J/ApJS/282/55 Single-lined spectroscopic binaries from LAMOST DR11 (Ye+, 2026)
New single-lined spectroscopic binaries identified from the LAMOST Medium-
Resolution Spectroscopic survey.
Ye T., Chen Y., Xia F., Fu Y.
<Astrophys. J. Suppl. Ser., 282, 55 (2026)>
=2026ApJS..282...55Y 2026ApJS..282...55Y
ADC_Keywords: Binaries, spectroscopic; Spectra, optical; Abundances, [Fe/H];
Binaries, orbits
Keywords: Spectroscopic binary stars ; Radial velocity ;
Astronomy data analysis ; Orbit determination
Abstract:
A typical single-lined spectroscopic binary (SB1) consists of two
stars with almost the same age but markedly different masses and
physical properties. SB1s are essential for obtaining the statistical
properties of stars and constraining stellar evolutionary models,
particularly when orbital parameters are well determined. In this
study, we first carry out a data-cleaning step on a sample of LAMOST
Medium-Resolution Spectroscopic Survey stars with a sufficient number
of observations and perform an F2 test, obtaining 7775 radial velocity
variables. After removing false positives and crossmatching with
variable and double-lined spectroscopic binary (SB2) catalogs, we
exclude known astrophysical variables and SB2s, leaving 6106 SB1
candidates. We estimate initial periods using the Heck-Manfroid-Mersch
method combined with Monte Carlo simulations and then fit each source
with both an orbital model and a trend model, selecting between them
via the Snedecor F-test of nested models. For orbital models, we
accept the least-χ2 solution if it satisfies F2<3.1, s>10,
phasegapmax<0.3, σv/K<0.25 and passes the Markov Chain Monte
Carlo-based robustness tests. For trend cases, we discard zeroth-order
fits and require F2<3.1. In total, we obtain 623 accepted solutions,
of which 337 SB1s are new relative to existing catalogs.
Description:
LAMOST, a special reflecting Schmidt telescope, is located at the
Xinglong Station of the National Astronomical Observatories, Chinese
Academy of Sciences, in Xinglong County, Hebei Province, China
(40°N, 105°E) at an altitude of 960m. Its special design
allows both a large aperture (effective aperture of 3.6-4.9m) and a
wide field of view (5°).
Since September 2017, LAMOST has acquired a substantial volume of
Medium-Resolution Spectroscopic (MRS) data with a resolution of
R∼7500, covering the wavelength ranges 4950Å<λ<5350Å and
6300Å<λ<6800Å.
In this study, we use data from LAMOST DR11 v1.1, obtained by
observations between 2011 October and 2023 June.
We download the complete LAMOST-MRS General Catalog from LAMOST DR11's
data access and remove invalid data in it. We selected the B-band spectra.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 88 6106 Data information of SB1 candidates
in sample 2 (Section 3)
table2.dat 414 623 Orbital or trend solutions provided for the
identified SB1 collected in our SB1 catalog
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See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-)
B/sb9 : SB9: 9th Catalog of Spectroscopic Binary Orbits (Pourbaix+ 2004-2014)
B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)
II/366 : ASAS-SN catalog of variable stars (Jayasinghe+, 2018-2020)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
I/357 : Gaia DR3 Part 3. Non-single stars (Gaia Collaboration, 2022)
V/162 : LAMOST DR11 catalogs (Luo+, 2026)
J/AJ/140/184 : RAVE double-lined spectroscopic binaries (Matijevic+, 2010)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/A+A/635/A155 : Gaia-ESO Survey SB1 catalogue (Merle+, 2020)
J/A+A/638/A145 : GALAH survey. FGK binary stars (Traven+, 2020)
J/AJ/162/184 : APOGEE: radial velocities of binaries (Kounkel+, 2021)
J/A+A/655/A4 : MONOS II. SB1 Orbital review (Trigueros Paez+, 2021)
J/ApJS/256/14 : RVs from LAMOST MRS DR7 stellar spectra (Zhang+, 2021)
J/A+A/664/A159 : Radial velocities of Galactic SB1s (Mahy+, 2022)
J/ApJS/258/26 : Spectroscopic binaries from LAMOST MRS. I. (Zhang+, 2022)
J/ApJS/269/41 : New SB1s with sp. orbits from LAMOST DR8 LRS (Chen+, 2023)
J/ApJS/266/18 : Double-line spectroscopic binaries from LAMOST (Zheng+, 2023)
J/A+A/692/A192 : C, SB1, SB2 & SB3 southern O stars rot. rate (Blex+, 2024)
J/MNRAS/527/521 : SB2s in LAMOST-MRS (Kovalev+, 2024)
J/ApJS/278/46 : Orbits of 665 SB2s in Lamost-MRS (Guo+, 2025)
J/ApJS/276/11 : Spectroscopic binaries from LAMOST MRS DR9 (Li+, 2025)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- Gaia Gaia DR3 catalog identifier
21- 30 F10.6 deg RAdeg [2.7/348.4] Right Ascension (J2000)
32- 40 F9.6 deg DEdeg [-6.4/70.5] Declination (J2000)
42- 45 I4 K Teff [4000/8499]? LAMOST LASP effective temperature
47- 51 F5.3 [cm/s2] logg [0.8/4.85]? LAMOST LASP surface gravity
53- 58 F6.3 [-] [Fe/H] [-2.5/0.74]? LAMOST LASP metallicity
60- 68 F9.4 d Span [61.93/1982.7] Time span of the observation
70- 71 I2 --- Nrv [12/58] Number of radial velocity measurements
73- 81 F9.2 --- Chi2 [31.5/292160.1] Model χ2 value, equation 1
83- 88 F6.2 --- F2 [3.1/236.6] The F2 statistic; equation 2
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- Gaia Gaia DR3 catalog identifier
21- 28 A8 --- Type "SB1" or "TrendSB1"
30- 40 F11.6 d Per [0.98/1857.8]? Orbital period
42- 51 F10.6 d E_Per [1.7e-05/318.5]? Upper (positive) posterior
uncertainty of Per
53- 62 F10.6 d e_Per [1.6e-05/277.7]? Lower (negative) posterior
uncertainty of Per
64- 71 F8.6 rad M0 [0.04/6.3]? Mean anomaly at t0
73- 80 F8.6 rad E_M0 [0.007/3.4]? Upper (positive) posterior
uncertainty of M0
82- 89 F8.6 rad e_M0 [0.007/3.2]? Lower (negative) posterior
uncertainty of M0
91- 98 F8.6 --- e [0.009/0.8]? Orbital eccentricity
100- 107 F8.6 --- E_e [0.003/0.2]? Upper (positive) posterior
uncertainty of e
109- 116 F8.6 --- e_e [0.003/0.2]? Lower (negative) posterior
uncertainty of e
118- 125 F8.6 rad omega [0.03/6.3]? Longitude of periastron
127- 134 F8.6 rad E_omega [0.009/3.2]? Upper (positive) posterior
uncertainty of omega
136- 143 F8.6 rad e_omega [0.009/5.8]? Lower (negative) posterior
uncertainty of omega
145- 155 F11.6 km/s gamma [-310.3/116.4]? Center-of-mass velocity
157- 164 F8.6 km/s E_gamma [0.089/2.11]? Upper (positive) posterior
uncertainty of gamma
166- 173 F8.6 km/s e_gamma [0.089/1.7]? Lower (negative) posterior
uncertainty of gamma
175- 183 F9.6 km/s K [3.88/60.6]? RV semi-amplitude
185- 193 F9.6 km/s E_K [0.12/10.8]? Upper (positive) posterior
uncertainty of K
195- 202 F8.6 km/s e_K [0.12/2.3]? Lower (negative) posterior
uncertainty of K
204- 206 F3.1 --- degree [1/2]? Polynomial degree
208- 217 F10.6 --- V0 [-97.4/137]? V0=a'-c(ΔTm)2/12
219- 231 E13.6 --- dVdt [-0.12/0.22]? δV/δt=b
233- 245 E13.6 --- d2Vdt2 [-0.0004/0.003]? δ2V/δt2=2c
247- 260 F14.6 --- t0 ? Reference time (TDB)
262- 270 F9.1 --- r_t0 ? Reference epoch (J2021.0)
272- 282 F11.6 --- Delta-Tm [2075.29/2075.3]? The total time span of
the parent sample
284- 293 F10.6 --- Chi2-orb [4.42/173.4] Chi_{orbit}^2 calculated from
Equation 10
295- 303 F9.6 --- F2-orb [-9.7/3.1] The statistic in Section 4.4
305- 314 F10.6 --- s [10/245]? The significance of the solution
(Equation 11)
316- 323 F8.6 --- GapMax [0.07/0.3]? Maximum gap in phase
325- 332 F8.6 --- sigV/K [0.018/0.3]? The ratio between the mean RV
uncertainty and the semi-amplitude
334 I1 --- New [0/1] Flag on new SB1s (1: 377 occurrences)
336- 345 F10.6 deg RAdeg [10.3/348] Right Ascension in decimal
degrees (J2000)
347- 355 F9.6 deg DEdeg [-6.4/56.8] Declination in decimal degrees
(J2000)
357- 363 F7.2 K Teff [4008/8096]? LAMOST LASP effective
temperature
365- 369 F5.3 [cm/s2] logg [1.3/4.82]? LAMOST LASP surface gravity
371- 376 F6.3 [-] [Fe/H] [-2.5/0.52]? LAMOST LASP metallicity
378- 388 F11.6 d Span [88.8/1950] Time span of the observation
390- 391 I2 --- Nrv [12/57] Number of radial velocity
measurements
393- 404 F12.6 --- Chi2 [32.89/28880] Model χ^2 value, equation
1
406- 414 F9.6 --- F2 [3.1/93.4] The F2 statistic; equation 2
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History:
From electronic version of the journal
License: CC-BY-4.0
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Jul-2026