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Published December 2015 | Submitted
Journal Article Open

The Subaru COSMOS 20: Subaru optical imaging of the HST COSMOS field with 20 filters


We present both the observations and the data reduction procedures of the Subaru COSMOS 20 project, an optical imaging survey of the HST COSMOS field, carried out by using Suprime-Cam on the Subaru Telescope with the following 20 optical filters: six broad-band (B, g′, V, r′, i′, and z′), two narrow-band (NB711 and NB816), and 12 intermediate-band filters (IA427, IA464, IA484, IA505, IA527, IA574, IA624, IA679, IA709, IA738, IA767, and IA827). Part of this project is described in Taniguchi et al. (2007, ApJS, 172, 9) and Capak et al. (2007, ApJS, 172, 99) for the six broad-band and one narrow-band (NB816) filter data. In this paper, we present details of the observations and data reduction for the remaining 13 filters (the 12 IA filters and NB711). In particular, we describe the accuracy of both the photometry and astrometry in all the filter bands. We also present the optical properties of the Suprime-Cam IA filter system in appendices.

Additional Information

© 2015 The Author. Published by Oxford University Press on behalf of the Astronomical Society of Japan. Received January 30, 2015. Accepted October 2, 2015. Advance Access Publication Date: 2015 November 10. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at 〈http://www.astro.caltech.edu/∼cosmos〉. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS datasets. We are deeply grateful to the referee for his/her useful comments and excellent refereeing, which helped us to improve this paper very much. We would also like to thank the staff at the Subaru Telescope for their invaluable help. In particular, we would like to thank Hisanori Furusawa because his professional help as a support scientist made our Suprime-Cam observations successful. Data analysis was in part carried out on the common use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan. This work was financially supported in part by JSPS (YT: 15340059, 17253001, 19340046, 23244031; TN: 23654068 and 25707010) and by the Yamada Science Foundation (TN).

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