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II/208 BVRI CCD photometry in the field of M 31 (Magnier+ 1992)
The following files can be converted to FITS (extension .fit .fiz or .fiZ)
*.dat
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Query from: http://vizier.cds.unistra.fr/cgi-bin/VizieR?-source=II/208
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Beginning of ReadMe :II/208 BVRI CCD photometry in the field of M 31 (Magnier+ 1992)
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BVRI CCD photometry of 361281 objects in the field of M 31
Magnier E.A., Lewin W.H.G., van Paradijs J., Hasinger G.,
Jain A., Pietsch W., Truemper J.
<Astron. Astrophys. Suppl. Ser. 96, 379 (1992)>
=1992A&AS...96..379M
Astrometry in the field of M 31.
Magnier E.A., Lewin W.H.G., van Paradijs J., Hasinger G.,
Pietsch W., Truemper J.
<Astron. Astrophys., 272, 695 (1993)>
=1993A&A...272..695M
Extension of the Magnier et al. catalogue of objects in the field of M31.
Haiman Z., Magnier E., Lewin W.H.G., Lester R.R., van Paradijs J.,
Hasinger G., Pietsch W., Supper R., Truemper J.
<Astron. Astrophys., 286, 725 (1994)>
=1994A&A...286..725H
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ADC_Keywords: Photometry, CCD ; Regional catalog ; Stars, faint ;
Keywords: Galaxies: M31 - photometry - spiral - stellar content
Description:
Deep BVRI CCD photometry was performed on a 1 square degree region of
M31. The observations were made between September 12 and September 27,
1990, using the McGraw-Hill 1.3m telescope at the
Michigan-Dartmouth-MIT (MDM) observatory at Kitt Peak.
The catalogue has typical completion limits of 22.3Bmag, 22.2Vmag,
22.2Rmag and 20.9Imag. Photometric accuracy is about 2% at Vmag=19.
The final astrometric calibrations take into account the systematic
error discovered in the Berkhuijsen etal (1987) catalog (Magnier etal
1993). They are in the J2000 system and are eventually tied to the HST
Guide Star Catalog. The final photometric calibrations are tied via
the NGC 206 region to photometry taken at the Michigan-Dartmouth-MIT
(MDM) 1.3m in September and October 1993. These are tied to the
Landolt (1992) system of standard stars, and are in the
Johnson-Kron-Cousins system (BVRcIc).
Caveats:
There are several known problems with the catalog. First, there are
likely to be some repeated detections of certain sources (i.e.,
multiple entries for the same object). Second, the wings of bright
sources in some cases may be included as distinct sources. Third, the
completeness limits are a strong function of position, and a much
lower near the core and the core of M32. Fourth, variable stars,
blended star, and stars with cosmic ray hits, cosmetic problems or
other failures may have highly abnormal colors and magnitudes. In
general, we expect these problems to be small, but the user is
cautioned to watch for these possible problems.