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Mahalo-Subaru: Mapping Star Formation at the Peak Epoch of Massive Galaxy Formation

Published online by Cambridge University Press:  17 July 2013

Tadayuki Kodama ,
Masao Hayashi ,
Yusei Koyama ,
Ken-ichi Tadaki ,
Ichi Tanaka  and
Rhythm Shimakawa
Tadayuki Kodama
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720, USA email: t.kodama@nao.ac.jp Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181–8588, Japan Dept. of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo 181–8588, Japan
Masao Hayashi
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181–8588, Japan
Yusei Koyama
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181–8588, Japan Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
Ken-ichi Tadaki
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory, Mitaka, Tokyo 181–8588, Japan Dept. of Astronomy, Graduate School of Science, Univ. of Tokyo, Tokyo 113–0033, Japan
Ichi Tanaka
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720, USA email: t.kodama@nao.ac.jp
Rhythm Shimakawa
Affiliation:
Dept. of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo 181–8588, Japan
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Abstract

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MAHALO-Subaru (MApping HAlpha and Lines of Oxygen with Subaru) is our on-going large programme which aims to investigate how the star forming activities in galaxies are propagated as a function of time, mass, and environment. We are targeting 10 clusters and proto-clusters at 0.4<z<2.6, and two general fields (GOODS-N and SXDF-CANDELS) with Suprime-Cam and MOIRCS by utilizing our unique sets of narrow-band filters. The narrow-band imaging can map out star forming galaxies with the redshifted Halpha and/or [OII] emission lines from our targets, and thus providing relatively unbiased views of star forming activities across time and environment. We have almost completed narrow-band imaging of our targets, and found that star forming activity is very high even in the proto-cluster cores (z≳1.5), and that the peak of star formation is shifted outwards with time, indicating the inside-out formation of clusters. Moreover, we have identified many “red” emitters especially in high density regions at z>2, which suggests that the mode of star formation and/or the activation of AGN are dependent on environment, and thus holding the key to the environmental effects at the early stage of cluster galaxies formation and evolution.

Keywords

galaxies: clustersgalaxies: evolutiongalaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S295: The intriguing life of massive galaxies , August 2012 , pp. 74 - 77
Copyright
Copyright © International Astronomical Union 2013 

References

Bouwens, R. J., Illingworth, G. D., Franx, M., et al. 2008, ApJ, 686, 230Google Scholar
Cen, R. & Ostriker, J. P. 1993, ApJ, 417, 415CrossRefGoogle Scholar
Fan, X. 2006, NewAR, 50, 665Google Scholar
Furusawa, H., Kosugi, G., Akiyama, M., et al. 2008, ApJS, 176, 1Google Scholar
Grogin, N. A., Kocevski, D. D., Faber, S. M., et al. 2011, ApJS, 197, 35Google Scholar
Hayashi, M., Kodama, T., Koyama, Y., et al. 2010, MNRAS, 402, 1980Google Scholar
Hayashi, M., Kodama, T., Koyama, Y., et al. 2011, MNRAS, 415, 2670Google Scholar
Hayashi, M., Kodama, T., Tadaki, K., et al. 2012, ApJ, 757, 15Google Scholar
Lawrence, A., Warren, S. J., & Almaini, O. 2007, MNRAS, 379, 1599Google Scholar
Kodama, T., Arimoto, N., Barger, A. J., et al. 1998, A&A, 334, 99Google Scholar
Kodama, T., Balogh, M. L., Smail, I., et al. 2004, MNRAS, 354, 1103Google Scholar
Kodama, T., Tanaka, M., Arimoto, N., et al. 2005, PASJ, 57, 309Google Scholar
Kodama, T., Tanaka, I., Kajisawa, M., et al. 2007, MNRAS, 377, 1717Google Scholar
Koyama, Y., Kodama, T., Shimasaku, K., et al. 2010, MNRAS, 403, 1611Google Scholar
Koyama, Y., Kodama, T., Nakata, F., et al. 2011, ApJ, 734, 66CrossRefGoogle Scholar
Koyama, Y., Kodama, T., Tadaki, K., et al. 2013, MNRAS, 428, 1551CrossRefGoogle Scholar
Tadaki, K., Kodama, T., Koyama, Y., et al. 2011, PASJ, 63, 437CrossRefGoogle Scholar
Tadaki, K., Kodama, T., Ota, K., et al. 2012, MNRAS, 423, 2617CrossRefGoogle Scholar
Tanaka, I., De Breuck, C., Kurk, J., et al. 2011, PASJ, 63, 415Google Scholar