NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-25 T09:13:33 PDT
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For refcode 2010MNRAS.403.1611K:
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Copyright by Royal Astronomical Society. 2010MNRAS.403.1611K Panoramic H{alpha} and mid-infrared mapping of star formation in a z = 0.8 cluster Koyama, Yusei; Kodama, Tadayuki; Shimasaku, Kazuhiro; Hayashi, Masao; Okamura, Sadanori; Tanaka, Ichi; Tokoku, Chihiro Abstract. ABSTRACT We present the first wide-field H{alpha} imaging survey around the distant cluster RXJ1716.4+6708 at z = 0.81 with a narrow-band filter on MOIRCS/Subaru, which reveals the star formation activities down to a star formation rate (SFR) of ~1M_sun_yr^-1^ without extinction correction. Combining with a wide-field mid-infrared (MIR) imaging survey with the AKARI satellite, we compare in detail the unobscured and obscured star formation activities in the cluster. We find that both H{alpha} emitters and MIR galaxies avoid the cluster central region and their spatial distribution is quite similar. Most of the H{alpha} emitters show blue colours, but we find some H{alpha} emitters on the red sequence. The MIR galaxies tend to be systematically redder than the H{alpha} emitters probably due to heavy dust extinction. Interestingly, the red H{alpha} emitters and the red MIR galaxies (i.e. dusty red galaxies) are most commonly seen in the medium-density environment such as cluster outskirts, groups and filaments, where optical colours of galaxies change. We investigate the amount of hidden star formation by calculating a ratio, SFR(IR)/SFR(H{alpha}), and find that A_H{alpha}_ exceeds ~3 in extreme cases for actively star-forming galaxies with SFR(IR) >~20M_sun_yr^-1^. It is notable that most of such very dusty galaxies with A_H{alpha}_ >~ 3 are also located in the medium-density environment. These findings suggest that dusty star formation is triggered in the infall region of the cluster, implying a probable link between galaxy transition and dusty star formation. We finally calculate the cluster total SFR and find that the cluster total SFR based on H{alpha} alone can be underestimated more than a factor of ~2 even after 1-mag extinction correction. We suggest that the mass-normalized cluster SFR rapidly declines since z ~ 1 following ~ (1 + z)^6^, although the uncertainty is still large. Key words: galaxies: clusters: individual: RXJ1716.4+6708, galaxies: evolution, large-scale structure of Universe
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