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A&A Supplement series, Vol. 126, December II 1997, 401-406

Received November 14, 1996; accepted April 2, 1997

Cepheids as tracers of star formation in M 31gif,gif

I. Observations and identifications

E.A. Magniertex2html_wrap1021 - T. Augusteijntex2html_wrap1023 - S. Prinstex2html_wrap1025 - J. van Paradijstex2html_wrap1027 - W.H.G. Lewintex2html_wrap1029

Send offprint request: E.A. Magnier:

tex2html_wrap1031  Astronomical Institute "Anton Pannekoek'', Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
tex2html_wrap1033  Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
tex2html_wrap1035  University of Illinois, Astronomy Dept. Bldg. 103, 1002 W. Green St., Urbana, IL 61801, U.S.A.
tex2html_wrap1037  Astronomy Dept. 351580, University of Washington, Seattle, WA 98195, U.S.A.
tex2html_wrap1039  Massachusetts Institute of Technology, Room 37-624, Cambridge, MA 02139, U.S.A.
tex2html_wrap1041  European Southern Observatory, Casilla 19001, Santiago 19, Chile
tex2html_wrap1043  Physics Department, University of Alabama in Huntsville, Huntsville, AL 35899, U.S.A.


Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (< 3%). For V < 21, the completeness is tex2html_wrap_inline1015 53%. These Cepheids will be used to explore the star formation history in M 31.

keywords: (stars: variables:) Cepheids -- stars: formation -- galaxies: individual: M 31 -- galaxies: stellar content -- (cosmology:) distance scale

Copyright by the European Southern Observatory (ESO)