J/A+A/670/A75 New triple system candidates using Gaia DR3 (Czavalinga+, 2023)
New compact hierarchical triple system candidates identified using Gaia DR3.
Czavalinga D.R., Mitnyan T., Rappaport S.A., Borkovits T., Gagliano R.,
Omohundro M., Kristiansen M.H.K., Pal A.
<Astron. Astrophys. 670, A75 (2023)>
=2023A&A...670A..75C 2023A&A...670A..75C (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Binaries, orbits ; Optical
Keywords: binaries: close - binaries: eclipsing - binaries: spectroscopic -
binaries: visual - catalogs
Abstract:
We introduce a novel way to identify new compact hierarchical triple
stars by exploiting the huge potential of Gaia DR3 and also its future
data releases. We aim to increase the current number of compact
hierarchical triples significantly. We utilize several eclipsing
binary catalogs from different sky surveys totaling more than 1
million targets for which we search for Gaia DR3 Non-single Star (NSS)
orbital solutions with periods substantially longer than the eclipsing
periods of the binaries. Those solutions in most cases should belong
to outer orbits of tertiary stars in those systems. We also try to
validate some of our best-suited candidates using TESS eclipse timing
variations.
We find 403 objects with suitable Gaia orbital solutions of which 28
are already known triple systems. This makes 375 newly identified
hierarchical triple system candidates in our sample. We analyze the
cumulative probability distribution of the outer orbit eccentricities
and find that it is very similar to the ones found by earlier studies
based on the observations of the Kepler and OGLE missions. We found
measurable non-linear eclipse timing variations or third-body eclipses
in the TESS data for 189 objects which we also consider to be
confirmed candidates. Out of these, we construct analytical
light-travel time effect models for the eclipse timing variations of
22 objects with well-sampled TESS observations. We compare the outer
orbital parameters from our solutions with the ones from the Gaia
solutions and find that the most reliable orbital parameter is the
orbital period, while the values of the other parameters should be
used with caution.
Description:
We performed a search for possible hierarchical triple systems among
more than 1 million cataloged EBs. We did this by looking for Gaia
astrometric and/or spectroscopic NSS solutions with periods that are
at least five times longer than the corresponding EB period. We
identified 403 such triple candidates, of which 376 are newly
proposed, while 27 are previously known candidates confirmed by Gaia
observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 248 403 Orbital parameters of triple system candidates
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See also:
I/357 : Gaia DR3 Part 3. Non-single stars (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 28 A28 --- Name Common name of stars
30- 48 A19 --- GaiaDR3 Gaia DR3 Source Identifier (source_id)
50- 61 F12.6 deg RAdeg Right ascension (ICRS) at epoch J2000.0
63- 74 F12.6 deg DEdeg Declination (ICRS) at epoch J2000.0
76-105 A30 --- NSSmodel NSS model adopted from Gaia DR3 NSS
solution (1)
107-118 F12.6 d binPer Inner binary period
120-131 F12.6 d Per Period of the outer orbit (period)
133-144 F12.6 d e_Per Standard error of outer period (period_error)
146-157 F12.6 Rsun smasini Projected semi-major axis
159-170 F12.6 Rsun e_smasini Standard error of projected semi-major axis
172-183 F12.6 --- ecc Eccentricity of the outer orbit (eccentricity)
185-196 F12.6 --- e_ecc Standard error of eccentricity of the outer
orbit (eccentricity_error)
198-209 F12.6 deg omega Argument of periastron (arg_periastron)
211-222 F12.6 deg e_omega Standard error of argument of periastron
(arg_periastron)
224-235 F12.6 d Tperi Periastron epoch relative to J2016.0
(t_periastron)
237-248 F12.6 d e_Tperi Standard error of periastron epoch relative
to J2016.0 (tperiastronerror)
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Note (1): For objects with two different types of orbital solutions, we chose to
use the pure astrometric solution in every case as a convention.
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History: From Donat Robert Czavalinga, czdonat(at)titan.physx.u-szeged.hu
Acknowledgements:
This work has made use of data from the European Space
Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed
by the Gaia Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium).
(End) Patricia Vannier [CDS] 06-Dec-2022