Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://www.adass.org/adass/proceedings/adass99/P3-35/
Дата изменения: Wed Oct 4 05:31:09 2000 Дата индексирования: Tue Oct 2 05:13:10 2012 Кодировка: Поисковые слова: trifid nebula |
in galactic coordinates, where the acronyms in the Galactic plane are those described by Derue et al. (1999) while SN/NR indicates search fields for supernovæ and brown dwarfs.
The EROS II two colour CCD wide-field imager (Bauer & de Kat 1998) is mounted at the Cassegrain focus of the 1-m Marly telescope at ESO Observatory, La Silla. A beam-splitting dichroic cube with a CCD camera mounted behind each channel allows simultaneous imaging in wide pass-bands (420-650 nm, so-called ``blue'', and 650-900 nm, so-called ``red'') in a field of 0.7$^$(right ascension) x 1.4$^$ (declination). Each camera contains a mosaic of 8 Loral 2048 x 2048 thick CCD's and typical global image quality (atmospheric seeing + instrument) is 2 arcsec FWHM for a pixel size of 0.6 arcsec. Images are stored on DLT tapes which are shipped to the CCPN (IN2P3 computing center, CNRS) in Lyon, France, where data processing occurs. The dedicated photometry package PEIDA used in EROS experiment to produce individual light curves is described in details by Ansari (1996). Figure 2 shows the fields accumulated since early 1996.
![]() |
As a typical crowded field contains a set of 300,000 stars,
the relational database in CCPN is now managing tens of thousands of
images and tens of millions of light curves. The final amount of date is
estimated to several TB.
The EROS data contain a significant fraction of variables objects which are noise for the search of microlensing events but are goldmine for stellar variability studies. The EROS I data have already produced identification of Cepheids (Beaulieu et al. 1995b) and eclipsing binaries (Grison et al. 1995) in the bar of the Large Magellanic Cloud. This work has been pursued in the EROS II stage with the discovery of a slope change in the Period-Luminosity relation of the classical Cepheids in Small Magellanic Cloud with periods lower than 2 days (Bauer et al. 1999). In the same way, the first discovery of pre-main sequence stars in Magellanic Clouds (Beaulieu et al. 1996) and the recent detection of a slow nova in the Small Magellanic Cloud (de Laverny et al. 1998) show evidently that exploration of the EROS database (for both I and II stages) is far from to be achieved.
Afonso, C. et al. (EROS collaboration) 1998, A&A, 337, L17
Ansari., R. 1996, Vistas in Astronomy, 40, 519
Aubourg, E. et al. (EROS collaboration) 1993, Nature, 365, 623
Bauer, F., & de Kat, J. 1998, in Optical Detectors for
Astronomy, eds.
J.W. Beletic & P. Amico (Boston: Kluwer Academic Publishers), 191
Bauer, F. et al. (EROS collaboration) 1999, A&A, 348, 175
Beaulieu, J. P. et al. (EROS collaboration) 1995a, A&A, 299, 168
Beaulieu, J. P. et al. (EROS collaboration) 1995b, A&A, 303, 137
Beaulieu, J. P. et al. (EROS collaboration) 1996, Science, 272, 995
Derue, F. et al. (EROS collaboration) 1999, A&A, 357, 87
Goldman, B. et al. (EROS collaboration) 1999, A&A, 351, L5
Grison, P. et al. (EROS collaboration) 1995, A&AS, 109, 447
Hamilton, J. C. et al. (EROS collaboration) 1999, in preparation
Hardin, D. et al. (EROS collaboration) 1999, in preparation
de Laverny, P. et al. (EROS collaboration) 1998, A&A, 335, L93
Omont, A. et al. 1999, A&A, 348, 755
Paczyski, B. 1986, ApJ, 304, 1
Palanque-Delabrouille, N. et al. (EROS collaboration) 1998, A&A, 332, 1