The 10k zCOSMOS: Morphological transformation of galaxies in the group environment since z ∼ 1

K. Kovač, S. J. Lilly, C. Knobel, M. Bolzonella, A. Iovino, C. M. Carollo, C. Scarlata, M. Sargent, O. Cucciati, G. Zamorani, L. Pozzetti, L. A.M. Tasca, M. Scodeggio, P. Kampczyk, Y. Peng, P. Oesch, E. Zucca, A. Finoguenov, T. Contini, J. P. KneibO. Le Fèvre, V. Mainieri, A. Renzini, S. Bardelli, A. Bongiorno, K. Caputi, G. Coppa, S. De La Torre, L. De Ravel, P. Franzetti, B. Garilli, F. Lamareille, J. F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello, E. Perez Montero, E. Ricciardelli, J. D. Silverman, M. Tanaka, L. Tresse, D. Vergani, U. Abbas, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, L. Guzzo, A. M. Koekemoer, A. Leauthaud, D. Maccagni, C. Marinoni, H. J. McCracken, P. Memeo, B. Meneux, C. Porciani, R. Scaramella, N. Z. Scoville

研究成果: Article査読

55 被引用数 (Scopus)


We study the evolution of galaxies inside and outside of the group environment since z = 1 using a large well-defined set of groups and galaxies from the zCOSMOS-bright redshift survey in the COSMOS field. The fraction of galaxies with early-type morphologies increases monotonically with MB luminosity and stellar mass and with cosmic epoch. It is higher in the groups than elsewhere, especially at later epochs. The emerging environmental effect is superposed on a strong global mass-driven evolution, and at z ∼ 0.5 and log(M/M) ∼ 10.2, the "effect" of the group environment is equivalent to (only) about 0.2 dex in stellar mass or 2 Gyr in time. The stellar mass function of galaxies in groups is enriched in massive galaxies. We directly determine the transformation rates from late to early morphologies, and for transformations involving color and star formation indicators. The transformation rates are systematically about twice as high in the groups as outside, or up to three to four times higher correcting for infall and the appearance of new groups. The rates reach values as high as 0.3-0.7 Gyr-1 in the groups (for masses around the crossing mass 1010.5 M), implying transformation timescales of 1.4-3 Gyr, compared with less than 0.2 Gyr-1, i.e., timescales >5 Gyr, outside of groups. All three transformation rates decrease at higher stellar masses, and must also decrease at lower masses below 1010 M which we cannot probe well. The rates involving color and star formation are consistently higher than those for morphology, by a factor of about 50%. Our conclusion is that the transformations that drive the evolution of the overall galaxy population since z ∼ 1 must occur at a rate two to four times higher in groups than outside of them.

ジャーナルAstrophysical Journal
出版ステータスPublished - 2010 7 20

ASJC Scopus subject areas

  • 天文学と天体物理学
  • 宇宙惑星科学


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