Journal Article

Panoramic Hα and mid-infrared mapping of star formation in a z = 0.8 cluster

Yusei Koyama, Tadayuki Kodama, Kazuhiro Shimasaku, Masao Hayashi, Sadanori Okamura, Ichi Tanaka and Chihiro Tokoku

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 403, issue 3, pages 1611-1624
Published in print April 2010 | ISSN: 0035-8711
Published online April 2010 | e-ISSN: 1365-2966 | DOI:
Panoramic Hα and mid-infrared mapping of star formation in a z = 0.8 cluster

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We present the first wide-field Hα 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 ∼1 M 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 Hα emitters and MIR galaxies avoid the cluster central region and their spatial distribution is quite similar. Most of the Hα emitters show blue colours, but we find some Hα emitters on the red sequence. The MIR galaxies tend to be systematically redder than the Hα emitters probably due to heavy dust extinction. Interestingly, the red Hα 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(Hα), and find that A exceeds ∼3 in extreme cases for actively star-forming galaxies with SFR(IR) ≳20 M yr−1. It is notable that most of such very dusty galaxies with A≳ 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 Hα 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.

Keywords: galaxies: clusters: individual: RXJ1716.4+6708; galaxies: evolution; large-scale structure of Universe

Journal Article.  11277 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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