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Date and Time of the Query: 2019-05-22 T02:07:10 PDT
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For refcode 2011ApJ...731...93M:
Retrieve 17 NED objects in this reference.
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Copyright by American Astronomical Society. Reproduced by permission
2011ApJ...731...93M Star Clusters in the Tidal Tails of Interacting Galaxies: Cluster Populations Across a Variety of Tail Environments Mullan, B.; Konstantopoulos, I. S.; Kepley, A. A.; Lee, K. H.; Charlton, J. C.; Knierman, K.; Bastian, N.; Chandar, R.; Durrell, P. R.; Elmegreen, D.; English, J.; Gallagher, S. C.; Gronwall, C.; Hibbard, J. E.; Hunsberger, S.; Johnson, K. E.; Maybhate, A.; Palma, C.; Trancho, G.; Vacca, W. D. Abstract. We have searched for compact stellar structures within 17 tidal tails in 13 different interacting galaxies using F606W- and F814W-band images from the Wide Field Planetary Camera 2 on the Hubble Space Telescope. The sample of tidal tails includes a diverse population of optical properties, merging galaxy mass ratios, H I content, and ages. Combining our tail sample with Knierman et al., we find evidence of star clusters formed in situ with M_ V_ < -8.5 and V - I < 2.0 in 10 of 23 tidal tails; we are able to identify cluster candidates to M_ V_ = -6.5 in the closest tails. Three tails offer clear examples of "beads on a string" star formation morphology in V - I color maps. Two tails present both tidal dwarf galaxy candidates and cluster candidates. Statistical diagnostics indicate that clusters in tidal tails may be drawn from the same power-law luminosity functions (with logarithmic slopes ~-2 to -2.5) found in quiescent spiral galaxies and interiors of interacting systems. We find that the tail regions with the largest number of observable clusters are relatively young (<~250 Myr old) and bright (V <~ 24 mag arcsec^-2^), probably attributed to the strong bursts of star formation in interacting systems soon after periapse. Otherwise, we find no statistical difference between cluster-rich and cluster-poor tails in terms of many observable characteristics, though this analysis suffers from complex, unresolved gas dynamics and projection effects. Key words: galaxies: interactions, galaxies: photometry, galaxies: star clusters: general
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