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Environmental dependence of 8 μm luminosity functions of galaxies at z ~ 0.8: Comparison between RXJ1716.4+6708 and the AKARI NEP-deep field

Goto, T. and Koyama, Y. and Wada, T. and Pearson, C. and Matsuhara, H. and Tagaki, T. and Shim, H. and Im, M. and Lee, M. G. and Inami, H. and Malkan, M. and Okamura, S. and Takeuchi, T. T. and Serjeant, S. and Kodama, T. and Nakagawa, T. and Oyabu, S. and Ohyama, Y. and Lee, H. M. and Hwang, N. and Hanami, H. and Imai, K. and Ishigaki, T. (2010) Environmental dependence of 8 μm luminosity functions of galaxies at z ~ 0.8: Comparison between RXJ1716.4+6708 and the AKARI NEP-deep field. Astronomy and Astrophysics, 514 . Art. No. A7. ISSN 0004-6361.

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Aims. We aim to reveal environmental dependence of infrared luminosity functions (IR LFs) of galaxies at z ~ 0.8 using the AKARI satellite. AKARI’s wide field of view and unique mid-IR filters help us to construct restframe 8 μm LFs directly without relying on SED models. Methods. We construct restframe 8 μm IR LFs in the cluster region RXJ1716.4+6708 at z = 0.81, and compare them with a blank field using the AKARI north ecliptic pole deep field data at the same redshift. AKARI’s wide field of view (10' × 10') is suitable to investigate wide range of galaxy environments. AKARI’s 15 μm filter is advantageous here since it directly probes restframe 8 μm at z ~ 0.8, without relying on a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. Results. We have found that cluster IR LFs at restframe 8 μm have a factor of 2.4 smaller L^∗ and a steeper faint-end slope than that of the field. Confirming this trend, we also found that faint-end slopes of the cluster LFs becomes flatter and flatter with decreasing local galaxy density. These changes in LFs cannot be explained by a simple infall of field galaxy population into a cluster. Physics that can preferentially suppress IR luminous galaxies in high density regions is required to explain the observed results.

Item Type:Article
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Pearson, C.0000-0001-6139-649X
Im, M.0000-0002-8537-6714
Additional Information:© ESO 2010. Received 14 October 2009. Accepted 22 December 2009. Published online 03 May 2010. We thank the anonymous referee for many insightful comments, which significantly improved the paper. We are grateful to Masayuki Tanaka for useful discussions. We thank L. Bai for providing data for comparison. T.G., Y.K., and H.I. acknowledge financial support from the Japan Society for the Promotion of Science (JSPS) through JSPS Research Fellowships for Young Scientists. M.I. was supported by the Korea Science and Engineering Foundation (KOSEF) grant No. 2009-0063616, funded by the Korea government (MEST). H.M.L. acknowledges the support from KASI through its cooperative fund in 2008. This research is based on the observations with AKARI, a JAXA project with the participation of ESA. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this sacred mountain.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)UNSPECIFIED
Korea Science and Engineering Foundation2009-0063616
Ministry of Education, Science and Technology (Korea)UNSPECIFIED
Korea Astronomy and Space Science Institute (KASI)UNSPECIFIED
Subject Keywords:galaxies: evolution, galaxies: interactions, galaxies: starburst, galaxies: peculiar, galaxies: formation, infrared: galaxies
Record Number:CaltechAUTHORS:20100604-073622745
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Official Citation:Environmental dependence of 8 μm luminosity functions of galaxies at z ~ 0.8 - Comparison between RXJ1716.4+6708 and the AKARI NEP-deep field A7 T. Goto et al. Published Online: 03 May 2010 DOI: 10.1051/0004-6361/200913473
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18556
Deposited By: Ruth Sustaita
Deposited On:04 Jun 2010 16:45
Last Modified:24 Oct 2017 21:22

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