J/ApJS/247/50 Late-type contact binaries in CSS DR1 (Sun+, 2020)
Physical parameters of late-type contact binaries in the northern Catalina Sky
Survey.
Sun W., Chen X., Deng L., de Grijs R.
<Astrophys. J. Suppl. Ser., 247, 50 (2020)>
=2020ApJS..247...50S 2020ApJS..247...50S
ADC_Keywords: Binaries, eclipsing; Stars, masses ; Effective temperatures ;
Stars, diameters; Optical
Keywords: Astronomy data analysis ; contact binary stars ;
fundamental parameters of stars
Abstract:
We present the physical parameters of 2335 late-type contact binary
(CB) systems extracted from the Catalina Sky Survey (CSS). Our sample
was selected from the CSS Data Release 1 by strictly limiting the
prevailing temperature uncertainties and light-curve fitting
residuals, allowing us to almost eliminate any possible contaminants.
We developed an automatic Wilson-Devinney-type code to derive the
relative properties of CBs based on their light-curve morphology. By
adopting the distances derived from CB (orbital) period-luminosity
relations (PLRs), combined with the well-defined mass-luminosity
relation for the systems' primary stars and assuming solar
metallicity, we calculated the objects' masses, radii, and
luminosities. Our sample of fully eclipsing CBs contains 1530 W-, 710
A-, and 95 B-type CBs. A comparison with literature data and with the
results from different surveys confirms the accuracy and coherence of
our measurements. The period distributions of the various CB subtypes
are different, hinting at a possible evolutionary sequence. W-type CBs
are clearly located in a strip in the total mass versus mass-ratio
plane, while A-type CBs may exhibit a slightly different dependence.
There are no significant differences among the PLRs of A- and W-type
CBs, but the PLR zero-points are affected by their mass ratios and
fill-out factors. Determination of zero-point differences for
different types of CBs may help us improve the accuracy of the
resulting PLRs. We demonstrate that automated approaches to deriving
CB properties could be a powerful tool for application to the much
larger CB samples expected to result from future surveys.
Description:
We used contact binary (CB) data from the Catalina Sky Survey (CSS)
Data Release 1 (CSDR1; Drake+ 2014, J/ApJS/213/9). The survey used
three telescopes to cover the sky between declinations DEC=-75°
and +70° at Galactic latitudes |b|>15°.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 209 2335 Total-eclipsing contact binary (CB) catalog
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See also:
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
V/119 : Catalogue of field contact binary stars (Pribulla+, 2003)
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
J/AJ/106/2096 : Limb-darkening coefficients in binaries (Van Hamme 1993)
J/A+A/311/523 : Photometry of W UMa (Maceroni+, 1996)
J/A+A/426/1001 : Catalog of contact binary stars (Csizmadia+, 2004)
J/ApJ/629/1055 : Evolution of close binary systems (Yakut+, 2005)
J/MNRAS/373/1483 : W UMa type and CAB stars dynamical evolution (Eker+, 2006)
J/AJ/131/621 : Catalog of 1022 bright contact binary stars (Gettel+, 2006)
J/A+A/528/A90 : SuperWASP short period eclipsing binaries (Norton+, 2011)
J/ApJ/763/32 : Galactic halo RRab stars from CSS (Drake+, 2013)
J/AJ/146/101 : LINEAR. III. Periodic variables (Palaversa+, 2013)
J/ApJS/208/9 : Intrinsic colors & temperatures of PMS stars (Pecaut+, 2013)
J/MNRAS/430/2029 : Initial masses of W UMa contact binaries (Yildiz+, 2013)
J/ApJS/213/9 : Catalina Surveys periodic variable stars (Drake+, 2014)
J/AJ/148/81 : APASS BVgri photometry of RAVE stars. I. (Munari+, 2014)
J/MNRAS/446/2251 : Southern Catalina Survey type-ab RR Lyrae (Torrealba+, 2015)
J/AJ/152/129 : VR photometry for 914 stars in NGC 188 (Chen+, 2016)
J/MNRAS/465/4678 : 9380 contact binaries from CRTS VSC (Marsh+, 2017)
J/ApJ/859/140 : Multi-band magnitudes for W UMa EB* candidates (Chen+, 2018)
J/ApJS/237/28 : WISE catalog of periodic variable stars (Chen+, 2018)
J/AJ/156/241 : A first cat. of var. stars measured by ATLAS (Heinze+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [CSS_]
5- 20 A16 --- CRTS Catalina Sky Survey (CSS) identifier
(JHHMMSS.s+DDMMSS)
22- 30 F9.5 deg RAdeg Right Ascension (J2000)
32- 40 F9.5 deg DEdeg [-19.7/70.1] Declination (J2000)
42- 48 F7.5 d Period [0.196/0.56] Orbital period
50- 57 F8.2 K Teff1 [3436/15530] Primary effective temperature (1)
59- 66 F8.2 K Teff2 [3520/11079] Secondary effective
temperature (1)
68- 74 F7.2 K e_Teff1 [8/4226]? Uncertainty in Teff1 (1)
76- 82 F7.2 K e_Teff2 [13/3290]? Uncertainty in Teff2 (1)
84- 88 F5.2 deg inc [70/90] Inclination angle
90- 94 F5.2 deg e_inc [0.1/22.2] Uncertainty in inc
96-100 F5.2 --- Omega [1.8/15] Surface potential
(Ω=Ω1=Ω2)
102-105 F4.2 --- e_Omega [0/0.8] Uncertainty in Omega
107-110 F4.2 --- q [0.07/0.8] Mass ratio; M2/M1
112-115 F4.2 --- e_q [0.09] Uncertainty in q
117-121 F5.2 --- f [-1/1] Fill-out factor (2)
123-126 F4.2 --- e_f [0.01/4.1] Uncertainty in f
128-131 F4.2 --- LFrac [0.4/1] Primary to total V band luminosity
ratio
133-136 F4.2 --- e_LFrac [0/0.4] Uncertainty in LFrac
138 A1 --- OT CB classification (1530 W-, 710 A-, and
95 B-type CBs)
140-143 F4.2 Msun M1 [0.8/2.5] Primary mass
145-148 F4.2 Msun M2 [0.08/1.4] Secondary mass
150-153 F4.2 Msun e_M1 [0.02/0.1] Uncertainty in M1
155-158 F4.2 Msun e_M2 [0.07/0.3] Uncertainty in M2
160-163 F4.2 Rsun r1 [0.7/2.2] Primary radius
165-168 F4.2 Rsun r2 [0.3/1.5] Secondary radius
170-173 F4.2 Rsun e_r1 [0.02/0.07] Uncertainty in r1
175-178 F4.2 Rsun e_r2 [0.01/0.03] Uncertainty in r2
180-184 F5.2 Lsun L1 [0.3/26.8] Primary luminosity
186-189 F4.2 Lsun L2 [0.05/9.2] Secondary luminosity
191-194 F4.2 Lsun e_L1 [0.08/6.4] Uncertainty in L1
196-199 F4.2 Lsun e_L2 [0.02/4.6] Uncertainty in L2
201-204 F4.2 Rsun a [1.5/4.2] Semi-major axis
206-209 F4.2 Rsun e_a [0.03/0.1] Uncertainty in a
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Note (1): Temperatures without uncertainty estimates were derived using the
photometric method described in Section 3.1, while values with
uncertainties were obtained from the Wilson-Devinney-type (W-D;
Wilson & Devinney 1971ApJ...166..605W 1971ApJ...166..605W & Wilson 1979ApJ...234.1054W 1979ApJ...234.1054W) code.
Note (2): Fill-out factor f=(Ω-Ωo)/(Ωi-Ωo),
where Ωi and Ωo are the inner and outer Lagrangian
surface potential values, respectively.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 10-Jun-2020