J/AJ/158/155 SB candidates from the RAVE & Gaia DR2 surveys (Birko+, 2019)
Single-lined spectroscopic binary star candidates from a combination of
the RAVE and Gaia DR2 surveys.
Birko D., Zwitter T., Grebel E.K., Parker Q.A., Kordopatis G.,
Bland-Hawthorn J., Freeman K., Guiglion G., Gibson B.K., Navarro J.,
Reid W., Seabroke G.M., Steinmetz M., Watson F.
<Astron. J., 158, 155 (2019)>
=2019AJ....158..155B 2019AJ....158..155B (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Stars, masses ; Radial velocities
Keywords: binaries: spectroscopic - methods: data analysis - surveys
Abstract:
The combination of the final version of the Radial Velocity Experiment
(RAVE) spectroscopic survey data release 6 with radial velocities (RVs)
and astrometry from Gaia DR2 (Cat. I/345) allows us to identify and create
a catalog of single-lined binary star candidates (SB1), their inferred
orbital parameters, and to inspect possible double-lined binary stars
(SB2). A probability function for the detection of RV variations is used
for identifying SB1 candidates. The estimation of orbital parameters
for main-sequence dwarfs is performed by matching the measured RVs with
theoretical velocity curves sampling the orbital parameter space. The
method is verified by studying a mock sample from the SB 9 catalog
(Cat. B/sb9). Studying the boxiness and asymmetry of the spectral lines
allows us to identify possible SB2 candidates, while matching their spectra
to a synthetic library indicates probable properties of their components.
From the RAVE catalog we select 37664 stars with multiple RV measurements
and identify 3838 stars as SB1 candidates. Joining RAVE and Gaia DR2 yields
450646 stars with RVs measured by both surveys and 27716 of them turn out
to be SB1 candidates, which is an increase by an order of magnitude over
previous studies. For main-sequence dwarf candidates we calculate their
most probable orbital parameters: orbital periods are not longer than
a few years and primary components have masses similar to the solar mass.
All our results are available in the electronic version.
Description:
RAVE (Steinmetz et al. 2006AJ....132.1645S 2006AJ....132.1645S; Zwitter et al. 2008, Cat.
III/257; Siebert et al. 2011, Cat. III/265; Kordopatis et al. 2013,
Cat. III/272; Kunder et al. 2017, Cat. III/279; M. Steinmetz et al. 2019,
in preparation) is a medium resolution (R∼7500) spectroscopic survey
of the Milky Way. It used the UK Schmidt telescope at the Australian
Astronomical Observatory to obtain over half a million stellar spectra
over the period of 2003 April 12 to 2013 April 4. These cover a wavelength
range of 8410-8795 Å. The survey properties as well as all its data
products and analysis are described in detail in its final data release
paper (M. Steinmetz et al. 2019, in preparation). SB1s were searched for
in RAVE using a method similar to Matijevic et al. (2011AJ....141..200M 2011AJ....141..200M)
but applied to a larger sample. Instead of considering only data obtained
up to the third data release, the sixth and final RAVE data release
was used. This increases the number of SB1 candidates from 1333 to 3838
and keeps their percentage at ∼10% of the stars with repeated observations.
The Gaia satellite was launched on 2013 December 19 and started with
scientific observations in 2014 July (Gaia Collaboration et al. 2016,
Cat. I/337), and its main objectives are astrometric, photometric, and
spectroscopic measurements of stars. Most of the stars observed also by
RAVE lie at the faint end of objects accessible for Gaia RV measurements.
Gaia obtained its RV measurements after completion of the RAVE survey,
so combining the two data sets increases the time span of RV measurements
and thus allows a detection of SB1 systems with longer orbital periods.
Overall, 27716 SB1 candidates were identified in the RAVE + Gaia sample,
compared to 3838 from the Rave-only analysis.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 52 3838 Full list of SB1 candidates
table4.dat 75 406 Most probable values of parameters
table6.dat 52 27716 Full list of SB1 candidates obtained by
a combination of RAVE and Gaia RV measurements
table7.dat 75 383 Estimated orbital periods of the SB1 main-sequence
(MS) candidates with the combination of the RAVE
and the Gaia surveys
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See also:
B/sb9 : SB9: 9th Catalogue of Spectroscopic Binary Orbits
(Pourbaix+ 2004-2014)
III/257 : RAVE second data release (Zwitter+, 2008)
III/265 : RAVE 3rd data release (Siebert+, 2011)
III/272 : RAVE 4th data release (Kordopatis+, 2013)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
III/279 : RAVE 5th data release (Kunder+, 2017)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/124/1144 : Orbits of 171 single-lined spectroscopic binaries
(Latham, 2002)
J/AN/340/386 : Catalogue of spectroscopic binary candidate stars (Jack, 2019)
Byte-by-byte Description of file: table2.dat table6.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Object name (RAVE JHHMMSS.s+DDHHMM in Simbad)
18- 19 I2 --- Nobs [2/13] Number of observations
21- 25 F5.2 --- plog [2.79/15.95] Probability function for the variable
RVs
27- 30 I4 d Span [0/4447] Time span of RAVE observations
32- 41 A10 "date" Epoch1 Date of first observation (1)
43- 52 A10 "date" Epoch2 Date of last observation (1)
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Note (1): In Table 2, epoch of the first and the last observation by RAVE.
In Table 6, an epoch of 2015-06-15 was adopted for Gaia.
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Byte-by-byte Description of file: table4.dat table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Object name (RAVE JHHMMSS.s+DDHHMM in Simbad)
18- 21 F4.2 Msun M1 [0.45/1.65]? Mass of primary star (only in
Table 4)
23- 26 F4.2 --- q [0.1/0.8] Mass ratio (M2/M1)
28- 31 F4.2 --- e_q [0/0.3] Mass ratio, first quartile
33- 36 F4.2 --- E_q [0/0.5] Mass ratio, third quartile
38- 41 I4 d Per [1/1263] Orbital period
43- 45 I3 d e_Per [-9/961] Orbital period, first quartile
47- 50 I4 d E_Per [0/1162] Orbital period, third quartile
52- 55 F4.2 --- e [0/0.75] Eccentricity
57- 60 F4.2 --- e_e [0/0.6] Eccentricity, first quartile
62- 65 F4.2 --- E_e [0/0.65] Eccentricity, third quartile
67- 70 I4 km/s gamma [-102/124] System velocity γ
72 I1 km/s e_gamma [0/8] System velocity, first quartile
74- 75 I2 km/s E_gamma [0/10] System velocity, third quartile
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 05-Nov-2019