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The MV(RR)-[Fe/H] relation from the baade-wesselink method applied to field RR Lyrae stars

Published online by Cambridge University Press:  07 August 2017

G. Clementini ,
C. Cacciari  and
J.A. Fernley
G. Clementini
Affiliation:
Osservatorio Astronomico, Via Zamboni 33, I-40126 Bologna, Italy
C. Cacciari
Affiliation:
Osservatorio Astronomico, Via Zamboni 33, I-40126 Bologna, Italy
J.A. Fernley
Affiliation:
Dept. of Physics and Astronomy, University College London, London, England International Ultraviolet Explorer, VILSPA, Madrid, Spain

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We have applied two slightly different formulations of the Baade-Wesselink (B-W) method: (i) the Infrared Flux (IF) method (Fernley et al 1990a), and (ii) the Surface Brightness (SB) method (Cacciari et al 1989a), to derive the absolute magnitude of the field RR Lyrae stars UU Cet, RV Phe and W Tuc. The photometric (BVRIJHK) and radial velocity data used in the analysis have been published in Cacciari et al (1987, 1989b, 1991) and Clementini et al (1990). The Walraven photometry used in the IF method is by Lub (1977). Typical accuracies for individual data points are ±0.01-0.02 mag for the magnitudes and colours, and ±1-2km/sec for the radial velocity data. Excluding RV Phe, which may be affected by Blazhko effects, the results obtained from the IF and SB methods are rather consistent especially when the V–K colour is used in the SB method. For details see Cacciari et al. (1991).

Type
Poster Papers
Information
Symposium - International Astronomical Union , Volume 149: The Stellar populations of Galaxies , 1992 , pp. 407
Copyright
Copyright © Kluwer 

References

Cacciari, C., Clementini, G., Prévot, L., Lindgren, H., Lolli, M., and Oculi, L. 1987, Astron. Astrophys. Suppl. , 69, 135.Google Scholar
Cacciari, C., Clementini, G., Prévot, L., and Buser, R. 1989a, Astron. Astrophys. , 209, 141.Google Scholar
Cacciari, C., Clementini, , and Buser, R. 1989b, Astron. Astrophys. , 209, 154.Google Scholar
Cacciari, C., Clementini, , and Fernley, J.A. 1991, Ap.J. , submitted.Google Scholar
Clementini, G., Cacciari, C. and Lindgren, H. 1990, Astron. Astrophys. Suppl. , 85, 865.Google Scholar
Fernley, J.A., Skillen, I., Jameson, R.F., and Longmore, A.J. 1990, M.N.R.A.S. , 242, 685.Google Scholar
Jones, R.V., Carney, B.W., Storm, J., and Latham, D.W. 1991, preprint.Google Scholar
Lub, J. 1977, , .Google Scholar
VandenBerg, D.A., and Bell, R.A. 1985, Ap.J. Suppl. , 58, 561.Google Scholar