J/AJ/143/99 Photometry of W UMa eclipsing binaries (Terrell+, 2012)
A BVRcIc survey of W Ursae Majoris binaries.
Terrell D., Gross J., Cooney W.R.
<Astron. J., 143, 99 (2012)>
=2012AJ....143...99T 2012AJ....143...99T
ADC_Keywords: Binaries, eclipsing ; Photometry, UBVRI ; Reddening
Keywords: binaries: close - binaries: eclipsing
Abstract:
We report on a BVRcIc survey of field W Ursae Majoris (UMa) binary
stars and present accurate colors for 606 systems that have been
observed on at least three photometric nights from a robotic
observatory in southern Arizona. Comparison with earlier photometry
for a subset of the systems shows good agreement. We investigate two
independent methods of determining the interstellar reddening,
although both have limitations that can render them less effective
than desired. A subset of 101 systems shows good agreement between the
two reddening methods.
Description:
The survey began in 2005 with targets selected from the Pribulla et
al. (2003, Cat. V/119) catalog of 361 overcontact systems. Soon
thereafter, Gettel et al. (2006, Cat. J/AJ/131/621) published a catalog
of 1022 overcontact systems identified from
ROTSE-I (Akerlof et al., 2000, Cat. J/AJ/119/1901) sky patrol images.
The final list of observed targets came primarily from these two
catalogs, with two systems (GSC 0067-00348 and GSC 2545-00970) added
after we made follow-up observations of new discoveries. The last of
the observations reported herein were made in 2008.
Standardized photometry in Johnson-Cousins BVRcIc filters was
obtained for 606 known or suspected W UMa eclipsing binaries at the
Sonoita Research Observatory (SRO) in Arizona with a 0.35m
Schmidt-Cassegrain telescope (table 1). We can achieve photometric
precisions of 0.01mag at 14th magnitude with reasonable integration
times.
Estimates of the interstellar reddening were made with the color
difference method and by using the neutral hydrogen column density
along the line of sight to the stars. A subset of 101 systems
(table 2) in the survey shows good agreement between the two methods.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 106 606 The BVRcIc colors of 606 W Ursae Majoris binaries
table2.dat 32 101 Reddening estimates for the 101 systems showing a
maximum difference of 0.02mag in E(B-V) between
the color difference method and the NH1 method
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See also:
B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013)
V/119 : Catalogue of field contact binary stars (Pribulla+, 2003)
J/AJ/131/621 : A catalog of 1022 bright contact binary stars (Gettel+, 2006)
J/MNRAS/357/497 : Kinematics of W UMa-type binaries (Bilir+, 2005)
J/AJ/119/1901 : ROTSE all-sky surveys for variable stars (Akerlof+, 2000)
J/A+A/311/523 : Photometry of W UMa (Maceroni+, 1996)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- ID Star identification (1)
16- 23 F8.4 deg RAdeg Right ascension in decimal degrees (J2000) (2)
25- 32 F8.4 deg DEdeg Declination in decimal degrees (J2000) (2)
34- 43 F10.8 d Period Orbital period of the binary (3)
45- 46 I2 --- o_ID [3/54] Number of observations
48- 52 F5.3 mag B-V The measured (B-V) color index
54- 58 F5.3 mag e_B-V Error in B-V (4)
60- 64 F5.3 mag V-Rc The measured (V-Rc) color index
66- 70 F5.3 mag e_V-Rc Error in V-Rc (4)
72- 76 F5.3 mag Rc-Ic The measured (Rc-Ic) color index
78- 82 F5.3 mag e_Rc-Ic Error in Rc-Ic (4)
84- 88 F5.3 mag V-Ic The (V-Ic) color index (5)
90- 94 F5.3 mag e_V-Ic Error in V-Ic (4)
96-100 F5.2 mag Vmax [8.9/13] V magnitude at maximum brightness (3)
102-106 F5.2 mag Vmin [9.2/13.8] V magnitude at minimum brightness (3)
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Note (1): General Catalogue of Variable Stars (Cat. B/gcvs) designation, if
known, or the designation given in Gettel et al. (2006, Cat.
J/AJ/131/621, <[GGM2006] NNNNNNNN> in Simbad).
Note (2): Taken from either Pitbulla et al. (2003, Cat. V/119) or Gettel
et al. (2006, Cat. J/AJ/131/621). In a handful of cases, the positions
are from astrometry of our images where the positions from Gettel
et al. (2006, Cat. J/AJ/131/621) were ambiguous due to blending.
Note (3): Taken from either Pitbulla et al. (2003, Cat. V/119) or Gettel
et al. (2006, Cat. J/AJ/131/621).
Note (4): The errors given are the standard deviations of the individual
measurements, and these include both the measurement errors and any
intrinsic color changes in the stars, which we assume to be small.
Note (5): The (V-Ic) color is formed as the sum of (V-Rc) and (Rc-Ic).
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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- 14 A14 --- ID Star identification
16- 20 F5.3 mag E(B-V)0 Reddening produced with the Color Difference
method
22- 26 F5.3 mag e_E(B-V)0 Uncertainty on E(B-V)0
28- 32 F5.3 mag E(B-V)1 Reddening produced with the NH1 method (2)
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Note (2): The NH1 method uses the neutral hydrogen column density along the
line of sight to the stars (see Section 5).
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History:
* 31-May-2013: From electronic version of the journal
* 10-Oct-2013: Tables 1 and 2 corrected to switch GSC 67-34 for the right
identification: GSC 67-348.
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 31-May-2013