space Telescope Advanced Camera for Surveys. We focus on two stellar regions in the south and south-east, far from the nucleus of the low-velocity system (~22kpc). These regions of extended star formation trace the Hα filaments, drawn out by rising radio bubbles. In both regions, bimodal distributions of colour (B - R)0 against magnitude are apparent, suggesting two populations of star clusters with different ages; most of the Hα filaments show no detectable star formation. The younger, bluer population is found to be concentrated along the filaments while the older population is dispersed evenly about the galaxy. We construct colour-magnitude diagrams and derive ages of at most 108years for the younger population, a factor of 10 younger than the young population of star clusters in the inner regions of NGC 1275. We conclude that a formation mechanism or event different to that for the young inner population is needed to explain the outer star clusters and suggest that formation from the filaments, triggered by a buoyant radio bubble rising either above or below these filaments, is the most likely mechanism.
Tags cooling flows, galaxies: clusters: individual: Perseus, galaxies: individual: NGC 1275, galaxies: star clusters
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