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J/other/ApSS/361.175 M5 RR Lyr and HB VI light curves (Arellano Ferro+, 2016)
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Beginning of ReadMe :J/other/ApSS/361.175 M5 RR Lyr and HB VI light curves (Arellano Ferro+, 2016)
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RR Lyrae stars and the horizontal branch of NGC 5904 (M5).
Arellano Ferro A., Luna A., Bramich D.M., Giridhar S., Ahumada, J.H.,
Muneer S.
<Astrophys. Space Sci. 361, 175 (2016)>
=2016Ap&SS.361..175A (SIMBAD/NED BibCode)
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ADC_Keywords: Clusters, globular ; Stars, variable ; Photometry
Keywords: globular clusters: individual (NGC 5904) -
stars: variables: RR Lyrae, SX Phe, SR
Abstract:
We report the distance and [Fe/H] value for the globular cluster
NGC 5904 (M5) derived from the Fourier decomposition of the light
curves of selected RRab and RRc stars. The aim in doing this was to
bring these parameters into the homogeneous scales established by our
previous work on numerous other globular clusters, allowing a direct
comparison of the horizontal branch luminosity in clusters with a wide
range of metallicities. Our CCD photometry of the large variable star
population of this cluster is used to discuss light curve
peculiarities, like Blazhko modulations, on an individual basis. New
Blazhko variables are reported. From the RRab stars we found
[Fe/H]UVES=-1.335+/-0.003(statistical)+/-0.110(systematic), and a
distance of 7.6+/-0.2kpc, and from the RRc stars we found
[Fe/H]UVES=-1.39+/-0.03(statistical)+/-0.12(systematic) and a
distance of 7.5+/-0.3kpc. The results for RRab and RRc stars should
be considered independent since they come from different calibrations
and zero points. Absolute magnitudes, radii and masses are also
reported for individual RR Lyrae stars. The distance to the cluster
was also calculated by alternative methods like the Period-Luminosity
relation of SX Phe and the luminosity of the stars at the tip of the
red giant branch, and we obtained the results 7.7+/-0.4 and 7.2-7.5kpc
respectively. The distribution of RR Lyrae stars in the instability
strip is discussed and compared with other clusters in connection with
the Oosterhoff and horizontal branch type. The Oosterhoff type II
clusters systematically show a RRab-RRc segregation about the
instability strip first-overtone red edge, while the Oosterhoff type I
clusters may or may not display this feature. A group of RR Lyrae
stars is identified in an advanced evolutionary stage, and two of them
are likely binaries with unseen companions.
Description:
VI time-series photometry of all variable stars in M5 observed in this
work including the recently discovered variables (V170-V181) by
Arellano Ferro et al., 2015IBVS.6137....1A, Cat. J/other/IBVS/6137.