J/A+A/624/A68 47 single-line eclipsing binaries BEBOP velocities (Martin+, 2019)
The BEBOP radial-velocity survey for circumbinary planets.
I. Eight years of CORALIE observations of 47 single-line eclipsing binaries and
abundance constraints on the masses of circumbinary planets.
Martin D.V., Triaud A.H.M.J., Udry S., Marmier M., Maxted P.F.L.,
Collier Cameron A., Hellier C., Pepe F., Pollacco D., Segransan D., West R.
<Astron. Astrophys. 624, A68 (2019)>
=2019A&A...624A..68M 2019A&A...624A..68M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Binaries, eclipsing ;
Radial velocities ; Exoplanets
Keywords: binaries: eclipsing - planets and satellites: detection -
techniques: radial velocities - techniques: photometric -
stars: statistics - stars: low-mass
Abstract:
We introduce the BEBOP radial velocity survey for circumbinary
planets. We initiated this survey using the CORALIE spectrograph on
the Swiss Euler Telescope at La Silla, Chile. An intensive four year
observing campaign commenced in 2013, targeting 47 single lined
eclipsing binaries drawn from the EBLM survey for low mass eclipsing
binaries. Our specific use of binaries with faint M dwarf companions
avoids spectral contamination, providing observing conditions akin to
single stars. By combining new BEBOP observations with existing ones
from the EBLM programme, we report on the results of 1519 radial
velocity measurements over timespans as long as eight years. For the
best targets we are sensitive to planets down to 0.1 Jupiter masses,
and our median sensitivity is 0.4 Jupiter masses. In this initial
survey we do not detect any planetary mass companions. Nonetheless, we
present the first constraints on the abundance of circumbinary
companions, as a function of mass and period. A comparison of our
results to Kepler's detections indicates a dispersion of planetary
orbital inclinations less than ∼10°.
Description:
Radial velocities of the 47 single-lined eclipsing binaries targeted
for the BEBOP radial velocity survey for circumbinary planets
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 127 47 Observational and calculated parameters of
the inner binaries
vc/* . 47 Individual velocity curves
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [EBLM]
6- 13 A8 --- EBLM EBLM name (JHHMM+DD)
15- 16 I2 h RAh Right ascension (J2000)
18- 19 I2 min RAm Right ascension (J2000)
21- 25 F5.2 s RAs Right ascension (J2000)
27 A1 --- DE- Declination sign (J2000)
28- 29 I2 deg DEd Declination (J2000)
31- 32 I2 arcmin DEm Declination (J2000)
34- 37 F4.1 arcsec DEs Declination (J2000)
39- 43 F5.2 d Pbin Orbital period
45- 48 F4.2 Msun MassA Mass of component A
50- 54 F5.2 mag VmagA V magnitude of component A
56- 61 F6.4 Msun MassB Mass of component B
63- 67 F5.2 mag VmagB V magnitude of component B
69- 77 F9.4 d Tpri Mid-time of primary eclipse (BJD-2455000)
79- 87 F9.4 d Tsec Mid-time of secondary eclipse (BJD-2455000
89- 90 I2 --- Ntot Total number of observations
92- 93 I2 m/s sig1800s Photon noise uncertainty for all observations
of 1800 seconds on RV
95- 96 I2 m/s sigmedian Median photon noise precision for all
observations in RV (1)
98- 99 I2 m/s sigadd Additional error on RV (2)
101-104 F4.2 yr timespan Observational timespan
106-127 A22 --- FileName Name of the file with radial velocities in
subdirectory vc
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Note (1): that is both the 1800 second observations taken for BEBOP and earlier,
shorter observations taken in the EBLM programme
Note (2): sigadd=SQRT(deltabis2/4 - <siggamma2>), where deltabis is the
root mean square of the variation of the bisector measurements around their
mean and is the mean photon noise error.
If > deltabis2/4 then we take sigadd , which was the case for
30 of the 47 binaries. Otherwise, we add sigmaadd in quadrature to the
radial velocity measurements.
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Byte-by-byte Description of file: vc/*
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Bytes Format Units Label Explanations
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1- 12 F12.6 d BJD Barycentric Julian Date of observation
(BJD-2400000)
14- 22 F9.5 km/s RV Radial velocity
24- 30 F7.5 km/s e_RV Radial velocity error per point (1)
32- 39 F8.5 km/s FWHM Full Width at Half Maximum of each observation
41- 49 F9.6 km/s BisSpan Bisector inverse slope span of each observation
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Note (1): Note that 6m/s of Gaussian noise was added in quadrature to each
observation of every star to account for finite system stability.
Additionally, for some stars additional Gaussian noise was added in quadrature
to account for bisector variations (values given in Table A.1 and the
procedure described in Sect. 5.3).
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Acknowledgements:
David Martin, David.Martin(at)unige.ch
(End) Patricia Vannier [CDS] 03-Apr-2019