The Beijing-Arizona-Taipei-Connecticut (BATC) \\Color Survey of the Sky

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Session 41 -- Catalogs, Computer Information, Services, Analysis and Tools
Display presentation, Tuesday, 10, 1995, 9:20am - 6:30pm

[41.10] The Beijing-Arizona-Taipei-Connecticut (BATC) \\Color Survey of the Sky

D. Burstein, J.J. Hester, R.A. Windhorst, L. Clampitt, Y. Li, B. Moore (ASU), L.Z. Fang (UofA), J.S. Chen, J. Zhu, Z.J. Jiang, X.H. Fan, H. Wu, H.J. Yan, Z.Y. Zheng, X. Zhou (BAO), H.J. Su, Z.H. Shang (PMO), F.Z. Chen, Z.G. Deng (USTC), W.H. Sun, W.P. Chen, W.S. Tsay, T.H. Chiueh, C.M. Ko, C.K. Chou (NCU), P. Lu (WCSU)

The observational goal of the BATC Survey is to do spectrophotometry from 3300$\rm \AA$ to 1 $\mu$ of all objects found within 500 pre-selected 0.95~deg$^2$ areas of the Northern sky, to an effective magnitude limit of V~=~21. The 0.6m Schmidt telescopes of the Beijing Astronomical Observatory has been equipped with Ford $2048^2$ CCDs, Sun computers and specially designed intermediate and narrow band interference filters. The intermediate band filters are of width $\rm 200-300 \AA$ and cover the full spectral range, avoiding bright sky lines. The narrow band filters isolate well-known emission line features such as $\rm H\alpha$ and O[III]. 150 areas are preselected centered on quasars of known properties; 150 areas are centered on bright, nearby spiral galaxies; 150 are randomly selected and 50 areas are centered on calibration objects (star clusters; spectrophotometric standard fields, etc.). The scientific goals of our survey will be summarized. Various technical aspects of the survey will be described, together with first results on the photometric stability of the observing site (The Xing Long station of the Beijing Astronomical Observatory, 150 km NE of Beijing). Photometric observations of stellar objects in and around M67 have been used as a first test-case for the expected accuracy of this survey. Color-magnitude diagrams of the M67 field based on these observations will be presented. In addition, three blue stellar objects are high-z quasar candidates, for which we hope to obtain spectra before the meeting.

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