J/A+A/507/803 VI photometry of new M53 variables (Dekany+, 2009)
Study of globular cluster M53: new variables, distance, metallicity.
Dekany I., Kovacs G.
<Astron. Astrophys. 507, 803 (2009)>
=2009A&A...507..803D 2009A&A...507..803D
ADC_Keywords: Clusters, globular ; Stars, variable ; Photometry, VRI
Keywords: globular clusters: individual: M53 - methods: data analysis -
stars: variables: general - stars: variables: RR Lyr -
stars: oscillations - stars: abundances
Abstract:
We study the variable star content of the globular cluster M53 to
compute the physical parameters of the constituting stars and the
distance of the cluster. Covering two adjacent seasons in 2007 and
2008, new photometric data are gathered for 3048 objects in the field
of M53. By using the OIS (optimal image subtraction) method and
subsequently TFA (trend filtering algorithm), we search for variables
in the full sample by using discrete Fourier transformation and
box-fitting least squares method. We select variables based on the
statistics related to these methods combined with visual inspection.
We identified 12 new variables (2 RR Lyrae stars, 7 short periodic
stars - 3 of them are SX Phe stars - and 3 long-period variables). No
eclipsing binaries were found in the present sample. Except for the 3
(hitherto unknown) Blazhko RR Lyrae (two RRab and an RRc) stars, no
multiperiodic variables were found. We showed that after proper period
shift, the PLC (period-luminosity-color) relation for the first
overtone RR Lyrae sample tightly follows the one spanned by the
fundamental stars. Furthermore, the slope is in agreement with that
derived from other clusters. Based on the earlier Baade-Wesselink
calibration of the PLC relations, the derived reddening-free distance
modulus of M53 is 16.31±0.04mag, corresponding to a distance
modulus of 18.5mag for the Large Magellanic Cloud. From the Fourier
parameters of the RRab stars we obtained an average iron abundance of
-1.58±0.03 (error of the mean). This is ∼0.5dex higher than the
overall abundance of the giants as given in the literature and derived
in this paper from the three-color photometry of giants. We suspect
that the source of this discrepancy (observable also in other,
low-metallicity clusters) is the lack of a sufficient number of
low-metallicity objects in the calibrating sample of the Fourier
method.
Description:
Johnson V and Kron-Cousins I photometric time series of the variables
detected in our work and the Fourier decompositions of cluster RR
Lyrae stars with magnitude-transformed light curves in V band are
presented.
The file 'rrlvcoe.dat' contains the Fourier decompositions of the
TFA-filtered standard V light curves of 11 fundamental-mode and 13
first overtone mode RR Lyrae stars for which flux-to-magnitude
transformation was performed. Fourier parameters refer to a sine
decomposition defined by the following expression:
V(t) = A0 + A1*sin[2*{pi]*(t-t0)*1*f0+φ1]
+ A2*sin[2*{pi]*(t-t0)*2*f0+φ2] + ...
ID type period epoch A0 N sigma A M A_1 phi_1 ... A_M phi_M
Here 'ID' is the identification number of a star according to the
Catalog of Variable Stars in Globular Clusters (CVSGC, Clement et al.
2001AJ....122.2587C 2001AJ....122.2587C); 'type' has a value of 'RR0' or 'RR1' for
fundamental and first overtone pulsators, respectively; 'N' is the
number of the data points used in the calculation of the Fourier
decomposition; 'sigma' is the standard deviation of the residuals of
the fit; 'A' is the total amplitude of the light variation calculated
from the fitted Fourier sum; and 'M' is the order of the Fourier fit.
For RR0 stars, M=10, while M=3 for RR1 stars. In the case of RR1
stars table cells corresponding to Fourier terms higher than 3 are
filled with zero values.
Photometric time series of the M53 variable stars are given in the
following files:
'vXX.YZ.ext'
where 'XX' is a two-digit integer number corresponding to the
variable's name in the CVSGC (e.g., for variable V6, 'XX'='06'); the
value of 'Y' is 'v' or 'i', for V or I band data, respectively; the
value of 'Z' is 'r' or 'f', for raw (i.e., non-TFA) or TFA-filtered
data, respectively; and the value of 'ext' is either 'flx' or 'mag',
for data in differential flux units or standard magnitude units,
respectively. Note that TFA post-processing was done for the V data
only.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stars.dat 82 68 Properties of the RR Lyrae stars
rrlvcoe.dat 196 24 Fourier decompositions of cluster RR Lyrae stars
with magnitude-transformed light curves in V color
flux/* . 136 Individual raw differential flux curves
fluxtfa/* . 68 Individual TFA-processed differential flux curves
mag/* . 56 Individual V and I light curves
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See also:
J/AJ/109/269 : Photometry of NGC 5053 (Sarajedini+ 1995)
J/PAZh/23/454 : Identification and coordinates in M 53 (Evstigneeva+, 1997)
J/AJ/116/1775 : BV photometry of M53 (Rey+, 1998)
J/A+A/358/547 : M53 variable stars V light curves (Kopacki, 2000)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- ID Identification name, VNN
4 A1 --- n_ID [*] * for new detections
6- 10 A5 --- Type Variability type (1)
12- 13 I2 h RAh Right ascension (J2000)
15- 16 I2 min RAm Right ascension (J2000)
18- 21 F4.1 s RAs Right ascension (J2000)
23 A1 --- DE- Declination sign (J2000)
24- 25 I2 deg DEd Declination (J2000)
27- 28 I2 arcmin DEm Declination (J2000)
30- 33 F4.1 arcsec DEs Declination (J2000)
35- 39 F5.1 arcsec d Radial distance (2)
41- 50 F10.7 d Per ? Period
52- 53 I2 10-7d e_Per ? rms uncertainty on Per
55- 58 F4.1 --- SNR Signal-to-noise ratio (3)
60 A1 --- l_Vmag [~] Limit flag on Vmag
61- 66 F6.3 mag Vmag ? Average Johnson V magnitude (4)
68- 72 F5.3 mag V-Ic ? Average Johnson-Cousins V-I colour
index (4) (5)
74- 81 F8.5 d-1 Freq ? Frequency
--------------------------------------------------------------------------------
Note (1): Types as follows:
RRab = fundamental overtone
RRc = first overtone
RRabB = Blazhko variable
RRcB = Blazhko variable
sp = short period star
lp = long period variable
Note (2): The radial distance d is measured from the nominal cluster center
defined in Stetson's catalog of photometric standards (Stetson,
2000PASP..112..925S 2000PASP..112..925S; RA=13:12:55.26; DE=+18:10:09.8 [2000.0])
Note (3): Signal-to-noise ratio calculated in the [0.0,20]d-1 frequency
range for RR Lyrae (No V1-V72), [0.0,50]d-1 frequency range for
short period stars (No V73-V83)
Note (4): The V and V-I magnitude averages (i.e., the zero frequency
constant in their Fourier decompositions) are given in those cases in
which the flux-to-magnitude conversion was reliable.
Note (5): For variable V75, only instrumental V magnitude average is shown
because the star was saturated in the I band.
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Byte-by-byte Description of file: rrlvcoe.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- ID Star identification in CVSGC, VNN,
Cl* NGC 5024 GOR VNN in Simbad
5- 7 A3 --- Type RR Lyrae type (RR0 or RR1)
9- 17 F9.7 d Per Period
19- 27 F9.1 --- t0 Epoch of Fourier decomposition (1)
29- 35 F7.4 mag A0 Zero-frequency constant (magnitude average) (1)
37- 39 I3 --- N Number of data points
41- 46 F6.4 mag sigma Residual standard deviation
48- 53 F6.4 mag A Total amplitude
55- 56 I2 --- M Order of the Fourier decomposition
58- 63 F6.4 mag A1 A1 Fourier amplitude (1)
65- 70 F6.4 rad phi1 φ1 Fourier phase (1)
72- 77 F6.4 mag A2 A2 Fourier amplitude (1)
79- 84 F6.4 rad phi2 φ2 Fourier phase (1)
86- 91 F6.4 mag A3 A3 Fourier amplitude (1)
93- 98 F6.4 rad phi3 φ3 Fourier phase (1)
100-105 F6.4 mag A4 A4 Fourier amplitude (1)
107-112 F6.4 rad phi4 φ4 Fourier phase (1)
114-119 F6.4 mag A5 A5 Fourier amplitude (1)
121-126 F6.4 rad phi5 φ5 Fourier phase (1)
128-133 F6.4 mag A6 A6 Fourier amplitude (1)
135-140 F6.4 rad phi6 φ6 Fourier phase (1)
142-147 F6.4 mag A7 A7 Fourier amplitude (1)
149-154 F6.4 rad phi7 φ7 Fourier phase (1)
156-161 F6.4 mag A8 A8 Fourier amplitude (1)
163-168 F6.4 rad phi8 φ8 Fourier phase (1)
170-175 F6.4 mag A9 A9 Fourier amplitude (1)
177-182 F6.4 rad phi9 φ9 Fourier phase (1)
184-189 F6.4 mag A10 A10 Fourier amplitude (1)
191-196 F6.4 rad phi10 φ10 Fourier phase (1)
--------------------------------------------------------------------------------
Note (1): in Fourier decomposition (f0=1/Per):
V(t) = A0 + A1*sin[2*{pi]*(t-t0)*1*f0+φ1]
+ A2*sin[2*{pi]*(t-t0)*2*f0+φ2] + ...
--------------------------------------------------------------------------------
Byte-by-byte Description of file: flux/*
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.5 d HJD Heliocentric Julian Date
15- 24 F10.3 --- Flux Johnson V or Cousins I-band raw differential
flux (in ADU units)
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Byte-by-byte Description of file: fluxtfa/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.5 d HJD Heliocentric Julian Date
15- 24 F10.3 --- Flux Johnson V TFA-processed differential flux
(in ADU units)
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Byte-by-byte Description of file: mag/*
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.5 d HJD Heliocentric Julian Date
15- 21 F7.4 mag mag Johnson V or Cousins I-band standard magnitude
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Acknowledgements:
Istvan Dekany, dekany(at)konkoly.hu
(End) Istvan Dekany [Konkoly Obs., Hungary], Patricia Vannier [CDS] 24-Sep-2009