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 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 2015IBVS.6137....1A, Cat. J/other/IBVS/6137.
File Summary:
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FileName Lrecl Records Explanations
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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
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See also:
J/other/IBVS/6137 : New variables in M5 (NGC 5904) (Arellano Ferro+, 2015)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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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)
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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 2011MNRAS.411.1763J).
d = Classification based on the light curve of Drissen and Shara
(1998AJ....115..725D 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).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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
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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