J/MNRAS/520/2386 Extra-physics in ASAS-SN EBs and variables (Rowan+, 2023)
The value-added catalogue of ASAS-SN eclipsing binaries.
II. Properties of extra-physics systems.
Rowan D.M., Jayasinghe T., Stanek K.Z., Kochanek C.S., Thompson T.A.,
Shappee B.J., Holoien T.W.-S., Prieto J.L., Giles W.
<Mon. Not. R. Astron. Soc. 520, 2386-2404 (2023)>
=2023MNRAS.520.2386R 2023MNRAS.520.2386R (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Photometry ; Stars, variable ; Optical ;
Extinction ; Stars, distances ; Magnitudes, absolute ;
References ; Cross identifications ; X-ray sources
Keywords: surveys - binaries: eclipsing
Abstract:
Detached eclipsing binaries are the primary tool used to measure
precise masses and radii of stars. In our previous paper estimating
the parameters of more than 30000 detached eclipsing binaries, we
identified 766 eclipsing binaries with additional features in their
All-Sky Automated Survey for Supernovae (ASAS-SN) and Transiting
Exoplanet Survey Satellite light curves. Here, we characterize these
'extra-physics' systems, identifying eclipsing binaries with spotted
stars, pulsating components, and candidate triple/quadruple systems.
We use the Gaia, Asteroid Terrestrial-impact Last Alert System
(ATLAS), Zwicky Transient Facility (ZTF), and ASAS-SN variable star
catalogues to search for possible blends. We use MIST (MESA Isochrones
and Stellar Tracks) isochrones and evolutionary tracks to identify
systems with main-sequence, subgiant, and giant primaries and
highlight systems in sparsely populated regions of the
colour-magnitude diagram. We find that the orbital period distribution
of spotted binaries is divided by evolutionary state and find 68 with
X-ray detections. For the candidate triple/quadruples and pulsating
systems, we calculate the extra orbital/pulsational period and
identify systems with resonances. Finally, we highlight a number of
exotic systems, including eclipsing cataclysmic variables, subdwarfs,
and binaries with discs.
Description:
Machine learning techniques are almost always used to classify
variable stars, including eclipsing binaries. However, the detection
of unusual subclasses of systems, like pulsating eclipsing binaries or
doubly eclipsing binaries, is still often done through visual
inspection. In Rowan et al. (2022MNRAS.517.2190R 2022MNRAS.517.2190R, Cat. J/MNRAS/517/2190),
we visually inspected more than 40000 eclipsing binary light curves
from the ASAS-SN and TESS surveys to verify our eclipsing binary
models. In the process, we also identified 766 systems that could not
be described by simple models of eclipsing binaries due to the
presence of spots, pulsations, or additional eclipses. Here, we
present the ASAS-SN V-, ASAS-SN g-, and TESS T-band light curves and
discuss the properties of these 766 eclipsing binaries with
extra-physics.
We used phoebe a tool for modelling eclipsing binaries of all
morphological classes, to fit the ASAS-SN light curves. We started by
using an analytical geometry and the eclipsing binaries via artificial
intelligence. We then visually inspected all the models to identify
systems that required additional optimization. As a part of this
process, we downloaded the TESS light curves. We use the 'raw' light
curves rather than the detrended light curves since the detrending
procedure can often remove real stellar variability. We folded the
TESS light curves at the period calculated from the ASAS-SN light
curves and identified 766 targets that showed additional features in
the ASAS-SN or TESS light curves. We present extra-physics classes,
periods, astrometric and physical informations of our targets in
extrap.dat. More, we attached individual light curves for all our
extrap.dat sources.
Next, with a help of ATLAS r1 proximity statistic, we expect to find
multiple matches to variability catalogues for a single source by
cross-matching our catalogue with the GDR3, ZTF, ATLAS and ASAS-SN. We
give associated identifiers, angular separations, magnitudes of the
130 cross-matched sources in crmatch.dat.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
extrap.dat 753 766 Astrometric and physical informations of our
ASAS-SN extra-physics variables sample
crmatch.dat 181 130 Cross-matches of extra-physics targets to Gaia,
ZTF, and ATLAS with a radius of 21 arcsec
lcs/* . 766 The individual ASAS-SN/TESS time-series
photometry (with file names ID.dat)
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See also:
J/MNRAS/517/2190 : Physical properties of ∼30000 ASAS-SN EBs (Rowan+, 2022)
J/MNRAS/507/104 : Ellipsoidal variables in ASAS-SN catalog (Rowan+, 2021)
J/MNRAS/503/3975 : Var., period. and contact binaries in WISE (Petrosky+, 2021)
J/MNRAS/370/2013 : Catalogue of close binaries (Soydugan+, 2006)
J/ApJ/867/105 : ATLAS all-sky stellar ref. catalog, ATLAS-REFCAT2
(Tonry+, 2018)
J/A+A/664/A96 : Multiply eclipsing candidates from TESS satellite
(Zasche+, 2022)
J/A+A/640/A36 : OB stars TESS phot. & high-resolution spectroscopy
(Bowman+, 2020)
J/A+A/635/A193 : Catalogue of hot subdwarf stars DR2 (Geier, 2020)
J/A+A/606/A92 : Gaia LMC eclipsing binary and multiple systems
(Mowlavi+, 2017)
J/A+A/560/A4 : Rotation periods of active Kepler stars (Reinhold+, 2013)
J/A+A/453/635 : Modelling the Galactic Interstellar Extinction
(Marshall+, 2006)
J/ApJS/259/50 : EA-type eclipsing binaries observed by TESS (Shi+, 2022)
J/ApJS/259/66 : Eclipsing quadruple star candidates from TESS (Kostov+,2022)
J/ApJS/258/16 : TESS Eclipsing Binary stars. I. Sectors 1-26 (Prsa+, 2022)
J/ApJS/258/26 : Spectroscopic binaries from LAMOST MRS. I. (Zhang+, 2022)
J/ApJS/249/18 : The ZTF catalog of periodic variable stars (Chen+, 2020)
J/ApJS/237/28 : WISE catalog of periodic variable stars (Chen+, 2018)
J/AJ/154/250 : Kepler EB classifications and rotation periods (Lurie+,2017)
J/AcA/66/421 : Eclipsing binaries in the Magellanic System (Pawlak+, 2016)
J/AcA/65/297 : OGLE4 LMC and SMC Cepheids (Soszynski+, 2015)
J/AcA/63/323 : OGLE-III SMC eclipsing binary stars (Pawlak+, 2013)
J/AcA/61/217 : VI light curves of SMC long-period variables
(Soszynski+, 2011)
IX/61 : 4XMM-DR9s serendipitous source catalogue from stacks
(Traulsen+, 2020)
V/110 : Catalog of Cataclysmic Variables (Downes+ 2001)
II/340 : XMM-OM Serendipitous Source Survey Catalogue (XMM-SUSS2.1)
(Page+ 2014)
II/339 : Swift/UVOT Serendipitous Source Catalog (Yershov, 2015)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
B/cb : Cataclysmic Binaries, LMXBs, and related objects
(Ritter+, 2004)
B/sb9 : SB9: 9th Catalogue of Spectroscopic Binary Orbits
(Pourbaix+ 2004-2014)
Byte-by-byte Description of file: extrap.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- ID ASAS-SN ID used to match with light curve
(id)
21- 48 A28 --- ASASSN-V ASAS-SN V-band catalog designation
(asassn_name)
50- 68 I19 --- GaiaDR3 Gaia DR3 Source identifier (source)
70- 79 I10 --- TIC TESS Input Catalog v8.2 identifier (TIC)
81-100 F20.16 deg RAdeg Right ascension (J2000) (RA_ICRS)
102-121 F20.16 deg DEdeg Declination (J2000) (DE_ICRS)
123-142 F20.17 d Per Orbital period (period)
144-163 F20.17 d P2 ? The given second
orbital/pulsational/rotational period (p2)
165-166 I2 --- f_P2 Method of subtraction method used to
determine period P2 in section 3.2 Extra
eclipses (p2methodi)
168-185 A18 --- Group Type of extra-physics variability (group) (1)
187-191 A5 --- f_TIC True if TESS QLP or SPOC light curve are
available at 2022 October for 734 sources
(has_tess)
193-260 A68 --- Sector Number of TESS sectors with QLP or SPOC
light curves (tess_sectors)
262-271 F10.7 mag Gmag Gaia apparent G-band magnitude (Gmag)
273-293 F21.18 mag GMAG ? Absolute gaia G-band magnitude (absolute_g)
295-314 F20.17 mag BP-RP Gaia BP-RP color (bp_rp)
316-337 F22.19 mag BP-RPc ? Gaia BP-RP color corrected for extinction
(bprpcorrected)
339-359 F21.17 --- RPlx ? Gaia parallax to parallax error
(parallaxovererror)
361-373 F13.7 pc rpgeo ? Bailer-Jones photogeometric distance
(rpgeo)
375-392 F18.16 mag AV ? V-band extinction from mwdust (mwdust_av)
394-411 F18.16 mag AG ? G-band extinction from mwdust (mwdust_ag)
413-430 F18.16 mag ABP ? BP-band extinction from mwdust (mwdust_abp)
432-449 F18.16 mag ARP ? RP-band extinction from mwdust (mwdust_arp)
451-455 A5 --- f_ID Parallaxovererror > 10 and mwdust_av < 2
(gaia_filter)
457-458 A2 --- State State evolutionary state based on CMD
position (state) (2)
460-463 F4.1 arcsec r1 ATLAS REFCAT-2 r1 statistic from Tonry et
al. 2018ApJ...867..105T 2018ApJ...867..105T, Cat. J/ApJ/867/105
(r1) (3)
465-469 A5 --- Xray The boolean flag for X-ray detection in 74
cases in our sample (xray_source)
471-480 A10 --- Obs Name of X-ray observatory (xray_observatory)
(4)
482-509 A28 --- r_Xray Literature reference of Heasarc X-ray source
(xraycitationkey) (5)
511-702 A192 --- ADS Link to X-ray detection paper (xrayadslink)
704-711 F8.1 s ExpTime ? Exposure of X-ray observation
(xray_exposure)
713-734 E22.17 10-7W LX ? X-ray luminosity (xray_luminosity)
736-753 F18.16 arcsec Sep ? Source sky separation for X-ray detection
and optical ASAS-SN target positions
(xray_separation)
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Note (1): As explained in section 2, we broadly group these systems by nature
of the 'extra-physics' variability seen in the light curve as follows:
extra_eclipses = Triple and doubly eclipsing binaries,
225 occurences in our sample
spots = Spotted stars, 426 occurences in our sample
regular_pulsator = Regular pulsators, 36 occurences in our sample
reflection = Reflection effects, 29 occurences in our sample
sto_var = Stochastic variability,
24 occurences in our sample
irregular_pulsator = γ-Dor pulsators,
17 occurences in our sample
other = That do not fit into any of these catagories,
9 occurences in our sample
Note (2): Evolutionary states are as follows:
ms = Main sequence stars, 312 sources in our sample
rg = Red giant stars, 122 sources in our sample
sg = Subgiant stars, 221 sources in our sample
Note (3): Radius where cumulative G flux exceeds the one time flux star.
These are given the value 99.9 when a star is so isolated that
the cumulative flux never reaches the threshold within the 36"
search radius.
Note (4): Related to Heasarc X-ray database, these are the list of
involved X-ray observatory as follows:
CHANDRA = Chandra X-ray Observatory,
6 sources in our sample
ROSAT = ROentgen SATellite X-ray observatory,
29 sources in our sample
SWIFT = Swift Gamma-Ray Burst Explorer X-ray Observatory,
20 sources in our sample
XMM-NEWTON = XMM-Newton high throughput X-ray spectroscopy
Multi-Mirror mission, 19 sources in our sample
Note (5): The related references to X-ray database names Heasarc are as follows:
Boller16 = Boller et al. 2016A&A...588A.103B 2016A&A...588A.103B, Cat. J/A+A/588/A103,
RASS2RXS, ROSAT, 17 sources in our sample
Bross13 = Broos et al. 2013ApJS..209...32B 2013ApJS..209...32B, Cat. J/ApJS/209/32,
MYStIX study, 1 source in our sample
Dai15 = Dai et al. 2015ApJS..218....8D 2015ApJS..218....8D, Cat. J/ApJS/218/8,
SACSTPSCAT, SWIFT, 1 source in our sample
Evans10 = Evans et al. 2024ApJS..274...22E 2024ApJS..274...22E, Cat. IX/70,
CSC, CHANDRA, 4 sources in our sample
Evans20 = Evans et al. 2020ApJS..247...54E 2020ApJS..247...54E, Cat. IX/58,
2SXPS, SWIFT, 19 sources in our sample
Ptak03 = Ptak et al. 2003ASPC..295..465P 2003ASPC..295..465P,
CXOXASSIST, CHANDRA, 1 source in our sample
ROSATSc = Rosat scientific team, 2000yCat.9030....0R 2000yCat.9030....0R, Cat. IX/30,
ROSPSPC, ROSAT, 1 source in our sample
Salvato18 = Salvato et al. 2018MNRAS.473.4937S 2018MNRAS.473.4937S,
Cat. J/MNRAS/473/4937, NWAYAWGROS, ROSAT, 1 source in
our sample
Saxton08 = Saxton et al. 2008A&A...480..611S 2008A&A...480..611S, Cat. J/A+A/480/611,
XMMSLEWCLN, XMM-NEWTON, 9 sources in our sample
Traulsen20 = Traulsen et al. 2020A&A...641A.137T 2020A&A...641A.137T,
Cat. IX/61, IX/64, IX/66,
XMMSTACK, XMM-NEWTON, 3 sources in our sample
Voges00 = Voges et al. 2000IAUC.7432R...1V 2000IAUC.7432R...1V, Cat. IX/29,
RASSFSC, ROSAT, 5 sources in our sample
Voges99 = Vosges et al. 1999A&A...349..389V 1999A&A...349..389V, Cat. IX/10,
RASSBSC, ROSAT, 1 source in our sample
Webb20 = Webb et al. 2020A&A...641A.136W 2020A&A...641A.136W,
Cat. IX/59, IX/63, IX/65, IX/68, IX/69
XMMSSC, XMM-NEWTON, 7 sources in our sample
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Byte-by-byte Description of file: crmatch.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 Source identifier (Source)
21- 30 F10.7 mag Gmag Gaia apparent G-band magnitude (Gmag)
32- 50 I19 --- NGaiaDR3 ?=0 The Gaia DR3 source identifier of the
nearby star (Source_x)
52- 60 F9.6 mag NGmag ? Gaia apparent G-band magnitude of the
nearby star (Gmag_x)
62- 70 F9.6 arcsec GaiaSep ? Gaia angular separation (angDist_x)
72- 90 A19 --- ZTF ? ZTF identifier from Zwicky Transient
Facility (ZTF)
92- 97 F6.3 mag gmag ? The g-band associated magnitude (ztf_gmag)
99-116 F18.15 arcsec ZTFSep ? Angular separation with ZTF
(ztf_separation)
118-134 A17 --- ATLAS ATLAS refcat2 designation with RAdeg and
DEdeg positions (ATOID)
136-141 F6.3 mag omag ? ATLAS median o-band magnitude (ls-o-med)
143-161 F19.16 arcsec ATLASSep ? Angular separation with ATLAS (Separation)
163-181 F19.16 d P2 ? Gaia or ZTF or ATLAS period if is within 5
per cent the rotation period, spotted
period, or second orbital period in the TESS
light curve (p2bestmatch)
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Byte-by-byte Description of file: lcs/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 F18.10 d HJD The HJD ephemeris from ASAS-SN (hjd)
20- 45 E26.23 d Phase The phase value (Phase)
47- 64 F18.15 mag LCmag Apparent magnitude in T-band or V-band or
g-band (mag)
66- 89 F24.20 mag e_LCmag Uncertainty of LCmag (mag_err)
91 A1 --- f_LCmag [T V g] Magnitude band (filter)
93- 96 F4.1 --- Sector ? Number of TESS sectors with QLP or SPOC light
curve (sector)
98-119 E22.16 mag LCmag2 ? Second apparent magnitude in T-band or V-band
or g-band (mag2)
121-143 E23.16 mag e_LCmag2 []? Uncertainty of LCmag2 (mag2_err)
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History:
From electronic version of the journal
Online light curves : https://asas-sn.osu.edu/binaries/extra-physics
References:
Rowan et al., Paper I 2022MNRAS.517.2190R 2022MNRAS.517.2190R, Cat. J/MNRAS/517/2190
License: CC-BY-4.0 [see https://spdx.org/licenses/]
(End) Luc Trabelsi [CDS] 13-Mar-2026