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Date and Time of the Query: 2019-04-18 T04:44:24 PDT
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For refcode 2005ApJ...621..651H:
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Copyright by American Astronomical Society. Reproduced by permission
2005ApJ...621..651H The Transformation of Cluster Galaxies at Intermediate Redshift N. L. Homeier, R. Demarco, P. Rosati, M. Postman, J. P. Blakeslee, R. J. Bouwens, L. D. Bradley, H. C. Ford, T. Goto, C. Gronwall, B. Holden, M. J. Jee, A. R. Martel, S. Mei, F. Menanteau, A. Zirm, M. Clampin, G. F. Hartig, G. D. Illingworth, D. R. Ardila, F. Bartko, N. Benitez, T. J. Broadhurst, R. A. Brown, C. J. Burrows, E. S. Cheng, N. J. G. Cross, P. D. Feldman, M. Franx, D. A. Golimowski, L. Infante, R. A. Kimble, J. E. Krist, M. P. Lesser, G. R. Meurer, G. K. Miley, V. Motta, M. Sirianni, W. B. Sparks, H. D. Tran, Z. I. Tsvetanov, R. L. White, and W. Zheng Abstract. We combine imaging data from the Advanced Camera for Surveys (ACS) with VLT/FORS optical spectroscopy to study the properties of star-forming galaxies in the z=0.837 cluster Cl 0152-1357. We have morphological information for 24 star-forming cluster galaxies, which range in morphology from late-type and irregular to compact early-type galaxies. We find that while most star-forming galaxies have r_625_-i_775_ colors bluer than 1.0, eight are in the red cluster sequence. Among the star-forming cluster population, we find five compact early-type galaxies that have properties consistent with their identification as progenitors of dwarf elliptical galaxies. The spatial distribution of the star-forming cluster members is nonuniform. We find none within R~500 Mpc of the cluster center, which is highly suggestive of an intracluster medium interaction. We derive star formation rates from [O II] {lambda}3727 line fluxes and use these to compare the global star formation rate of Cl 0152-1357 to other clusters at low and intermediate redshifts. We find a tentative correlation between integrated star formation rates and T_X_, in the sense that hotter clusters have lower integrated star formation rates. Additional data from clusters with low X-ray temperatures are needed to confirm this trend. We do not find a significant correlation with redshift, suggesting that evolution is either weak or absent between z=0.2 and 0.8. Keywords: Galaxies: Clusters: General, Galaxies: Clusters: Individual: Cl 0152-1357, Galaxies: Evolution, Galaxies: High-Redshift, Galaxies: Interactions
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