J/ApJS/255/1 Morphology of OGLE LCs of Eclipsing binaries (Bodi+, 2021)
Classification of OGLE eclipsing binary stars based on their morphology type
with locally linear embedding.
Bodi A., Hajdu T.
<Astrophys. J. Suppl. Ser., 255, 1-1 (2021)>
=2021ApJS..255....1B 2021ApJS..255....1B (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing; Photometry; Magellanic Clouds; Milky Way;
Optical
Keywords: Eclipsing binary stars; Astronomy data analysis; Astronomy databases
Abstract:
The Optical Gravitational Lensing Experiment (OGLE) continuously
monitors hundreds of thousands of eclipsing binaries in the Galactic
bulge field and the Magellanic Clouds. These objects have been
classified into major morphological subclasses, such as contact,
noncontact, ellipsoidal, and cataclysmic variables, both by matching
the light curves with predefined templates and by visual inspections.
Here we present the result of a machine-learned automatic
classification based on the morphology of light curves inspired by the
classification of eclipsing binaries observed by the original Kepler
mission. We similarly use a dimensionality reduction technique with
locally linear embedding to map the high dimension of the data set
into a low-dimensional embedding parameter space, while keeping the
local geometry and the similarities of the neighboring data points.
After three consecutive steps, we assign one parameter to each binary
star, which scales well with the "detachness," i.e., the sum of the
relative radii of the components. This value is in good agreement with
the morphology types listed in the OGLE catalog and, along with the
orbital periods, can be used to filter any morphological subtypes
based on the similarity of light curves. Our open-source pipeline can
be applied in a fully automatic way to any other large data set to
classify binary stars.
Description:
We downloaded all OGLE-IV I-band eclipsing binary light curves
obtained in the Galactic bulge field and the Magellanic Clouds from
the OGLE database (http://www.astrouw.edu.pl/ogle/). If needed, we
complemented the data set with OGLE-III light curves.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 54 498268 OGLE eclipsing binaries in the field of Galactic
bulge, Large-, and Small Magellanic Clouds
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See also:
J/AJ/121/254 : Eclipsing Binaries in OGLE (Rucinski+, 2001)
J/AcA/53/1 : OGLE eclipsing binaries in LMC (Wyrzykowski+, 2003)
J/AcA/54/1 : OGLE II SMC eclipsing binaries (Wyrzykowski+, 2004)
J/A+A/439/559 : OGLE eclipsing binaries (bulge+lmc+smc) (Groenewegen+, 2005)
J/A+A/494/739 : Automatic classification of OGLE variables (Sarro+, 2009)
J/AcA/61/103 : VI light curves of LMC eclipsing binaries (Graczyk+, 2011)
J/AcA/63/115 : OGLE-III Galactic disk eclipsing binaries (Pietrukowicz+, 2013)
J/AcA/63/323 : OGLE-III SMC eclipsing binary stars (Pawlak+, 2013)
J/MNRAS/443/432 : Eclipsing binaries in LMC (Muraveva+, 2014)
J/MNRAS/448/946 : Kepler eclipse timing variation analyses (Borkovits+, 2015)
J/MNRAS/455/4136 : Kepler triples (Borkovits+, 2016)
J/MNRAS/456/2260 : K2 Variability Catalogue II (Armstrong+, 2016)
J/AJ/151/68 : Kepler Mission. VII. Eclipsing binaries in DR3 (Kirk+, 2016)
J/A+A/590/A85 : Massive LMC eclipsing binaries minima timings (Zasche+, 2016)
J/AcA/66/405 : Galactic bulge eclipsing & ellipsoidal bin. (Soszynski+, 2016)
J/AcA/66/421 : Eclipsing binaries in the Magellanic System (Pawlak+, 2016)
J/A+A/606/A92 : Gaia LMC eclipsing binary and multiple systems (Mowlavi+, 2017)
http://www.astrouw.edu.pl/ogle/ : OGLE online data
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- Field Field: LMC, SMC or BLG (Bulge)
5- 23 A19 --- Star Star's ID (1)
25- 35 F11.5 d T0 [1006.16/10866.52] Time of minimum brightness,
Heliocentric Julian Date; HJD-2450000
37- 48 F12.7 d Per [0.05/4198] Fine-tuned orbital periods
50- 54 F5.3 --- Class [0/1] Morphology classification parameter, c (2)
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Note (1): IDs of bulge and Magellanic Cloud objects are taken from
Soszynski+ (2016, J/AcA/66/405) and Pawlak+ (2016, J/AcA/66/421),
respectively.
Note (2): The morphology parameter c scales with the "detachness" of the
eclipses. The "detachness" is a measure of the sum of the relative
radii of the components, thus it can be used as an indicator.
It is not easy to put strict limits between the classes, but we can
see that the range of c≤0.5 is dominated by detached binaries, the
semidetached systems lie between 0.5<c≤0.7, and above c∼0.7 the light
curves become more sinusoidal, where the ellipsoidal and overcontact
systems can be found.
See Section 3.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 25-Oct-2021