The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star formation in cluster infall

By Christian Wolf, A. Aragón-Salamanca, M. Balogh, M. Barden, Eric F. Bell, M. Gray, C. Peng, D. Bacon, F. Barazza, A. Boehm and 15 more. 2008

164 citations recorded by the source corpus.

We investigate the properties of optically passive spirals and dusty red galaxies in the A901/2 cluster complex at redshift ∼0.17 using rest-frame near-ultraviolet–optical spectral energy distributions, 24-μm infrared data and Hubble Space Telescope morphologies from the STAGES data set. The cluster sample is based on COMBO-17 redshifts with an rms precision of σcz ≈ 2000 km s −1 . We find that ‘dusty red galaxies’ and ‘optically passive spirals’ in A901/2 are largely the same phenomenon, and that they form stars at a substantial rate, which is only four times lower than that in blue spirals at fixed mass. This star formation is more obscured than in blue galaxies and its optical signatures are weak. They appear predominantly in the stellar mass range of log M∗/M� = [10, 11] where they constitute over half of the star-forming galaxies in the cluster; they are thus a vital ingredient for understanding the overall picture of star formation quenching in clusters. We find that the mean specific star formation rate (SFR) of star-forming galaxies in the cluster is clearly lower than in the field, in contrast to the specific SFR properties of blue galaxies alone, which appear similar in cluster and field. Such a rich red spiral population is best explained if quenching is a slow process and morphological transformation is delayed even more. At log M∗/M� < 10, such galaxies are rare, suggesting that their quenching is fast and accompanied by morphological change. We note that edge-on

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d97294c7bc37262cf6bfed3f26f54b14fd178ff9

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In Astronomy and Astrophysics

1. M. Cappellari
2. P. Hopkins
3. L. Hernquist
4. C. Conroy
5. P. V. van Dokkum
6. R. Somerville
7. R. Dav'e
8. A. Dekel

In Instrumentation

1. M. Cappellari
2. P. V. van Dokkum
3. P. Hopkins
4. C. Conroy
5. L. Hernquist
6. M. Franx
7. R. Dav'e
8. A. Dekel

Citations in the corpus

• THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, background): “A number of KINGFISH galaxies appear to be similar to ‘passive disks’ and ‘red spirals’22 recently studied by other authors (e.g., Wolf et al. 2009; Skibba et al. 2009; van der Wel et al. 2009; Masters et al. 2010b; Bundy et al. 2010).”
• MegaMorph - multiwavelength measurement of galaxy structure: complete Sersic profile information from modern surveys (2012, background): “• Even using perfect classifications, one would always find both blue ellipticals in the blue cloud and disks that show red colours given their dust properties and possibly seen edge-on ( .g. Rowlands et al. 2012; Wolf et al. 2009).”
• A DOZEN NEW GALAXIES CAUGHT IN THE ACT: GAS STRIPPING AND EXTENDED EMISSION LINE REGIONS IN THE COMA CLUSTER (2010, result): “…the dependency of the star formation quench on the mass was similar to those in previous studies (Kauffmann et al. 2004; Haines et al. 2007; Wolf et al. 2009; Mahajan, Haines, Raychaudhury 2010), although this is the first time that galaxies of low mass (< 109 M ) have been investigated in…”
• Measures of Galaxy Environment I - What is "Environment"? (2011, background): “Work focused on galaxy clusters have also yielded complementary results (e.g. Poggianti et al. 2008; Bamford et al. 2009; Gallazzi et al. 2009; Rudnick et al. 2009; Wolf et al. 2009).”
• Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample (2009, background): “…or with cluster haloes at large distances from the cor, the gas cannot be accreted anymore and the galaxy will exhaust the remaining cold gas through the star formation, in a timescal which can be instantaneous or slow, i.e., in few Gyr, depending also on the mass of the galaxy (Wolf et al. 2009).”
• The environmental history of group and cluster galaxies in a Λ cold dark matter universe (2011, result): “This is in agreement with what discussed about Figure 10, and in contrast with results from Wolf et al. (2009).”
• On the evolution and environmental dependence of the star formation rate versus stellar mass relation since z ∼ 2 (2013, background): “A prominent example aredusty red galaxies, which are reported to populate the outskirts of rich galaxy clusters out to z ∼ 1 (e.g. Koyama et al. 2008; 2010; see also Wolf, Gray, & Meisenheimer 2005; Geach et al. 2006; Verdugo, Ziegler, & Gerken 2008; Wolf et al. 2009; Tran et al. 2009).”
• The accretion of galaxies into groups and clusters (2009, background): “Additionally, Wolf et al. (2009) find that massive galaxies are uniformly old and red in the cluster cores, while having a significant population of dusty, star-forming red galaxies in the infall regions.”
• THE DEAD SEQUENCE: A CLEAR BIMODALITY IN GALAXY COLORS FROM z = 0 to z = 2.5 (2009, background): “The bottom panel of Figure 3 shows that a red galaxy selection based on a single rest-frame color will contain a significant fraction of dusty-starburst galaxies (∼20% with AV > 1) that would otherwise be much bluer (see also Cimatti et al. 2002; Brammer & van Dokkum 2007; W07; Gallazzi et al. 2009;”
• The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, background): “Theexistence of these intermediate spiral systems, recently named“red spirals”, is now being clearly recognized in large galaxy surveys using multi-colour CCD imaging (Goto et al. 2003; Moran et al. 2006; Wolf et al. 2009; Masters et al. 2010).”
• Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “The decreased quenching with D also agrees with several other studies of SFR or the blue/red fractions within groups and clusters (Gómez et al. 2003; Balogh et al. 2004; Tanaka et al. 2004; Rines et al. 2005; Haines et al. 2007; Wolf et al. 2009; von der Linden et al. 2010).”
• Galaxy Zoo: Passive Red Spirals . (2009, methodology): “As also discovered by Wolf et al. (2009), red (or passive) spirals are an insignificant fraction of the total spiral population at stellar masses below ∼ 1010 M⊙ (although note that Bamford et al. 2009 shows that in the densest regions the few remaining low mass spirals are mostly red) but are a…”