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Mapping and resolving galaxy formation at its peak epoch with Mahalo-Subaru and Gracias-ALMA

Published online by Cambridge University Press:  09 February 2015

Tadayuki Kodama ,
Masao Hayashi ,
Yusei Koyama ,
Ken-ichi Tadaki ,
Ichi Tanaka ,
Rhythm Shimakawa ,
Tomoko Suzuki  and
Moegi Yamamoto
Tadayuki Kodama
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, Tokyo181-8588, Japan email: t.kodama@nao.ac.jp Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI96720, USA Department of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo181-8588, Japan
Masao Hayashi
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, Tokyo181-8588, Japan email: t.kodama@nao.ac.jp
Yusei Koyama
Affiliation:
Institute of Space Astronomical Science, Japan Aerospace Exploration Agency Sagamihara, Kanagawa, 252-5210, Japan
Ken-ichi Tadaki
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, Tokyo181-8588, Japan email: t.kodama@nao.ac.jp
Ichi Tanaka
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI96720, USA
Rhythm Shimakawa
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI96720, USA Department of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo181-8588, Japan
Tomoko Suzuki
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, Tokyo181-8588, Japan email: t.kodama@nao.ac.jp Department of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo181-8588, Japan
Moegi Yamamoto
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, Tokyo181-8588, Japan email: t.kodama@nao.ac.jp Department of Astronomical Science, Graduate University for Advanced Studies, Mitaka, Tokyo181-8588, Japan
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Abstract

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MAHALO-Subaru (MApping HAlpha and Lines of Oxygen with Subaru) project aims to investigate how the star forming activities in galaxies are propagated as a function of time, mass, and environment. It employs a unique set of narrow-band filters on MOIRCS/Subaru to search for Ha emitters associated to the proto-clusters or in narrow redshift slices in the general field. We have shown not only filamentary/clumpy structures of all the proto-clusters but also very high star formation activities therein especially at z > 2. HST images from the CANDELS survey have revealed that nearly half of the Hα emitters in the field at z ∼ 2 have clumpy structures. Among them, “red dusty clumps” are preferentially found at or near the mass center of galaxies. Therefore, they are probably linked to the formation of bulge component. To explore physical states and the mode of star formation of those forming galaxies, we have started Gracias-ALMA project in full coordination with the Mahalo-Subaru project. We will resolve molecular gas contents and dusty star formation within these galaxies, and tell whether clumps are formed by gravitational instability of gas rich disks, and whether bulges are formed by clump migration or through galaxy-galaxy mergers.

Keywords

galaxies: clustersgalaxies: formationgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 255 - 258
Copyright
Copyright © International Astronomical Union 2015 

References

Bournaud, F., Perret, V., Renaud, F., et al. 2013, ApJ, 780, 57Google Scholar
Dekel, A., Birnboim, Y., Engel, G., et al. 2009, Nature, 457, 451CrossRefGoogle 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., Tadaki, K., et al. 2012, ApJ, 757, 15Google Scholar
Hopkins, A. M. & Beacom, J. F. 2006, ApJ, 651, 142Google Scholar
Kodama, T., Balogh, M. L., Smail, I., et al. 2004, MNRAS, 354, 1103Google Scholar
Kodama, T., Tanaka, I., Hayashi, M., et al. 2013, ASPC, 476, 37Google 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, 1551Google Scholar
Koyama, Y., Kodama, T., Tadaki, K., et al. 2014, ApJ, 789, 18Google Scholar
Shimakawa, R., Kodama, T., Tadaki, K., et al. 2014a, MNRAS, 441, L1CrossRefGoogle Scholar
Shimakawa, R., Kodama, T., Tadaki, K., et al. 2014b, arXiv1406.5219Google Scholar
Suzuki, T., et al. 2014, in preparationGoogle Scholar
Tadaki, K., Kodama, T., Koyama, Y., et al. 2011, PASJ, 63, 437Google Scholar
Tadaki, K., Kodama, T., Ota, K., et al. 2012, MNRAS, 423, 2617CrossRefGoogle Scholar
Tadaki, K., Kodama, T., Tanaka, I., et al. 2013, ApJ, 778, 114CrossRefGoogle Scholar
Tanaka, I., De Breuck, C., Kurk, J., et al. 2011, PASJ, 63, 415Google Scholar