Volume 553, May 2013
|Number of page(s)||15|
|Published online||15 May 2013|
III. Nurture builds up the Hubble sequence in the Great Wall
1 Università degli Studi di Milano-Bicocca Piazza della Scienza 3 20126 Milano Italy
2 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, 3122 Victoria, Australia
3 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany
4 Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA
5 Department of Astrophysics, Princeton University, Princeton, NJ 08544-1001, USA
6 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
7 Instituto de Astronomía, Universidad Nacional Autónoma de México, Carretera Tijuana-Ensenada, km 103, 22860 Ensenada, B.C., Mexico
8 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 México D.F., Mexico
9 Center for Radiophysics and Space Research, Space Science Building, Ithaca, NY, 14853, USA
e-mail: email@example.com; firstname.lastname@example.org
Received: 14 December 2012
Accepted: 10 March 2013
Context. We present the analysis of Hα3, an Hα narrow-band imaging follow-up survey of galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Coma supercluster.
Aims. Taking advantage of Hα3, which provides the complete census of the recent star formation in HI-rich galaxies in the local universe, we explored the hypothesis that a morphological sequence of galaxies of progressively earlier type and lower gas-content exists in the neighborhood of a rich cluster of galaxies such as Coma, with a specific star formation activity that decreases with increasing local galaxy density and velocity dispersion.
Methods. By using the Hα hydrogen recombination line as a tracer of the “instantaneous” star formation, complemented with optical colors from SDSS, we investigated the relationships between atomic neutral gas and newly formed stars in different local galaxy density intervals, for many morphological types, and over a wide range of stellar masses (109 to 1011.5 M⊙).
Results. In the dwarf regime (8.5 < log (M∗/M⊙) < 9.5) we identify a four-step sequence of galaxies with progressively redder colors (corrected for dust extinction), i.e., of decreasing specific star formation, from (1) HI-rich late-type galaxies (LTGs) belonging to the blue cloud that exhibit extended plus nuclear star formation, (2) ~0.1 mag redder, HI-poor LTGs with nuclear star formation only, (3) ~0.35 mag redder, HI-poor galaxies without either extended or nuclear star formation, but with nuclear post-star-burst (PSB) signature, (4) ~ 0.5 mag redder early-type galaxies (ETGs) that belong to the red sequence, and show no gas or star formation on all scales. Along this sequence the quenching of the star formation proceeds radially outside-in. The progression toward redder colors found along this “morphological” (gas content) sequence is comparable to the one obtained from increasing the local galaxy density, from cosmic filaments (1 2), to the rich clusters (2 3 4).
Conclusions. In the dwarf regime we find evidence for an evolution of HI-rich LTGs into ETGs through HI-poor LTGs and PSB galaxies driven by the environment. We identify ram-pressure as the mechanism most likely responsible for this transformation. We conclude that infall of galaxies has proceeded for the last 7.5 Gyr, building up the Coma cluster at a rate of approximately 100 galaxies with log (M∗/M⊙) > 9.0 per Gyr.
Key words: galaxies: clusters: individual: Coma / galaxies: fundamental parameters / galaxies: ISM
Based on observations taken at the observatory of San Pedro Martir (Baja California, Mexico), belonging to the Mexican Observatorio Astronómico Nacional.
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2013
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