Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-25T15:55:42.017Z Has data issue: false hasContentIssue false
  • English
  • Français

Investigating the early phase of the galaxy evolution through high-z damped Lyα absorption systems

Published online by Cambridge University Press:  10 June 2020

Kazuyuki Ogura ,
Tohru Nagao ,
Masatoshi Imanishi ,
Nobunari Kashikawa ,
Yoshiaki Taniguchi ,
Masaru Kajisawa ,
Masakazu A. R. Kobayashi  and
Yoshiki Toba
Kazuyuki Ogura
Affiliation:
Faculty of Education, Bunkyo University, 3337 Minamiogishima, Koshigaya, Saitama, Japan email: [email protected]
Tohru Nagao
Affiliation:
Research Center for Space and Cosmic Evolution, Ehime University
Masatoshi Imanishi
Affiliation:
Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan Department of Astronomy, School of Science, SOKENDAI
Nobunari Kashikawa
Affiliation:
Department of Astronomy, School of Science, The University of Tokyo
Yoshiaki Taniguchi
Affiliation:
The Open University of Japan
Masaru Kajisawa
Affiliation:
Graduate School of Science and Engineering, Ehime University
Masakazu A. R. Kobayashi
Affiliation:
Faculty of Natural Sciences, National Institute of Technology, Kure college
Yoshiki Toba
Affiliation:
Department of Astronomy, Kyoto University
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the physical properties of Lyα emitters (LAEs) in a “DLA-concentrated regions” where there are 3 or more DLA within (50 Mpc)3 cubic box. We observed LAEs in a DLA-concentrated region at z = 2.3, the J1230+34 field, with Subaru/Suprime-Cam. In the 50 Mpc scale, we found no deferences in properties of LAEs such as Lyα luminosity function in the DLA-concentrated region compared to other fields at similar redshift. On the other hand, we found a ∼10 Mpc scale LAE overdensity around a strong DLA with NHI = 1021.08 cm−2.

Keywords

quasars: absorption linesgalaxies: emission linesgalaxies: formationlarge-scale structure of universe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 294 - 296
Copyright
© International Astronomical Union 2020

References

Franck, J. R. & McGaugh, S. S. 2016, ApJ, 817, 15810.3847/0004-637X/817/2/158CrossRefGoogle Scholar
Krogager, J.-K., Møller, P., Fynbo, J. P. U., & Noterdaeme, P. 2017, A&A, 469, 2959Google Scholar
Noterdaeme, P., Petitjean, P., Carithers, W. C., Pâris, I., Font-Ribera, A., Bailey, S., Aubourg, E., Bizyaev, D., et al. 2012, A&A, 547, L1Google Scholar
Noterdaeme, P., Petitjean, P., Ledoux, C., & Srianand, R. 2009, A&A, 505, 1087Google Scholar
Ogura, K., Nagao, T., Imanishi, M., Kashikawa, N., Taniguchi, Y., Kajisawa, M., Kobayasi, M. A. R., Toba, Y., Nobuhara, K., et al. 2017, PASJ, 69, 5110.1093/pasj/psx027CrossRefGoogle Scholar
Overzier, R. A. 2016, A&AR, 24, 14Google Scholar
Wolfe, A. M., Gawiser, E., & Prochaska, J. X. 2005, ARA&A, 43, 86110.1146/annurev.astro.42.053102.133950CrossRefGoogle Scholar