Hostname: page-component-78c5997874-j824f Total loading time: 0 Render date: 2024-11-02T19:02:43.983Z Has data issue: false hasContentIssue false
  • English
  • Français

Panoramic Views of Cluster Evolution Since z = 3

Published online by Cambridge University Press:  01 August 2006

Tadayuki Kodama ,
M. Tanaka ,
Ichi Tanaka  and
M. Kajisawa
Tadayuki Kodama
Affiliation:
National Astronomical Obseravtory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan email: [email protected], [email protected]
M. Tanaka
Affiliation:
Department of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan email: [email protected]
Ichi Tanaka
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 650 North Aohoku Place, Hilo, HI 96720, USA email: [email protected]
M. Kajisawa
Affiliation:
National Astronomical Obseravtory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan email: [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Extract

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 have been conducting PISCES project (Panoramic Imaging and Spectroscopy of Cluster Evolution with Subaru; Kodama et al. 2005) with making use of the wide-field imaging capability of Subaru. Our motivations are first to map out large scale structures and define local envioronments of galaxies therein, and then to investigate the variation in galaxy properties as a function of environment and mass. We have completed multi-colout imaging of 8 distant clusters between 0.4 < z < 1.3 so far, and we have mapped out filamentary/clumpy structures in and around the clusters across 15–30 Mpc scales (see some examples in Fig. 1). These two clusters have secure spectroscopic confirmation of the physical association of the structures to the main body of the clusters. From the photometric and spectroscopic properties of galaxies over a wide range in environment, we have found that the truncation of galaxies is seen in the outskirts of clusters rather than in cluster cores. We have also seen a clear environmental dependence of the “down-sizing” in the sense that the stage of down-sizing is delayed in lower density environments.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 170 - 171
Copyright
Copyright © International Astronomical Union 2007

References

Kajisawa, M., Kodama, T., Tanaka, I., Yamada, T., & Bower, R.G. 2006, MNRAS 371, 577.CrossRefGoogle Scholar
Kodama, T., Arimoto, N.Barger, A.J. & Aragón-Salamanca, A. 1998, A&A 334, 99.Google Scholar
Kodama, T. 2005, PASJ 57, 309.CrossRefGoogle Scholar
Tanaka, M., Kodama, T., Arimoto, N., & Tanaka, 2006, MNRAS 365, 1392.CrossRefGoogle Scholar