J/A+A/682/A7 Ensemble seismology of Gaia DR3 binary systems (Beck+, 2024)
Constraining stellar and orbital co-evolution through ensemble seismology of
solar-like oscillators in binary systems.
A census of oscillating red giants and dwarf stars in Gaia DR3 binaries.
Beck P.G., Grossmann D.H., Steinwender L., Schimak L.S., Muntean N.,
Vrard M., Patton R.A., Merc J., Mathur S., Garcia R.A., Pinsonneault M.H.,
Rowan D.M., Gaulme P., Allende Prieto C., Arellano-Cordova K.Z., Cao L.,
Corsaro E., Creevey O., Hambleton K.M., Hanslmeier A., Holl B., Johnson J.,
Mathis S., Godoy-Rivera D., Simon-Diaz S., Zinn J.C.
<Astron. Astrophys. 682, A7 (2024)>
=2024A&A...682A...7B 2024A&A...682A...7B (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology ; Binaries, orbits
Keywords: binaries: eclipsing - asteroseismology - stars: oscillations -
binaries: spectroscopic - stars: late-type - binaries: general
Abstract:
Binary systems constitute a valuable astrophysics tool for testing our
understanding of stellar structure and evolution. Systems contain- ing
at least one oscillating component are interesting in this regard
because asteroseismology offers independent parameters for the
oscillating component that aid in the analysis. Systems of particular
interest include those with known inclinations. With 0.8 million
binary candidates, the two-body orbit catalog (TBO) of Gaia Data
Release 3 (DR3) substantially increases the number of known binaries
and the quality of the astrometric data available for them.
To enlarge the sample of these astrophysically valuable benchmark
objects, we searched for new binary system candidates identified in
the Gaia DR3 TBO, for which one component has a detection of
solar-like oscillations reported in the literature.
We cross-matched the TBO, the full non-single star (NSS) and eclipsing
binary catalogs from Gaia DR3 with catalogs of confirmed solar-like
oscillators in the main-sequence and red-giant phase from the NASA
Kepler mission and stars in the Southern Continuous Viewing Zone of
NASA TESS. The wealth of seismic information is used to characterize
the oscillating primary. To test the completeness and robustness of
the values reported in the TBO catalog, we performed a similar
analysis on stars of the Ninth Catalog of Spectroscopic Binary Orbits
(SB9). Results. The analysis of the SB9 reveals an overall
completeness factor for the Gaia TBO catalog of up to ∼30% providing
reliable orbital parameters for >90% of the systems Porb-SB9≲250d.
We obtained new 954 unique binary system candidates from Gaia DR3,
which host solar-like oscillators, of which we found 45 stars in
binary candidates to be on the main sequence and 909 in the red giant
phase. Additionally, we report 918 oscillators in potentially
long-periodic systems. We present the seismic properties of the full
sample and test whether the reported orbital periods are physically
possible. For 146 giants, the evolutionary state has been determined
from their mixed-mode period spacing, showing a clear trend to long
periodic and less eccentric systems in the advanced phases of stellar
evolution. Two new eclipsing binary systems, hosting a red-giant
primary were found. For another 146 systems hosting oscillating stars,
the values for the orbital inclination were found in the TBO. Of 181
TBO candidate systems observed multiple times with APOGEE, 149 (82%)
are confirmed as binaries from radial-velocity (RV) measurement.
We conclude that the grand majority of the orbital elements reported
in the TBO catalog are physically reasonable and realistic. This
finding increases the number included in the sample of known
solar-like oscillators in binary systems by an order of magnitude. The
large fraction of confirmed binaries from APOGEE RV measurements
indicates that the TBO catalog is robust. We suggest that due to
instrumental noise, the seismically inferred masses and radii of stars
observed with the TESS satellite and with an excess of oscillation
power of νmax≤30uHz could be significantly overestimated. The
differences in the distributions of the orbital period and
eccentricity are due to the accumulative effect of the equilibrium
tide acting in these evolved binary systems.
Description:
We provide the orbital and seismic parameters of oscillating binaries
identified by Gaia DR3 two-body orbit (TBO, tableB1.dat) and
non-linear and acceleration solutions catalogues (NL/ACC,
tableB2.dat). Furthermore, we provide the APOGEE radial velocity
measurements for the system with at least two available spectroscopic
observations from APOGEE (tableB3.dat).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 151 1172 Orbital and seismic parameters of the TBO
systems reported in this work
tableb2.dat 116 937 Seismic parameters of binary candidates with
non-linear and acceleration solutions
tableb3.dat 55 208 APOGEE radial velocity measurements for
Gaia DR3 binaries
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See also:
V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16)
(Ahumada+, 2020)
J/MNRAS/502/1947 : Giant stars in TESS continuous viewing zones
(Mackereth+, 2021)
J/A+A/657/A31 : Solar-like oscillations in Kepler DR25 SC data
(Mathur+, 2022)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 identifier
21- 32 A12 --- KIC Kepler identifier
34- 46 A13 --- TIC TESS identifier
48- 64 A17 --- 2MASS 2MASS survey identifier
66- 70 F5.2 --- RUWE Renormalized Unit Weight Error
72- 79 F8.3 d Per Orbital period from Gaia DR3 TBO
81- 87 F7.3 d e_Per ?=- Orbital period from Gaia DR3 TBO uncertainty
89- 93 F5.3 --- ecc ?=- Orbital eccentricity from Gaia DR3 TBO
95- 99 A5 --- e_ecc ?=- Orbital eccentricity from Gaia DR3 TBO
uncertainty
102-106 F5.1 deg inc ?=- Orbital inclination
109-112 F4.1 deg e_inc ?=- Orbital inclination uncertainty
114-117 A4 --- Type Type of binary solution in Gaia DR3 TBO
119-125 F7.2 uHz numax ?=- Frequency at maximum power (G1)
127-132 F6.2 uHz e_numax ?=- Frequency at maximum power uncertainty (G1)
134-140 F7.3 uHz deltanu ?=- Large frequency separation (G1)
142-147 F6.3 uHz e_deltanu ?=- Large frequency separation uncertainty (G1)
149-151 I3 s deltaPi ?=- Asymptotic period spacing of
dipole g modes (G2)
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Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 identifier
21- 32 A12 --- KIC Kepler identifier
34- 46 A13 --- TIC TESS identifier
48- 64 A17 --- 2MASS 2MASS survey identifier
66- 70 F5.2 --- RUWE Renormalized Unit Weight Error
72- 80 A9 --- Type Type of binary solution in Gaia DR3 TBO
82- 89 F8.3 uHz numax ? Frequency at maximum power (G1)
91- 96 F6.2 uHz e_numax ? Frequency at maximum power uncertainty (G1)
98-104 F7.3 uHz deltanu ? Large frequency separation (G1)
106-112 F7.3 uHz e_deltanu ? Large frequency separation uncertainty (G1)
114-116 I3 uHz deltaPi ?=- Asymptotic period spacing dipole
g modes (G2)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler identifier
10- 26 A17 --- 2MASS 2Mass survey identifier
28- 33 F6.1 d Per Orbital period from Gaia DR3 TBO
35- 36 I2 --- N Number of available spectra from APOGEE
survey (1)
38- 40 I3 d deltaT Timebase between first and last observation (1)
42- 47 F6.3 km/s sigmaRV Mean uncertainty of RV measurements (1)
49- 53 F5.3 km/s meanDRV Mean difference between spectra (1)
55 A1 --- binFlag [x] Indicator for binarity from Gaia in
this work
--------------------------------------------------------------------------------
Note (1): The radial velocity data is taken from DR17 of APOGEE
(Ahumada et al., 2020ApJS..249....3A 2020ApJS..249....3A, Cat. V/154).
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Global notes:
Note (G1): The seismic parameters numax and deltanu are obtained from
Mathur et al. (2022A&A...657A..31M 2022A&A...657A..31M, Cat. J/A+A/657/A31) (MS+SG) or
Mackereth et al. (2021MNRAS.502.1947M 2021MNRAS.502.1947M, Cat. J/MNRAS/502/1947) (RG).
Note (G2): The asymptotic period spacing deltapi and subsequent evolutionary
classification comes from Vrard et al. (2021tsc2.confE.141V).
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History:
From Desmond Grossmann, desmond.grossmann(at)iac.es
Acknowledgements:
We acknowledge the work of curators of the catalogues we used in this
work (see References).
References:
Ahumada et al., 2020ApJS..249....3A 2020ApJS..249....3A, Cat. V/154
Mackereth et al., 2021MNRAS.502.1947M 2021MNRAS.502.1947M, Cat. J/MNRAS/502/1947
Mathur et al., 2022A&A...657A..31M 2022A&A...657A..31M, Cat. J/A+A/657/A31
Vrard et al., 2021tsc2.confE.141V
(End) D.H. Grossmann + P.G. Beck [IAC, Spain], P. Vannier [CDS] 05-Dec-2023