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A&A Supplement series, Vol. 122, April II 1997, 201-213

Received March 20; accepted April 22, 1996

The ROSAT Galactic Plane Survey: Analysis of a low latitude sample area in Cygnus

The observations

C. Motch tex2html_wrap1558 - P. Guillout tex2html_wrap1560 - F. Haberl tex2html_wrap1562 - M.W. Pakull tex2html_wrap1564 - W. Pietsch tex2html_wrap1566 - K. Reinsch tex2html_wrap1568

Send offprint request: C. Motch

tex2html_wrap1570  Observatoire Astronomique, UA 1280 CNRS, 11 rue de l'Université, F-67000 Strasbourg, France
tex2html_wrap1572  Max-Planck-Institut für Extraterrestrische Physik, D-85740, Garching bei München, Germany
tex2html_wrap1574  Sternwarte, Geismarlandstrasse 11, D-37083, Göttingen, Germany


The analysis of the part of the ROSAT all-sky survey covering the galactic plane is the scope of a dedicated project called the ROSAT Galactic Plane Survey. In order to statistically understand the nature of the tex2html_wrap_inline1518 14 000 sources discovered by ROSAT at |b| tex2html_wrap_inline1522 20tex2html_wrap1576 , a number of sample areas have been chosen for follow-up optical identification. In this paper we present the X-ray and optical material gathered in a region located in the Cygnus constellation, centered at l = 90tex2html_wrap1578 , b = 0tex2html_wrap1580 and covering an area of 64.5degtex2html_wrap_inline1534. A total of 95 and 128 sources are detected with a maximum likelihood larger than 10 and 8 respectively. With a typical survey exposure time of the order of 700 to 900s the flux completeness level is tex2html_wrap_inline1536 0.02 cts stex2html_wrap_inline1538 corresponding to tex2html_wrap_inline1540 2 10tex2html_wrap_inline1542erg cmtex2html_wrap_inline1544 stex2html_wrap_inline1546 . The position of the sample area allows to investigate the soft X-ray content of a rather typical region of the galactic plane. In this paper we describe the details of the observational procedures and data reduction. For each ROSAT source we list the main X-ray characteristics together with those of the proposed optical identification. When appropriate, we also show optical spectra and finding charts. The full analysis and discussion of these data are presented in a companion paper (Motch et al. 1997).gif

keywords: X-ray general, X-ray stars, stars: activity, stars: neutron, stars: statistics

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