J/ApJS/244/43 Binary stars parameters from LAMOST & Kepler obs. (Zhang+, 2019)
Unbiased distribution of binary parameters from LAMOST and Kepler observations.
Zhang J., Qian S.-B., Wu Y., Zhou X.
<Astrophys. J. Suppl. Ser., 244, 43 (2019)>
=2019ApJS..244...43Z 2019ApJS..244...43Z
ADC_Keywords: Binaries, eclipsing; Abundances, [Fe/H]; Stars, ages;
Stars, masses; Stars, distances; Stars, diameters;
Spectra, optical
Keywords: binaries: eclipsing ; binaries: general
Abstract:
The parameter distribution of binaries is a fundamental knowledge of
the stellar systems. A statistical study on the binary stars is
carried out based on the LAMOST spectral and Kepler photometric
database. We presented a catalog of 1320 binary stars with plentiful
parameters, including period, binary subtype, atmosphere parameters
(Teff, [Fe/H], and logg), and the physical properties, such as mass,
radius, and age, for the primary component stars. Based on this
catalog, the unbiased distribution, rather than the observed
distribution, was obtained after the correction of selection biases by
the Monte Carlo method considering comprehensive affecting factors.
For the first time, the orbital eccentricity distribution of the
detached binaries is presented. The distribution differences between
the three subtypes of binaries (detached, semidetached, and contact)
are demonstrated, which can be explained by the generally accepted
evolutional scenarios. Many characteristics of the binary stars, such
as huge mass transfer on semidetached binaries, period cutoff on
contact binaries, period-temperature relationship of contact binaries,
and the evolved binaries, are reviewed by the new database. This work
supports a common evolutionary scenario for all subtypes of binary
stars.
Description:
The Kepler eclipsing binary stars were cataloged thoroughly
(Prsa+ 2011, J/AJ/141/8 ; Slawson+ 2011, J/AJ/142/160;
Matijevic+ 2012AJ....143..123M 2012AJ....143..123M ; Conroy+ 2014, J/AJ/147/45 and
2014, J/PASP/126/914 ; LaCourse+ 2015, J/MNRAS/452/3561 and
Kirk+ 2016, J/AJ/151/68), containing parameters such as orbital
periods, the morphology of light curves, and phase positions of
secondary minimum on which this work depends.
The LAMOST data we used come from DR4 (the observation duration is
from 2011 October 24 to 2016 June 2).
According to the Kepler Eclipsing Binary Catalog
(http://keplerebs.villanova.edu/ ; see Cat. J/AJ/151/68) maintained by
the Kepler binary group, Kepler observed 3541 binary targets up to
2016 November 14, and 1601 of them were also observed by LAMOST DR4,
covering about half of the Kepler targets. Among the 1601 binaries
with both observations, 1379 of them were measured with atmosphere
parameters successfully. Furthermore, among the 1379 targets with
atmosphere parameters, 1320 of them were obtained with physical
properties (such as mass, radius, and age) successfully. A catalog of
1320 binary stars is given in Table 1 deriving from Kepler, LAMOST,
and our own calculations with the help of the PARSEC (PAdova and
TRieste Stellar Evolution Code; Bressan+ 2012MNRAS.427..127B 2012MNRAS.427..127B ;
Chen+ 2014MNRAS.444.2525C 2014MNRAS.444.2525C and 2015MNRAS.452.1068C 2015MNRAS.452.1068C and
Tang+ 2014MNRAS.445.4287T 2014MNRAS.445.4287T) isochrone database.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 189 1320 Catalog of the binary stars observed by
both LAMOST and Kepler
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See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014)
V/133 : Kepler Input Catalog (Kepler, 2009)
VII/271 : Properties of Galactic Globular Clusters (Francis+, 2014)
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
V/153 : LAMOST DR4 catalogs (Luo+, 2018)
V/164 : LAMOST DR5 catalogs (Luo+, 2019)
J/MNRAS/371/703 : MILES library of empirical spectra (Sanchez-Blazquez+, 2006)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/MNRAS/404/1639 : MILES base models & new line index system (Vazdekis+, 2010)
J/AJ/141/83 : Kepler Mission. I. Eclipsing binaries in DR1 (Prsa+, 2011)
J/AJ/142/160 : Kepler Mission. II. EBs in DR2 (Slawson+, 2011)
J/other/RAA/11.924 : Atmospheric parameters for 771 stars (Wu+, 2011)
J/A+A/525/A71 : Atmospheric parameters for 1273 stars (Wu+, 2011)
J/ApJ/773/1 : HD19356 period recorded in the Cairo Calendar (Jetsu+, 2013)
J/MNRAS/437/3473 : Temperatures of Kepler eclipsing binaries (Armstrong+, 2014)
J/AJ/147/45 : Kepler mission. IV. Eclipse times (Conroy+, 2014)
J/PASP/126/914 : Kepler eclipsing binary stars. V. (Conroy+, 2014)
J/MNRAS/441/2316 : 10 nearby solar-type dwarfs RV curves (Gorynya+, 2014)
J/MNRAS/452/3561 : Kepler EB stars. K2 Campaign 0 (LaCourse+, 2015)
J/MNRAS/455/4136 : Kepler triples (Borkovits+, 2016)
J/ApJ/832/121 : 4-yr RV survey of red giant in EBs (Gaulme+, 2016)
J/AJ/151/68 : Kepler Mission. VII. Eclipsing binaries in DR3 (Kirk+, 2016)
J/other/RAA/19.64 : LAMOST spectrosc. binaries & variable stars (Qian+, 2019)
http://keplerebs.villanova.edu/ : Online Kepler Ecplising Binary Catalog
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [KIC]
4- 12 I9 --- Name [1026957/212175535] KIC (for numbers <13161029)
or EPIC number
14- 22 F9.5 deg RAdeg [53/336.1] Right Ascension (J2000) (1)
24- 32 F9.6 deg DEdeg [-4/51.8] Declination (J2000) (1)
34- 45 F12.7 d Per [0.09/1087.3] Period (1)
47- 51 I5 K Teff [4131/36000] Surface temperature (2)
53- 56 I4 K e_Teff [45/9654] Uncertainty in Teff (2)
58- 62 F5.3 [cm/s2] logg [1.8/4.9] Surface gravity (2)
64- 68 F5.3 [cm/s2] e_logg [0.06/4.7] Uncertainty in logg (2)
70- 75 F6.3 [-] FeH [-2.5/0.8] Metallicity (2)
77- 81 F5.3 [-] e_FeH [0.04/2] Uncertainty in FeH (2)
83- 87 I5 pc Dist [57/12042]? Distance of the binary target
from the Sun (3)
89- 93 I5 pc B_Dist [64/15425]? Upper bound on Dist (3)
95- 98 I4 pc b_Dist [52/9630]? Lower bound on Dist (3)
100-105 F6.4 --- Sep [0.07/1]? Phase separation of the secondary
minimum from the primary minimum measured
from the light curves (1)(4)
107-111 F5.2 --- Morph [-1/1] Morphology of the binary
light curve (1)(5)
113-117 F5.2 Msun Mass [0.5/19] Mass, PARSEC derived
119-123 F5.2 Msun b_Mass [0.1/15] Lower bound on Mass
125-129 F5.2 Msun B_Mass [0.6/66] Upper bound on Mass
131-135 F5.2 Rsun Rad [0.5/19] Radius, PARSEC derived
137-141 F5.2 Rsun b_Rad [0.1/18] Lower bound on Rad
143-149 F7.2 Rsun B_Rad [0.6/1674] Upper bound on Rad
151-158 E8.2 yr Age [3980000/13200000000] Age, PARSEC derived
160-167 E8.2 yr b_Age [3980000/11800000000] Lower bound on Age
169-176 E8.2 yr B_Age [10200000/13200000000] Upper bound on Age
178-178 I1 --- Stage [1/4] Rough evolution stage, PARSEC derived (6)
180-180 I1 --- b_Stage [1/3] Lower bound on Stage
182-182 I1 --- B_Stage [1/8] Upper bound on Stage
184-189 F6.4 --- Prob [0.001/1]? Probability of the binary target to
be a detected eclipsing binary
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Note (1): From the Kepler Eclipsing Binary Catalog:
http://keplerebs.villanova.edu/
Note (2): Derived from Lamost DR4 spectra.
Note (3): From Bailer-Jones et al. (2018AJ....156...58B 2018AJ....156...58B ; Cat. I/347).
Note (4): If the phase separation is a null then no secondary minimum was
found in the light curve.
Note (5): "Morph" is the morphology of the binary light curve that is also
taken from the Kepler Eclipsing Binary Catalog, and it is used to
define the binary subtypes roughly.
Values <0.5 are predominantly detached, semidetached are roughly
0.5-0.7, overcontact broadly lie between 0.7-0.8 and higher values are
a mix of ellipsoidal and uncertain classifications.
-1 means the morphology is unclear or unknown.
Note (6): Stage is the "rough" evolutionary sections
from http://stev.oapd.inaf.it/cmd_3.2/faq.html --Code as follows:
1 = main sequence (MS);
2 = subgiant branch (SGB), or Hertzsprung gap for more intermediate+massive
stars;
3 = red giant branch (RGB), or the quick stage of red giant for
intermediate+massive stars;
4 = core He-burning (CHeB) for low mass stars, or the very initial stage
of CHeB for intermediate+massive stars.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 11-Mar-2020