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The [O II] λ3727 Luminosity Function and Star Formation Rate at z ≈ 1.2 in the COSMOS 2 Square Degree Field and the Subaru Deep Field

Takahashi, M. I. and Shioya, Y. and Taniguchi, Y. and Murayama, T. and Ajiki, M. and Sasaki, S. S. and Koizumi, O. and Nagao, T. and Scoville, N. Z. and Mobasher, B. and Aussel, H. and Capak, P. and Carilli, C. and Ellis, R. S. and Garilli, B. and Giavalisco, M. and Guzzo, L. and Hasinger, G. and Impey, C. and Kitzbichler, M. G. and Koekemoer, A. and Le Fèvre, O. and Lilly, S. J. and Maccagni, D. and Renzini, A. and Rich, M. and Sanders, D. B. and Schinnerer, E. and Scodeggio, M. and Shopbell, P. and Smolčić, V. and Tribiano, S. and Ideue, Y. and Mihara, S. (2007) The [O II] λ3727 Luminosity Function and Star Formation Rate at z ≈ 1.2 in the COSMOS 2 Square Degree Field and the Subaru Deep Field. Astrophysical Journal Supplement Series, 172 (1). pp. 456-467. ISSN 0067-0049. http://resolver.caltech.edu/CaltechAUTHORS:20100112-113531217

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Abstract

We have carried out a wide-field imaging survey for [O II] λ3727 emitting galaxies at z ≈ 1.2 in the HST COSMOS 2 square degree field using the Suprime-Cam on the Subaru Telescope. The survey covers a sky area of 6700 arcmin^2 in the COSMOS field, and a redshift range between 1.17 and 1.20 (Δz = 0.03), corresponding to a survey volume of 5.56 × 10^5 Mpc^3. We obtain a sample of 3176 [O II] emitting galaxies with observed emission-line equivalent widths greater than 26 Å. Since our survey tends to sample brighter [O II] emitting galaxies, we also analyze a sample of fainter [O II] emitting galaxies found in the Subaru Deep Field (SDF). We find an extinction-corrected [O II] luminosity density of 10^(40.35)^(+0.08)_(-0.06) ergs s^(-1) Mpc^(-3), corresponding to star formation rate density of 0.32^(+0.06)_(-0.04) M_☉ yr^(-1) Mpc^(-3) in the COSMOS field at z ≈ 1.2. This is the largest survey for [O II] emitters beyond z = 1 currently available.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/518037DOIArticle
http://www.iop.org/EJ/abstract/0067-0049/172/1/456/PublisherArticle
Additional Information:© 2007 American Astronomical Society . Print publication: Issue 1 (2007 September); received 2006 September 15; accepted for publication 2007 March 3. The HST COSMOS treasury program was supported through NASA grant HST-GO-09822. We greatly acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. The COSMOS science meeting in 2005 May was supported by in part by the NSF through grant OISE-0456439. We would also like to thank the Subaru Telescope staff for their invaluable help. This work was financially supported in part by the JSPS (grants 15340059 and 17253001). S. S. S. and T. N. are JSPS fellows.
Group:COSMOS
Funders:
Funding AgencyGrant Number
NASAHST-GO-09822
NSFOISE-0456439
Japan Society for the Promotion of Science (JSPS)15340059
Japan Society for the Promotion of Science (JSPS)17253001
Subject Keywords:galaxies: distances and redshifts; galaxies: evolution; galaxies: luminosity function, mass function
Record Number:CaltechAUTHORS:20100112-113531217
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100112-113531217
Official Citation:The [O II] λ3727 Luminosity Function and Star Formation Rate at z 1.2 in the COSMOS 2 Square Degree Field and the Subaru Deep Field M. I. Takahashi, Y. Shioya, Y. Taniguchi, T. Murayama, M. Ajiki, S. S. Sasaki, O. Koizumi, T. Nagao, N. Z. Scoville, B. Mobasher, H. Aussel, P. Capak, C. Carilli, R. S. Ellis, B. Garilli, M. Giavalisco, L. Guzzo, G. Hasinger, C. Impey, M. G. Kitzbichler, A. Koekemoer, O. Le Fèvre, S. J. Lilly, D. Maccagni, A. Renzini, M. Rich, D. B. Sanders, E. Schinnerer, M. Scodeggio, P. Shopbell, V. Smolčić, S. Tribiano, Y. Ideue, and S. Mihara 2007 ApJS 172 456-467 doi: 10.1086/518037
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17146
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:25 Jan 2010 19:13
Last Modified:25 Jun 2015 20:19

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