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J/other/ApSS/361.175    M5 RR Lyr and HB VI light curves (Arellano Ferro+, 2016)

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)
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. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 88 134 General data for all of the variables in M5 in the FoV of our images table2.dat 94 102078 Time-series V and I photometry for all variable stars discussed in this paper
See also: J/other/IBVS/6137 : New variables in M5 (NGC 5904) (Arellano Ferro+, 2015) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 A4 --- VName Variable star ID 6- 12 A7 --- VType Variable type (1) 13 A1 --- n_VType [bd] Note on Vtype (2) 17 A1 --- l_Vmag Limit flag on Vmag 18- 23 F6.3 mag Vmag Mean V magnitude 25 A1 --- l_Imag Limit flag on Imag 26- 31 F6.3 mag Imag Mean I magnitude 33- 36 F4.2 mag AV ?=- Amplitude in V band (3) 38- 41 F4.2 mag AI ?=- Amplitude in I band (3) 43- 53 F11.7 d Per ?=- Period (this work) 54 A1 --- n_Per [c] Note on Per (4) 56- 64 F9.4 d HJDmax ?=- Date of maximum brightness (HJD-2450000) 66- 67 I2 h RAh Right ascension (J2000.0) 69- 70 I2 min RAm Right ascension (J2000.0) 72- 76 F5.2 s RAs Right ascension (J2000.0) 78 A1 --- DE- Declination sign (J2000.0) 79- 80 I2 deg DEd Declination (J2000.0) 82- 83 I2 arcmin DEm Declination (J2000.0) 85- 88 F4.1 arcsec DEs Declination (J2000.0)
Note (1): All variable types follow the designations from the General Catalogue of Variable Stars (Samus et al., 2009, Cat. B/gcvs). Or see also the AAVSO link http://www.aavso.org/vsx/help/VariableStarTypeDesignationsInVSX.pdf All variables with Blazhko modulations are labelled 'Bl'. Note (2): Note on Vtype as follows: b = Blazhko variations identified by Jurcsik et al. (2011MNRAS.411.1763J). d = Classification based on the light curve of Drissen and Shara (1998AJ....115..725D). Note (3): Amplitudes for Blazhko variables correspond to the maximum observed. Note (4): Note on Per as follows: c = Adopted from Szeidl et al. (2011, Cat. J/MNRAS/411/1744).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 A4 --- VName Variable name, VNN (V1-V181) 7 A1 --- Filter [VI] Observation filter ("V" or "I") 10- 22 F13.5 d HJD Heliocentric Julian date 25- 30 F6.3 mag magst [10/23] Standard magnitude 33- 38 F6.3 mag maginst Instrumental magnitude 41- 45 F5.3 mag e_maginst Error on the magnitude 48- 57 F10.3 s-1 Fref Reference flux (in ADU/s) 60- 65 F6.3 s-1 e_Fref Error on the reference flux (in ADU/s) 67- 77 F11.3 s-1 Fdiff ?=- Differential flux (in ADU/s) 80- 86 F7.3 s-1 e_Fdiff Error on the differential flux (in ADU/s) 89- 94 F6.4 --- p Photometric scale factor
Acknowledgements: Armando Arellano Ferro, armando(at)astro.unam.mx History: 09-May-2016: Firts on-line version 31-May-2016: table2 corrected (from author)
(End) Armando Arelano Ferro [IA-UNAM Mexico], Patricia Vannier [CDS] 06-May-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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