RR Lyrae stars and the horizontal branch of NGC 5904 (M5)

• Published in: Astrophysics and space science 2016-05, Vol.361 (5), p.1, Article 175
• Main Authors: Arellano Ferro, A., Luna, A., Bramich, D. M., Giridhar, Sunetra, Ahumada, J. A., Muneer, S.
• Format: Article
• Language: English
• Subjects: Astrobiology; Astronomy; Astrophysics; Astrophysics and Astroparticles; Cosmology; Observations and Techniques; Original Article; Physics; Physics and Astronomy; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Star & galaxy formation; Stars & galaxies
• ISSN: 0004-640X; 1572-946X
• DOI: 10.1007/s10509-016-2757-5

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 ± 0.2  kpc , and from the RRc stars we found [ Fe / H ] UVES = − 1.39 ± 0.03  (statistical) ± 0.12  (systematic) and a distance of 7.5 ± 0.3  kpc . 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 7.2–7.5 kpc 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.