J/MNRAS/477/4641 LAMOST DR5 White dwarf-main sequence binaries (Ren+, 2018)
White dwarf-main sequence binaries from LAMOST: the DR5 catalogue.
Ren J.-J., Rebassa-mansergas A., Parsons S.G., Liu X.-W., Luo A.-L.,
Kong X., Zhang H.-T.
<Mon. Not. R. Astron. Soc., 477, 4641-4654 (2018)>
=2018MNRAS.477.4641R 2018MNRAS.477.4641R (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Stars, white dwarf ; Stars, dwarfs ;
Radial velocities
Keywords: binaries: close - binaries: spectroscopic - stars: low-mass -
white dwarfs
Abstract:
We present the data release (DR) 5 catalogue of white dwarf-main
sequence (WDMS) binaries from the Large sky Area Multi-Object fibre
Spectroscopic Telescope (LAMOST). The catalogue contains 876 WDMS
binaries, of which 757 are additions to our previous LAMOST DR1 sample
and 357 are systems that have not been published before. We also
describe a LAMOST-dedicated survey that aims at obtaining spectra of
photometrically selected WDMS binaries from the Sloan Digital Sky
Survey (SDSS) that are expected to contain cool white dwarfs and/or
early-type M dwarf companions. This is a population under-represented
in previous SDSS WDMS binary catalogues. We determine the stellar
parameters (white dwarf effective temperatures, surface gravities and
masses, and M dwarf spectral types) of the LAMOST DR5 WDMS binaries
and make use of the parameter distributions to analyse the properties
of the sample. We find that, despite our efforts, systems containing
cool white dwarfs remain under-represented. Moreover, we make use of
LAMOST DR5 and SDSS DR14 (when available) spectra to measure the NaI
λλ 8183.27, 8194.81 absorption doublet and/or Hα
emission radial velocities of our systems. This allows identifying 128
binaries displaying significant radial velocity variations, 76 of
which are new. Finally, we cross-match our catalogue with the Catalina
Surveys and identify 57 systems displaying light-curve variations.
These include 16 eclipsing systems, two of which are new, and nine
binaries that are new eclipsing candidates. We calculate periodograms
from the photometric data and measure (estimate) the orbital periods
of 30 (15) WDMS binaries.
Description:
The catalogue of WDMS binaries from LAMOST DR5 contains 876 objects
and it is ∼8 times larger than our previous DR1 sample. 357 of these
systems (∼40 per cent of the catalogue) are new identifications
that have not been published before. Moreover, 339 were observed as
part of a dedicated LAMOST survey for obtaining spectra of WDMS
binaries photometrically selected within SDSS that are expected to
contain cool WDs and/or early-type M dwarf companions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 313 1150 Catalogue of LAMOST DR5 WDMS binaries, including
a total of 1150 spectra of 876 unique targets
table3.dat 81 8296 RVs measured from the NaI λλ
8183.27,8194.81 absorption doublet and the
Hα emission for the LAMOST DR5 WDMS binaries
table4.dat 37 76 *The 76 new PCEBs found in this work
table5.dat 93 57 LAMOST DR5 WDMS binaries that display light-curve
variations as revealed by the Catalina
photometric surveys
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Note on table4.dat: PCEB refers to any type of binary that evolved through
CE evolution.
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See also:
V/164 : LAMOST DR5 catalogs (Luo+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- SName Short name (JHHMM+DDMM)
12- 30 A19 --- Name J name (JHHMMSS.ss+DDMMSS.s)
32 I1 --- flagWT [0/1] Identified by the wavelet transform?
34 I1 --- flagPhot [0/1] Photometrically selected SDSS WDMS
binary that obtained a LAMOST spectrum ?
36 I1 --- flagSDSS [0/1] Part of the SDSS DR12 WDMS
spectroscopic catalogue?
38 I1 --- flagCAND [0/1] WDMS binary candidate ?
40- 41 I2 --- flagDR1 [0/11] Part of the LAMOST DR1 WDMS binary
catalogue?
43- 77 A35 --- specID LAMOST spectrum id (MJD-Plate_spID-fiberID)
79- 83 I5 --- MJD [55859/57921] LAMOST MJD
85-104 A20 --- Plate LAMOST Plate
106-107 I2 --- spID [1/16] LAMOST sp ID
109-111 I3 --- fiberID [1/250] LAMOST fiber ID
113-126 F14.10 deg RAdeg Right ascension (J2000)
128-140 F13.10 deg DEdeg Declination (J2000)
142-146 F5.2 --- snu LAMOST Signal Noise Ratio of u filter
148-153 F6.2 --- sng LAMOST Signal Noise Ratio of g filter
155-160 F6.2 --- snr LAMOST Signal Noise Ratio of r filter
162-167 F6.2 --- sni LAMOST Signal Noise Ratio of i filter
169-174 F6.2 --- snz LAMOST Signal Noise Ratio of z filter
176-181 F6.3 mag umag ? LAMOST u magnitude
183-187 F5.3 mag e_umag ? rms uncertainty on umag
189-194 F6.3 mag gmag ? LAMOST g magnitude
196-200 F5.3 mag e_gmag ? rms uncertainty on gmag
202-207 F6.3 mag rmag ? LAMOST r magnitude
209-213 F5.3 mag e_rmag ? rms uncertainty on rmag
215-220 F6.3 mag imag ? LAMOST i magnitude
222-226 F5.3 mag e_imag ? rms uncertainty on imag
228-233 F6.3 mag zmag ? LAMOST z magnitude
235-241 F7.5 mag e_zmag ? rms uncertainty on zmag
243-251 F9.3 K TeffWD ? WD effective temperature
253-260 F8.3 K e_TeffWD ? rms uncertainty on TeffWD
262-265 F4.2 [cm/s2] loggWD ? WD surface gravity
267-270 F4.2 [cm/s2] e_loggWD ? rms uncertainty on loggWD
272-275 F4.2 Msun massWD ? WD mass
277-280 F4.2 Msun e_massWD ? rms uncertainty on massWD
282 I1 --- SpType [0/9]?=- Spectral type of the M dwarf
companion
284-313 A30 --- SpSimbad Simbad spectral type
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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- 10 A10 --- SName Short name (JHHMM+DDMM)
12- 30 A19 --- Name J name (JHHMMSS.ss+DDMMSS.s)
32- 44 F13.5 d HJD Heliocentric Julian date
46- 52 F7.2 km/s RVNaI ?=- NaI (8183.27,8194.81) absorption doublet
radial velocity
54- 59 F6.2 km/s e_RVNaI ?=- rms uncertainty on RVNaI
61- 67 F7.2 km/s RVHa ?=- Hα emission line radial velocity
69- 74 F6.2 km/s e_RVHa ?=- rms uncertainty on RVHa
76- 81 A6 --- Tel Telescope
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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- 19 A19 --- Name J name (JHHMMSS.ss+DDMMSS.s)
21- 22 A2 --- Flag [01] Flag for PCEBs detections (1)
24- 29 F6.2 km/s sRVNaI ?=- NaI maximum RV shift
32- 37 F6.2 km/s sRVHa ?=- Hα maximum RV shift
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Note (1): Flag as follows:
10 = PCEBs detection based on NaI RV measurements
01 = PCEBs detection based on Hα RV measurements
11 = PCEBs detection based on NaI and Hα RV measurements
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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- 19 A19 --- Name J name (JHHMMSS.ss+DDMMSS.s)
21- 46 A26 --- Notes Notes
48- 70 A23 --- Class Classification
72 I1 --- Ref [1/8]? Reference for Known eclipser (1)
75- 93 A19 --- Com Orbital period (2)
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Note (1): References as follows:
1 = Parsons et al. (2013MNRAS.436..241P 2013MNRAS.436..241P)
2 = Parsons et al. (2013MNRAS.429..256P 2013MNRAS.429..256P)
3 = Drake et al. (2010, ApJ, preprint, 1009.3048)
4 = Drake et al. (2014ApJS..213....9D 2014ApJS..213....9D, Cat. J/ApJS/213/9)
5 = Parsons et al. (2015MNRAS.449.2194P 2015MNRAS.449.2194P)
6 = Pyrzas et al. (2012MNRAS.419..817P 2012MNRAS.419..817P)
7 = Parsons et al. (2012MNRAS.420.3281P 2012MNRAS.420.3281P)
8 = Pyrzas et al. (2009MNRAS.394..978P 2009MNRAS.394..978P)
Note (2): orbital periods obtained by calculating periodograms from the
photometric data.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Jun-2021