Zhou, Xu and Fan, Zhou and Jiang, Zhaoji and Ashley, M. C. B. and Cui, Xiangqun and Feng, Longlong and Gong, Xuefei and Hu, Jingyao and Kulesa, C. A. and Lawrence, J. S. and Liu, Genrong and Luong-Van, D. M. and Ma, Jun and Moore, A. M. and Qin, Weijia and Shang, Zhaohui and Storey, J. W. V. and Sun, Bo and Travouillon, T. and Walker, C. K. and Wang, Jiali and Wang, Lifan and Wu, Jianghua and Wu, Zhenyu and Xia, Lirong and Yan, Jun and Yang, Ji and Yang, Huigen and Yuan, Xiangyan and York, D. and Zhang, Zhanhai and Zhu, Zhenxi (2010) The First Release of the CSTAR Point Source Catalog from Dome A, Antarctica. Publications of the Astronomical Society of the Pacific, 122 (889). pp. 347-353. ISSN 0004-6280 http://resolver.caltech.edu/CaltechAUTHORS:20100324-111509854
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In 2008 January the twenty-fourth Chinese expedition team successfully deployed the Chinese Small Telescope ARray (CSTAR) to Dome A, the highest point on the Antarctic plateau. CSTAR consists of four 14.5 cm optical telescopes, each with a different filter (g, r, i, and open) and has a 4.5° × 4.5° field of view (FOV). It operates robotically as part of the Plateau Observatory, PLATO, with each telescope taking an image every ~30 s throughout the year whenever it is dark. During 2008, CSTAR 1 performed almost flawlessly, acquiring more than 0.3 million i-band images for a total integration time of 1728 hr during 158 days of observations. For each image taken under good sky conditions, more than 10,000 sources down to ~16th magnitude could be detected. We performed aperture photometry on all the sources in the field to create the catalog described herein. Since CSTAR has a fixed pointing centered on the south celestial pole (decl. = -90°), all the sources within the FOV of CSTAR were monitored continuously for several months. The photometric catalog can be used for studying any variability in these sources, and for the discovery of transient sources such as supernovae, gamma-ray bursts, and minor planets.
|Additional Information:||© 2010 Astronomical Society of the Pacific. Received 2009 November 23; accepted 2010 January 25; published 2010 February 24. This study has been supported by the Chinese National Natural Science Foundation through grants 10873016, 10803007, 10473012, 10573020, 10633020, 10673012, and 10603006, and by the National Basic Research Program of China (973 Program), No. 2007CB815403. This research is also supported by the Chinese PANDA International Polar Year project, the Polar Research Institute of China (PRIC), and the international science and technology cooperation projects 2008DFA20420 of the Ministry of Science and Technology of China. The PLATO observatory was supported by the Australian Research Council and the Australian Antarctic Division. Iridium communications were provided by the US National Science Foundation and the United States Antarctic Program. The authors wish to thank all members of the 2008 and 2009 PRIC Dome A expeditions for their heroic effort in reaching the site and for providing invaluable assistance to the expedition astronomers in setting up and servicing the PLATO observatory and its associated instrument suite. Additional financial contributions have been made by the institutions involved in this collaboration.|
|Official Citation:||The First Release of the CSTAR Point Source Catalog from Dome A, Antarctica Xu Zhou, Zhou Fan, Zhaoji Jiang, M. C. B. Ashley, Xiangqun Cui, Longlong Feng, Xuefei Gong, Jingyao Hu, C. A. Kulesa, J. S. Lawrence, Genrong Liu, D. M. Luong-Van, Jun Ma, A. M. Moore, Weijia Qin, Zhaohui Shang, J. W. V. Storey, Bo Sun, T. Travouillon, C. K. Walker, Jiali Wang, Lifan Wang, Jianghua Wu, Zhenyu Wu, Lirong Xia, Jun Yan, Ji Yang, Huigen Yang, Xiangyan Yuan, D. York, Zhanhai Zhang, and Zhenxi Zhu Publications of the Astronomical Society of the Pacific 2010 122:889, 347-353|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||30 Mar 2010 22:30|
|Last Modified:||26 Dec 2012 11:55|
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