NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-25 T22:44:13 PDT
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For refcode 2010A&A...518L..18S:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2010A&A...518L..18S LoCuSS: Probing galaxy transformation physics with Herschel Smith, G. P.; Haines, C. P.; Pereira, M. J.; Egami, E.; Moran, S. M.; Hardegree-Ullman, E.; Babul, A.; Rex, M.; Rawle, T. D.; Zhang, Y.-Y.; Finoguenov, A.; Okabe, N.; Sanderson, A. J. R.; Edge, A. C.; Takada, M. Abstract. We present an early broad-brush analysis of Herschel/PACS observations of star-forming galaxies in 8 galaxy clusters drawn from our survey of 30 clusters at z ~= 0.2. We define a complete sample of 192 spectroscopically confirmed cluster members down to L_TIR_ > 3 x 10^10^ L_o_ and L_K_ > 0.25 L_K^star. The average K-band and bolometric infrared luminosities of these galaxies both fade by a factor of 2 from clustercentric radii of 2 r_200_ to 0.5 r_200_, indicating that as galaxies enter the clusters ongoing star-formation stops first in the most massive galaxies, and that the specific star-formation rate (SSFR) is conserved. On smaller scales the average SSFR jumps by 25%, suggesting that in cluster cores processes including ram pressure stripping may trigger a final episode of star-formation that presumably exhausts the remaining gas. This picture is consistent with our comparison of the Herschel-detected cluster members with the cluster mass distributions, as measured in our previous weak-lensing study of these clusters. For example, the spatial distribution of the Herschel sources is positively correlated with the structures in the weak-lensing mass maps at 5{sigma} significance, with the strongest signal seen at intermediate group-like densities. The strong dependence of the total cluster IR luminosity on cluster mass - L_TIR_ is proportional to M_virial_^2^ - is also consistent with accretion of galaxies and groups of galaxies (i.e. the substructure mass function) driving the cluster IR luminosity. The most surprising result is that roughly half of the Herschel-detected cluster members have redder S_100_/S_24_ flux ratios than expected, based on the Rieke et al. models. On average cluster members are redder than non-members, and the fraction of red galaxies increases towards the cluster centers, both of which indicate that these colors are not attributable to systematic photometric errors. Our future goals include to intepret physically these red galaxies, and to exploit this unique large sample of clusters with unprecedented multi-wavelength observations to measure the cluster-cluster scatter in S0 progenitor populations, and to intepret that scatter in the context of the hierarchical assembly of clusters. Key words: galaxies: clusters: general, galaxies: star formation, Galaxy: evolution, infrared: galaxies
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