J/ApJS/273/31 Contact binaries from CSS DR2 (Wang+, 2024)
A method of rapidly deriving late-type contact binary parameters and its
application in the Catalina Sky Survey.
Wang J., Ding Xu, Li J., Xiong J., Cheng Q., Ji K.
<Astrophys. J. Suppl. Ser., 273, 31 (2024)>
=2024ApJS..273...31W 2024ApJS..273...31W
ADC_Keywords: Binaries, eclipsing; Models; Surveys; Effective temperatures;
Stars, diameters; Optical
Keywords: Astronomy data analysis ; Eclipsing binary stars ;
Contact binary stars
Abstract:
With the continuous development of large optical surveys, a large
number of light curves of late-type contact binary systems (CBs) have
been released. Deriving parameters for CBs using the the
Wilson-Devinney program and the PHOEBE program poses a challenge.
Therefore, this study developed a method for rapidly deriving light
curves based on the Neural Networks model combined with the
Hamiltonian Monte Carlo (HMC) algorithm (NNHMC). The neural network
was employed to establish the mapping relationship between the
parameters and the pregenerated light curves by the PHOEBE program,
and the HMC algorithm was used to obtain the posterior distribution of
the parameters. The NNHMC method was applied to a large contact binary
sample from the Catalina Sky Survey, and a total of 19104 late-type
contact binary parameters were derived. Among them, 5172 have an
inclination greater than 70° and a temperature difference less
than 400K. The obtained results were compared with the previous
studies for 30 CBs, and there was an essentially consistent goodness-
of-fit (R2) distribution between them. The NNHMC method possesses the
capability to simultaneously derive parameters for a vast number of
targets. Furthermore, it can provide an extremely efficient tool for
the rapid derivation of parameters in future sky surveys involving
large samples of CBs.
Description:
This article's experimental samples were selected from the Catalina
Sky Survey (CSS) DR2 (Drake+ 2014, J/ApJS/213/9). The CSS began in
2004, covering the sky between decl. -75° to +65° using three
telescopes. To maximize throughput, all observation results were
unfiltered, and the data was then transformed to the V band.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 163 5172 Contact binary system (CB) catalog
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See also:
J/ApJ/629/1055 : Evolution of close binary systems (Yakut+, 2005)
J/ApJ/723/1469 : Flux calibrations and WZ Oph photometry (Wilson+, 2010)
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/MNRAS/430/2029 : Initial masses of W UMa type contact bin. (Yildiz+, 2013)
J/ApJS/213/9 : Catalina Surveys periodic variable stars (Drake+, 2014)
J/MNRAS/465/4678 : 9380 contact binaries from CRTS VSC (Marsh+, 2017)
J/A+A/616/A10 : Open clusters GaiaDR2 HR diagrams (Gaia Collaboration, 2018)
J/AJ/156/241 : Variable stars measured by ATLAS (Heinze+, 2018)
J/ApJS/247/50 : Late-type contact binaries in CSS DR1 (Sun+, 2020)
J/ApJS/254/10 : Compilation of W UMa stars (Latkovic+, 2021)
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 CSS identifier (JHHMMSS.s+DDMMSS)
22- 30 F9.5 deg RAdeg Right Ascension (J2000)
32- 40 F9.5 deg DEdeg [-20/70] Declination (J2000)
42- 49 F8.6 d Period [0.1/9.7] Orbital period
51- 57 F7.2 K T1init [3536/8440] Primary initial effective
temperature (1)
59- 65 F7.2 K Teff1 [3702/8057] Primary effective temperature
67- 72 F6.2 K e_Teff1 [146/322] Uncertainty in Teff1
74- 78 F5.2 deg inc [70/89.6] Inclination angle
80- 84 F5.2 deg e_inc [0.3/16.1] Uncertainty in inc
86- 89 F4.2 --- q [0.02/0.96] Mass ratio; M2/M1
91- 94 F4.2 --- e_q [0.01/0.4] Uncertainty in q
96- 100 F5.3 --- T2/T1 [0.9/1.1] Temperature ratio
102- 106 F5.3 --- e_T2/T1 [0.003/0.1] Uncertainty in T2/T1
108- 111 F4.2 --- f [0.01/1] Fill-out factor (2)
113- 116 F4.2 --- e_f [0.01/0.3] Uncertainty in f
118- 121 F4.2 --- Omega [1.67/3.7] Surface potential where
Ω=Ω1=Ω2
123- 126 F4.2 --- e_Omega [0.01/0.2] Uncertainty in Omega
128- 131 F4.2 Rsun r1 [0.39/0.7] Primary radius
133- 136 F4.2 Rsun e_r1 [0.01/0.1] Uncertainty in r1
138- 142 F5.3 Rsun r2 [0.6/0.99] Secondary radius
144- 147 F4.2 Rsun e_r2 [0.01/0.04] Uncertainty in r2
149- 152 F4.2 --- L2/L1 [0/1.3] Luminosity ratio
154- 157 F4.2 --- e_L2/L1 [0.01/0.05] Uncertainty in L2/L1
159- 163 F5.3 --- R2 [0.6/0.99] Goodness of fit, R2
(closer to 1=the better)
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Note (1): Initial effective temperature of primary star from Gaia DR2.
Note (2): Fill-out factor f=(Ω-Ωin)/(Ωout-Ωin),
where Ωin and Ωout are the modified potential
of the inner and the outer Lagrangian points, respectively.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 08-Jan-2025