J/MNRAS/465/3693 7 WASP-South transiting exoplanets (Hellier+, 2017)
WASP-South transiting exoplanets: WASP-130b, WASP-131b, WASP-132b, WASP-139b,
WASP-140b, WASP-141b and WASP-142b.
Hellier C., Anderson D.R., Collier Cameron A., Delrez L., Gillon M.,
Jehin E., Lendl M., Maxted P.F.L., Neveu-vanmalle M., Pepe F., Pollacco D.,
Queloz D., Segransan D., Smalley B., Southworth J., Triaud A.H.M.J.,
Udry S., Wagg T., West R.G.
<Mon. Not. R. Astron. Soc., 465, 3693-3707 (2017)>
=2017MNRAS.465.3693H 2017MNRAS.465.3693H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities
Keywords: stars: individual: WASP-130, WASP-131, WASP-132, WASP-139, WASP-140,
WASP-141, WASP-142 - planetary systems
Abstract:
We describe seven exoplanets transiting stars of brightness
V=10.1-12.4. WASP-130b is a 'warm Jupiter' having an orbital period of
11.6d around a metal-rich G6 star. Its mass and radius
(1.23±0.04MJup and 0.89±0.03RJup) support the trend that warm
Jupiters have smaller radii than hot Jupiters. WASP-131b is a bloated
Saturn-mass planet (0.27MJup and 1.22RJup). Its large scaleheight
and bright (V=10.1) host star make it a good target for atmospheric
characterization. WASP-132b (0.41MJup and 0.87RJup) is among the
least irradiated and coolest of WASP planets, having a 7.1-d orbit
around a K4 star. WASP-139b is a 'super-Neptune' akin to HATS-7b and
HATS-8b, being the lowest mass planet yet found by WASP (0.12MJup
and 0.80RJup). The metal-rich K0 host star appears to be anomalously
dense, akin to HAT-P-11. WASP-140b is a 2.4MJup planet in an
eccentric (e=0.047±0.004) 2.2d orbit. The planet's radius is large
(1.4RJup), but uncertain owing to the grazing transit (b=0.93). The
10.4d rotation period of the K0 host star suggests a young age, and
the time-scale for tidal circularization is likely to be the lowest of
all known eccentric hot Jupiters. WASP-141b (2.7MJup, 1.2RJup and
P=3.3d) and WASP-142b (0.84MJup, 1.53RJup and P=2.1d) are typical
hot Jupiters orbiting metal-rich F stars. We show that the period
distribution within the hot-Jupiter bulge does not depend on the
metallicity of the host star.
Description:
The ongoing WASP surveys continue to discover novel objects which push
the bounds of known exoplanets (e.g. the rapid circularization
time-scale of WASP-140b) along with planets transiting bright stars
which are good targets for atmospheric characterization (e.g.
WASP-131b, with a V=10.1 star). We also present the longest period
(WASP-130b), lowest mass (WASP-139b) and second-coolest (WASP-132b) of
WASP-discovered planets. We also demonstrate the power of WASP
photometry in the possible detection of a 0.4-mmag rotational
modulation of the star WASP-132.
We present radial velocities of seven exoplanets transiting stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 110 7 List of studied stars
tablea1.dat 46 194 Radial velocities
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name WASP name
10- 35 A26 --- 1SWASP 1SWASP name (1SWASP JHHMMSS/ss+DDMMSS.s)
37- 59 A23 --- 2MASS 2MASS name (2MASS HHMMSSss+DDMMSSs)
60- 61 I2 h RAh Right ascension (J2000)
63- 64 I2 min RAm Right ascension (J2000)
66- 70 F5.2 s RAs Right ascension (J2000)
72 A1 --- DE- Declination sign (J2000)
73- 74 I2 deg DEd Declination (J2000)
76- 77 I2 arcmin DEm Declination (J2000)
79- 82 F4.1 arcsec DEs Declination (J2000)
84- 87 F4.1 mag Vmag V magnitude
89- 93 F5.1 mas/yr pmRA Proper motion along RA
95- 97 F3.1 mas/yr e_pmRA rms uncertainty on pmRA
99-103 F5.1 mas/yr pmDE proper motion along DE
105-107 F3.1 mas/yr e_pmDE rms uncertainty on pmDE
109-110 A2 --- SpType Spectral type
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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- 8 A8 --- Name WASP name
10 A1 --- Inst [CH] C for Coralie, H for Harps
12- 22 F11.5 d BJD Baricentric Julain date (BJD-2400000)
24- 31 F8.4 km/s RV Radial velocity
33- 38 F6.4 km/s e_RV rms uncertainty on RV
40- 46 F7.4 km/s Bis Bisector span (Bisector errors are twice RV errors)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Mar-2019