J/ApJ/832/121 4-yr RV survey of red giant in eclipsing binaries (Gaulme+, 2016)
Testing the asteroseismic scaling relations for red giants with
eclipsing binaries observed by Kepler.
Gaulme P., McKeever J., Jackiewicz J., Rawls M.L., Corsaro E., Mosser B.,
Southworth J., Mahadevan S., Bender C., Deshpande R.
<Astrophys. J., 832, 121-121 (2016)>
=2016ApJ...832..121G 2016ApJ...832..121G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, giant ; Binaries, eclipsing ; Radial velocities ; Surveys ;
Abundances, [Fe/H]
Keywords: binaries: eclipsing; stars: evolution; stars: oscillations
Abstract:
Given the potential of ensemble asteroseismology for understanding
fundamental properties of large numbers of stars, it is critical to
determine the accuracy of the scaling relations on which these
measurements are based. From several powerful validation techniques,
all indications so far show that stellar radius estimates from the
asteroseismic scaling relations are accurate to within a few percent.
Eclipsing binary systems hosting at least one star with detectable
solar-like oscillations constitute the ideal test objects for
validating asteroseismic radius and mass inferences. By combining
radial velocity (RV) measurements and photometric time series of
eclipses, it is possible to determine the masses and radii of each
component of a double-lined spectroscopic binary. We report the
results of a four-year RV survey performed with the echelle
spectrometer of the Astrophysical Research Consortium's 3.5m telescope
and the APOGEE spectrometer at Apache Point Observatory. We compare
the masses and radii of 10 red giants (RGs) obtained by combining
radial velocities and eclipse photometry with the estimates from the
asteroseismic scaling relations. We find that the asteroseismic
scaling relations overestimate RG radii by about 5% on average and
masses by about 15% for stars at various stages of RG evolution.
Systematic overestimation of mass leads to underestimation of stellar
age, which can have important implications for ensemble
asteroseismology used for Galactic studies. As part of a second
objective, where asteroseismology is used for understanding binary
systems, we confirm that oscillations of RGs in close binaries can be
suppressed enough to be undetectable, a hypothesis that was proposed
in a previous work.
Description:
In this paper, we report the results of a four-year radial velocity
(RV) survey performed with the echelle spectrometer of the
Astrophysical Research Consortium (ARC) 3.5m telescope at Apache Point
Observatory (APO). We benefited from complementary observations by the
Apache Point Observatory Galactic Evolution Experiment (APOGEE)
spectrograh for one system. The targets are 17 EB systems of the 18
Gaulme+ (2013ApJ...767...82G 2013ApJ...767...82G, 2014ApJ...785....5G 2014ApJ...785....5G) red giant
eclipsing-binary (RG/EB) candidates, whose orbital periods range from
15 to 1058 days.
All spectra were obtained with the echelle spectrometer of the 3.5m
ARC telescope at APO (ARCES), except a set of 25 spectra of the system
KIC 7037405 from the APOGEE spectrometer of the Sloan Digital Sky
Survey, also based at APO.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 71 17 Atmospheric parameters of the red giants from
the ARC 3.5m visible spectra
table2.dat 170 16 *Orbital parameters from dynamical modeling with
JKTEBOP
table3.dat 33 14 Asteroseismic frequencies at maximum amplitude
νmax and observed mean large spacings
Δνobs of the oscillating red giant
of our sample
table5.dat 48 315 Radial velocities
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Note on table2.dat: JKTEBOP software home page :
http://www.astro.keele.ac.uk/jkt/codes/jktebop.html
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/ApJS/211/2 : Revised properties of Q1-16 Kepler targets (Huber+, 2014)
J/A+A/557/A119 : Eclipsing binary system LL Aquarii (Southworth, 2013)
J/A+A/555/A150 : Physical parameters of cool solar-type stars (Tsantaki+, 2013)
J/A+A/546/A14 : Limb-darkening for CoRoT, Kepler, Spitzer (Claret+, 2012)
J/ApJS/199/30 : Effective temperatures for KIC stars (Pinsonneault+, 2012)
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/A+A/510/A21 : Stellar Limb-Darkening Coefficients (Sing, 2010)
J/A+A/469/783 : Code for automatic determination of EW (ARES) (Sousa+, 2007)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [3955867/10001167] KIC number
10- 14 F5.2 mag Kpmag [9.2/14] Kepler magnitude
16- 19 I4 K Teff [4516/5058]? Effective temperature from ARCES
21- 23 I3 K e_Teff [36/152]? Teff uncertainty
25- 28 F4.2 [cm/s2] logg [2.2/3.7]? Surface gravity from ARCES
30- 33 F4.2 [cm/s2] e_logg [0.09/0.4]? logg uncertainty
35- 39 F5.2 [Sun] [Fe/H] [-0.7/0.3]? Metallicity from ARCES
41- 44 F4.2 [Sun] e_[Fe/H] [0.01/0.1]? [Fe/H] uncertainty
46- 49 I4 K Teff2 [4539/5044]? Effective temperature from APOGEE
51- 52 I2 K e_Teff2 [91]? Teff2 uncertainty
54- 56 F3.1 [cm/s2] logg2 [2.3/3.3]? Surface gravity from APOGEE
58- 60 F3.1 [cm/s2] e_logg2 [0.1]? logg2 uncertainty
62- 66 F5.2 [Sun] [Fe/H]2 [-0.7/0.5]? Metallicity from APOGEE
68- 71 F4.2 [Sun] e_[Fe/H]2 [0.02/0.08]? [Fe/H]2 uncertainty
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [3955867/10001167] KIC number
10- 20 F11.6 d Per [14.6/1058.2] Orbital period
22- 29 F8.6 d e_Per [0/0.02] Per uncertainty
31- 38 F8.4 d Tp Time of periastron in Kepler Julian Date
(BJD-2454833 days)
40- 45 F6.4 d e_Tp [0.0003/0.02] Tp uncertainty
47- 52 F6.2 deg omega [4.1/356] Argument of periastron ω
54- 57 F4.2 deg e_omega [0.02/5] omega uncertainty
59- 64 F6.4 --- e [0.001/0.5] Eccentricity
66- 71 F6.4 --- e_e [0.0002/0.01] e uncertainty
73- 78 F6.3 deg i [81.5/90] Orbital plane inclination
80- 84 F5.3 deg e_i [0.006/0.6]? i uncertainty
86 A1 --- f_i Flag on i (1)
88- 92 F5.2 % R2/R1 [5.3/23.3] R2/R1 value (2)
94- 97 F4.2 % e_R2/R1 [0.02/0.3] R2/R1 uncertainty
99-104 F6.3 % Ratio [1.924/24.4] (R1+R2)/a value (2)
106-110 F5.3 % e_Ratio [0.007/0.3] Ratio uncertainty
112-116 F5.3 --- T2/T1 [0.07/4] (T2/T1)4 (2)
118-122 F5.3 --- e_T2/T1 [0.002/0.4] T2/T1 uncertainty
124-130 F7.4 % L2/L1 [0.02/15.1] L2/L1 value (2)
132-137 F6.4 % e_L2/L1 [0.0006/0.1] L2/L1 uncertainty
139-142 F4.1 km/s K1 [12.3/50.2] Radial velocity semiamplitude of
the red giant
144-146 F3.1 km/s e_K1 [0.1/0.8] K1 uncertainty
148-151 F4.1 km/s K2 [23/58]? Radial velocity semiamplitude of
the companion
153-155 F3.1 km/s e_K2 [0.3/3]? K2 uncertainty
157-164 F8.3 km/s gamma [-185/25] Radial velocity offset
166-170 F5.3 km/s e_gamma [0.009/0.4] gamma uncertainty
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Note (1):
b = As regards 9540226, we fixed the inclination at 90° because JKTEBOP
would not converge properly and its inclination is almost 90°, as the
almost-vertical ingress and egress of the companion star indicate
(Figure 3).
Note (2): where (R1, T1, L1) and (R2, T2, L2) are the red giant and companion's
radii, effective temperatures, and luminosities.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [4663623/10001167] KIC number
10- 15 F6.2 uHz numax [19.9/322] Asteroseismic frequency at maximum
amplitude
17- 20 F4.2 uHz e_numax [0.09/2.1] numax uncertainty
22- 27 F6.3 uHz delnu [2.7/22.3] Observed mean large spacing
Δνobs
29- 33 F5.3 uHz e_delnu [0.01/0.06] delnu uncertainty
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [KIC]
5- 12 I8 --- KIC [3955867/10001167] Object identifier
14- 22 F9.4 d KJD Kepler Julian Date; BJD-2454833 (1)
24- 30 F7.2 km/s RVel1 [-228.5/58.7] Primary radial velocity
32- 35 F4.2 km/s e_RVel1 [0.02/0.2] Uncertainty in RVel1
37- 43 F7.2 km/s RVel2 [-242/70]? Secondary radial velocity
45- 48 F4.2 km/s e_RVel2 [0/7]? Uncertainty in RVel2
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Note (1): Kepler Julian dates KJD are related to barycentric Julian dates BJD
by: KJD = BJD - 2454833 days.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Feb-2017