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

Creators: Takahashi, M. I.; Shioya, Y.; Taniguchi, Y.; Murayama, T.; Ajiki, M.; Sasaki, S. S.; Koizumi, O.; Nagao, T.; Scoville, N. Z.; Mobasher, B.; Aussel, H.; Capak, P.; Carilli, C.; Ellis, R. S.; Garilli, B.; Giavalisco, M.; Guzzo, L.; Hasinger, G.; Impey, C.; Kitzbichler, M. G.; Koekemoer, A.; Le Fèvre, O.; Lilly, S. J.; Maccagni, D.; Renzini, A.; Rich, M.; Sanders, D. B.; Schinnerer, E.; Scodeggio, M.; Shopbell, P.; Smolčić, V.; Tribiano, S.; Ideue, Y.; Mihara, S.

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.

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.

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