Free Access
Issue
Astron. Astrophys. Suppl. Ser.
Volume 143, Number 2, April II 2000
Page(s) 215 - 226
DOI https://doi.org/10.1051/aas:2000178
Published online 15 April 2000
DOI: 10.1051/aas:2000178

Astron. Astrophys. Suppl. Ser. 143, 215-226

RR Lyrae variables in the globular cluster M 5

J. Kaluzny1 - A. Olech2 - I. Thompson3 - W. Pych2 - W. Krzeminski1,3 - A. Schwarzenberg-Czerny1,4

Send offprint request: A. Olech,
e-mail: olech@sirius.astrouw.edu.pl


1 - Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
e-mail: jka,wk,alex@camk.edu.pl
2 - Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warsaw, Poland
e-mail: olech,pych@sirius.astrouw.edu.pl
3 - Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, U.S.A.
e-mail: ian@ociw.edu
4 - Astronomical Observatory of Adam Mickiewicz University, ul. Sloneczna 36, 61-286 Poznan, Poland

Received July 2, 1999; accepted January 27, 2000

Abstract:

We present V-band CCD photometry of 65 RR Lyr variables from the globular cluster M 5. We have estimated the basic physical parameters for 16 RRc stars and 26 RRab stars using a Fourier decomposition of the light curves of the variables. The mean values of mass, luminosity, effective temperature and relative helium abundance for the RRc stars are measured to be ${\cal M}=0.54~{\cal M}_\odot$, $\log
(L/L_\odot)=1.69$, $T_{\rm eff}=7353$ K and Y=0.28, respectively. For the RRab variables the derived mean values of absolute magnitude, metallicity and effective temperature are: MV=0.81, ${\rm
[Fe/H]}=-1.23$ and $T_{\rm eff}=6465$ K. We find that the V amplitude of an RRab star for a given period is a function of metal abundance rather than Oosterhoff type.

We find significant problems with the calibration of both the zero point and the scale of the luminosities measured with the Fourier technique. The apparent distance modulus derived from RRc stars is equal to $14.47\pm0.11$ and it is in good agreement with recent determinations. On the other hand distance modulus obtained from the sample of RRab stars (calibrated by the Baade-Wesselink observations of field RR Lyr variables) is significantly smaller and equal to $14.27\pm0.04$

Key words: stars: RR Lyr -- stars: variables -- globular clusters: individual: M 5

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Copyright The European Southern Observatory (ESO)

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