J/AJ/154/216 Radial velocities of 41 Kepler eclipsing binaries (Matson+, 2017)
Radial velocities of 41 Kepler eclipsing binaries.
Matson R.A., Gies D.R., Guo Z., Williams S.J.
<Astron. J., 154, 216 (2017)>
=2017AJ....154..216M 2017AJ....154..216M (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Radial velocities ; Stars, masses
Keywords: binaries: close - binaries: eclipsing - binaries: spectroscopic -
stars: fundamental parameters
Abstract:
Eclipsing binaries are vital for directly determining stellar parameters
without reliance on models or scaling relations. Spectroscopically
derived parameters of detached and semi-detached binaries allow us to
determine component masses that can inform theories of stellar and
binary evolution. Here we present moderate resolution ground-based
spectra of stars in close binary systems with and without (detected)
tertiary companions observed by NASA's Kepler mission and analyzed for
eclipse timing variations. We obtain radial velocities and spectroscopic
orbits for five single-lined and 35 double-lined systems, and confirm
one false positive eclipsing binary. For the double-lined spectroscopic
binaries, we also determine individual component masses and examine
the mass ratio M2/M1 distribution, which is dominated by binaries
with like-mass pairs and semi-detached classical Algol systems that
have undergone mass transfer. Finally, we constrain the mass of the
tertiary component for five double-lined binaries with previously
detected companions.
Description:
Spectra for all 41 eclipsing binaries were obtained over the course of
six observing runs between 2010 June and 2013 August at the Kitt Peak
National Observatory (KPNO) with the 4 m Mayall telescope and R-C
Spectrograph. Using the BL380 grating (1200 grooves/mm) in second order
provided wavelength coverage of 3930-4600Å with an average resolving
power of R=λ/δλ∼6200.
Additional observations for 16 of the brighter systems (Kepler magnitude,
Kp~<12) were made at the Anderson Mesa Station of the Lowell Observatory
between 2010 July and 2012 November. The 1.8 m Perkins telescope and
the DeVeny Spectrograph were used along with a 2160 grooves/mm grating
to obtain a resolving power of R=λ/δλ∼6000 over
the wavelength range of 4000-4530Å.
Ten of the binaries were also observed at the Dominion Astrophysical
Observatory (DAO) 1.8 m Plaskett telescope in 2010 July. The Cassegrain
Spectrograph was used with the 1200B grating in first order to obtain
wavelength coverage from 4260-4600Å and an average resolving power
of R=λ/δλ∼4200.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 64 41 Eclipsing Binary System Parameters
table4.dat 74 454 Radial Velocity Measurements; from erratum
published in 2018, AJ, 155, 145
table5.dat 148 40 Orbital Solutions; from erratum published in
2018, AJ, 155, 145
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/AJ/141/83 : Kepler Mission. I. Eclipsing binaries in DR1 (Prsa+, 2011)
J/AJ/142/160 : Kepler Mission. II. Eclipsing binaries in DR2
(Slawson+, 2011)
J/A+A/557/A79 : Spectra of KIC10661783 (Lehmann+, 2013)
J/AJ/147/45 : Kepler mission. IV. Eclipse times for close binaries
(Conroy+, 2014)
J/MNRAS/437/3473 : Temperatures of Kepler eclipsing binaries
(Armstrong+, 2014)
J/PASP/126/914 : Kepler eclipsing binary stars. V. (Conroy+, 2014)
J/AJ/150/178 : Minima of 41 binaries from entire Kepler mission
(Gies+, 2015)
J/AJ/151/68 : Kepler Mission. VII. Eclipsing binaries in DR3 (Kirk+, 2016)
J/AJ/154/105 : Parameters of 529 Kepler eclipsing binaries
(Kjurkchieva+, 2017)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC [2305372/12071006] Kepler Input Catalog number
(Cat. V/133)
10- 33 A24 --- OName Other name
35- 40 F6.3 mag Kpmag [9.586/13.821] Kepler magnitude
42- 46 I5 K T1 [5587/11061] Template temperature of the primary
48- 51 I4 K T2 [421/7750] Template temperature of the secondary
52 A1 --- n_T2 [b] Note on T2 (1)
54 A1 --- l_f2/f1 [<] Limit flag on Flux
55- 58 F4.2 --- f2/f1 [0.01/2] Monochromatic flux ratio (at 4275Å)
(2)
59 A1 --- n_f2/f1 [c] Note on f2/f1 (3)
61- 64 A4 --- Source Template temperature source (4)
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Note (1): Note as follows:
b = Temperature ratio from Armstrong et al. (2014, J/MNRAS/437/3473) used to
determine secondary temperature.
Note (2): All flux ratios derived by maximizing the average cross-correlation
functions over a grid of flux ratios unless otherwise noted (see Section 3.3
for details).
Note (3): Note as follows:
c = Flux ratio adopted from Matson et al. (2016AJ....151..139M 2016AJ....151..139M).
Note (4): Template temperature sources are defined as follows:
A = Armstrong et al. (2014, J/MNRAS/437/3473);
G1 = Guo et al. (2016ApJ...826...69G 2016ApJ...826...69G);
G2 = Guo et al. (2017ApJ...851...39G 2017ApJ...851...39G);
H = Hambleton et al. (2013MNRAS.434..925H 2013MNRAS.434..925H);
L = Lehmann et al. (2013, J/A+A/557/A79);
M = Matson et al. (2016AJ....151..139M 2016AJ....151..139M);
S = Slawson et al. (2011, J/AJ/142/160);
spec = Observed spectral type.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [2305372/12071006] Kepler Input Catalog number
(Cat. V/133)
10- 19 F10.4 d HJD [55366.6695/56522.9367] Heliocentric Julian Date
(HJD-2400000)
21- 25 F5.3 --- Phase [0.003/0.996]? Orbital phase (1)
27- 33 F7.2 km/s RV1 [-294.39/159.65] Primary radial velocity
35- 39 F5.2 km/s e_RV1 [0.67/21.78] Uncertainty in RV1
41- 46 F6.2 km/s (O-C)1 [-123.48/52.51]? Primary (O-C) value (2)
48- 54 F7.2 km/s RV2 [-519.73/351.06]? Secondary radial velocity
56- 60 F5.2 km/s e_RV2 [1.89/46.74]? Uncertainty in RV2
62- 67 F6.2 km/s (O-C)2 [-50.14/52.57]? Secondary (O-C) value (2)
69- 74 A6 --- Obs Observatory where data were obtained (KPNO,
Lowell, DAO) (3)
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Note (1): Relative to T0 at primary eclipse.
Note (2): No data indicates RV measurement was excluded from the orbital fit.
Note (3): Observatory as follows:
KPNO = Kitt Peak National Observatory;
Lowell = Anderson Mesa Station of the Lowell Observatory;
DAO = Dominion Astrophysical Observatory.
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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- 8 I8 --- KIC [2305372/12071006] Kepler Input Catalog number
(Cat. V/133)
9 A1 --- n_KIC [h] Note on KIC (1)
11- 21 F11.9 d Per [0.5625607/6.09604]? Period (2)
23- 34 F12.6 d T0 [55625.5/55928.709]? Time of primary eclipse
(HJD-2400000) (2)
36- 40 F5.1 km/s K1 [8.6/151]? Velocity semi-amplitude of the primary
42- 44 F3.1 km/s e_K1 [0.4/7]? Uncertainty in K1
46- 50 F5.1 km/s K2 [92.8/247]? Velocity semi-amplitude of the
secondary
52- 55 F4.1 km/s e_K2 [0.8/22]? Uncertainty in K2
57- 61 F5.1 km/s gamma1 [-64.1/27.9]? Systemic velocity of the primary
γ1
63- 65 F3.1 km/s e_gamma1 [0.4/5]? Uncertainty in gamma1
67- 71 F5.1 km/s gamma2 [-64.1/21]? Systemic velocity of the secondary
γ2
73- 75 F3.1 km/s e_gamma2 [0.7/7]? Uncertainty in gamma2
76 A1 --- n_gamma2 [a] Note on gamma2 (3)
78- 81 F4.2 --- e [0/0.28]? Eccentricity
82 A1 --- n_e [bc] Note on e (4)
84- 86 I3 deg omega [145/329]? Argument of periastron ω
87 A1 --- n_omega [bc] Note on omega (4)
89- 92 F4.1 km/s rms1 [1.1/13.5]? Root mean square of the primary
velocity fit
94- 97 F4.1 km/s rms2 [2.3/37.1]? Root mean square of the secondary
velocity fit
99-103 F5.3 --- M2/M1 [0.083/1.08]? Mass ratio
105-109 F5.3 --- e_M2/M1 [0.002/0.05]? Uncertainty in M2/M1
111-114 F4.1 deg i [69.9/90]? Inclination (5)
115 A1 --- n_i [bdefg] Note on i (4)
117-121 F5.2 Rsun a [3.6/22]? Semimajor axis
123-126 F4.2 Rsun e_a [0.03/2]? Uncertainty in a
128-131 F4.2 Msun M1 [1.16/4.05]? Mass of the primary
133-136 F4.2 Msun e_M1 [0.01/0.7]? Uncertainty in M1
138-142 F5.3 Msun M2 [0.169/1.83]? Mass of the secondary
144-148 F5.3 Msun e_M2 [0.005/0.1]? Uncertainty in M2
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Note (1): Note as follows:
h = Possible triple system (see Section 4.3.1).
Note (2): The period (P) and epoch (T0 at primary eclipse) were fixed to
values from Gies et al. (2015, J/AJ/150/178).
Note (3): Note as follows:
a = Fixed to systemic value of the primary.
Note (4): Note as follows:
b = Fixed to value derived by Hambleton et al. (2013MNRAS.434..925H 2013MNRAS.434..925H);
c = Fixed to value derived by Slawson et al. (2011, J/AJ/142/160);
d = Fixed to value derived by Matson et al. (2016AJ....151..139M 2016AJ....151..139M);
e = Fixed to value derived by Guo et al. (2016ApJ...826...69G 2016ApJ...826...69G);
f = Fixed to value obtained from preliminary light curve fit;
g = Inclination set to 90° as sin i>1 in Slawson et al. (2011,
J/AJ/142/160). See the text for more details.
Note (5): Inclination values are from Slawson et al. (2011, J/AJ/142/160) and
were used to determine the semimajor axis (a), mass of the primary (M1) and
mass of the secondary (M2) unless otherwise noted.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 13-Aug-2018