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8131. WASP-19b secondary eclipses
ID:
ivo://CDS.VizieR/J/A+A/553/A49
Title:
WASP-19b secondary eclipses
Short Name:
J/A+A/553/A49
Date:
21 Oct 2021
Publisher:
CDS
Description:
The ASTEP (Antarctica Search for Transiting ExoPlanets) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. The WASP-19 system was observed during 24 nights in May 2010. Once brought back from Antarctica, the data were processed using various methods, the best results were with an implementation of the optimal image subtraction (OIS) algorithm.
8132. WASP-121 b Swift UVOT near-UV transit observations
ID:
ivo://CDS.VizieR/J/A+A/623/A57
Title:
WASP-121 b Swift UVOT near-UV transit observations
Short Name:
J/A+A/623/A57
Date:
21 Oct 2021
Publisher:
CDS
Description:
Close-in gas planets are subject to continuous photoevaporation that can erode their volatile envelopes. Today, ongoing mass loss has been confirmed in a few individual systems via transit observations in the ultraviolet spectral range. We demonstrate that the Ultraviolet/Optical Telescope (UVOT) onboard the Neil Gehrels Swift Observatory enables photometry to a relative accuracy of about 0.5% and present the first near-UV (200-270nm, NUV) transit observations of WASP-121 b, a hot Jupiter with one of the highest predicted mass-loss rates. The data cover the orbital phases 0.85 to 1.15 with three visits. We measure a broad-band NUV transit depth of 2.10+/-0.29%. While still consistent with the optical value of 1.55%, the NUV data indicate excess absorption of 0.55% at a 1.9-sigma level. Such excess absorption is known from the WASP-12 system, and both of these hot Jupiters are expected to undergo mass loss at extremely high rates. With a CLOUDY simulation, we show that absorption lines of Fe II in a dense extended atmosphere can cause broad-band NUV absorption at the 0.5% level. Given the numerous lines of low-ionization metals, the NUV range is a promising tracer of photoevaporation in the hottest gas planets.
8133. WASP-43b thirty eclipses
ID:
ivo://CDS.VizieR/J/A+A/542/A4
Title:
WASP-43b thirty eclipses
Short Name:
J/A+A/542/A4
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present twenty-three transit light curves and seven occultation light curves for the ultra-short period planet WASP-43 b, in addition to eight new measurements of the radial velocity of the star. Thanks to this extensive data set, we improve significantly the parameters of the system.
8134. WASP-4b transit griz light curves
ID:
ivo://CDS.VizieR/J/A+A/539/A159
Title:
WASP-4b transit griz light curves
Short Name:
J/A+A/539/A159
Date:
21 Oct 2021
Publisher:
CDS
Description:
Ground-based simultaneous multiband transit observations allow an accurate system parameter determination and may lead to the detection and characterization of additional bodies via the transit timing variations (TTVs) method. We aim to (i) characterize the heavily bloated WASP-4b hot Jupiter and its star by measuring system parameters and the dependence of the planetary radius as a function of four (Sloan g', r', i', z') wavelengths and (ii) search for TTVs.
8135. WASP-12b transits
ID:
ivo://CDS.VizieR/J/A+A/528/A65
Title:
WASP-12b transits
Short Name:
J/A+A/528/A65
Date:
21 Oct 2021
Publisher:
CDS
Description:
The transiting extrasolar planet WASP-12b was found to be the one of the most intensely irradiated exoplanets. It is unexpectedly bloated and is losing mass which may accrete into the host star. Our aim was to refine parameters of this intriguing system and search for signs of transit timing variations. We gathered high-precision light curves of two transits of WASP-12b. Assuming various limb darkening laws, we generated best-fitting models and redetermined parameters of the system. Error estimates were derived by the prayer bread method and Monte Carlo simulations. System's parameters obtained by us were found to agree with previous studies within one sigma. Use of the non-linear limb darkening laws resulted in the best- fitting models. With two new mid-transit times, the ephemeris was refined to BJD_TDB_=(2454508.97682+/-0.00020)+(1.09142245+/-0.00000033)E. Interestingly, indications for transit timing variation were detected at the level of 3.4 sigma. This signal could be induced by an additional planet in the system. Simplified numerical simulations showed that a perturber could be a terrestrial-type planet if both planets are in a low-order orbital resonance. However, we emphasise that further observations are needed to confirm variation and to put constraints on properties of the perturber.
8136. WASP-69b, WASP-70Ab and WASP-84b
ID:
ivo://CDS.VizieR/J/MNRAS/445/1114
Title:
WASP-69b, WASP-70Ab and WASP-84b
Short Name:
J/MNRAS/445/1114
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of the transiting exoplanets WASP-69b, WASP-70Ab and WASP-84b, each of which orbits a bright star (V~10). WASP-69b is a bloated Saturn-mass planet (0.26M_Jup_, 1.06R_Jup_) in a 3.868-d period around an active, ~1-Gyr, mid-K dwarf. ROSAT detected X-rays 60+/-27" from WASP-69. If the star is the source then the planet could be undergoing mass-loss at a rate of ~10^12^g/s. This is one to two orders of magnitude higher than the evaporation rate estimated for HD 209458b and HD 189733b, both of which have exhibited anomalously large Lyman {alpha} absorption during transit. WASP-70Ab is a sub-Jupiter-mass planet (0.59M_Jup_, 1.16R_Jup_) in a 3.713-d orbit around the primary of a spatially resolved, 9-10-Gyr, G4+K3 binary, with a separation of 3.3 arcsec ( >=800AU). WASP-84b is a sub-Jupiter-mass planet (0.69M_Jup_, 0.94R_Jup_) in an 8.523-d orbit around an active, ~1-Gyr, early-K dwarf. Of the transiting planets discovered from the ground to date, WASP-84b has the third-longest period. For the active stars WASP-69 and WASP-84, we pre-whitened the radial velocities using a low-order harmonic series. We found that this reduced the residual scatter more than did the oft-used method of pre-whitening with a fit between residual radial velocity and bisector span. The system parameters were essentially unaffected by pre-whitening.
8137. WASP-161b, WASP-163b and WASP-170b
ID:
ivo://CDS.VizieR/J/AJ/157/43
Title:
WASP-161b, WASP-163b and WASP-170b
Short Name:
J/AJ/157/43
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the discovery by the WASP-South transit survey of three new transiting hot Jupiters, WASP-161 b, WASP-163 b and WASP-170 b. Follow-up radial velocities obtained with the Euler/CORALIE spectrograph and high-precision transit light curves obtained with the TRAPPIST-North, TRAPPIST-South, SPECULOOS-South, NITES, and Euler telescopes have enabled us to determine the masses and radii for these transiting exoplanets. WASP-161 b completes an orbit around its V=11.1 F6V-type host star in 5.406 days, and has a mass and radius of 2.5+/-0.2M_Jup_ and 1.14+/-0.06R_Jup_ respectively. WASP-163 b has an orbital period of 1.609-days, a mass of 1.9+/-0.2M_Jup_, and a radius of 1.2+/-0.1R_Jup_. Its host star is a V=12.5 G8-type dwarf. WASP-170 b is on a 2.344-days orbit around a G1V-type star of magnitude V=12.8. It has a mass of 1.7+/-0.2M_Jup_ and a radius of 1.14+/-0.09R_Jup_. Given their irradiations (~10^9^erg/s/cm^2^) and masses, the three new planets' sizes are in good agreement with classical structure models of irradiated giant planets.
8138. WASP-151b, WASP-153b, WASP-156b
ID:
ivo://CDS.VizieR/J/A+A/610/A63
Title:
WASP-151b, WASP-153b, WASP-156b
Short Name:
J/A+A/610/A63
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of three transiting exoplanets by the SuperWASP survey and the SOPHIE spectrograph with mass and radius determined with a precision better than 15%. WASP-151b and WASP-153b are two hot Saturns with masses, radii, densities and equilibrium temperatures of 0.31^+0.04^_-0.03_M_J_, 1.13^+0.03^_-0.03_R_J_, 0.22^+0.03^_-0.02_rho_J_ and 1,290^+20^_-10_K, and 0.39^+0.02^_-0.02_M_J_, 1.55^+0.10^_-0.08_R_J_, 0.11^+0.02^_-0.02{rho}_J_ and 1,700^+40^ _-40_K, respectively. Their host stars are early G type stars (with magV ~ 13) and their orbital periods are 4.53 and 3.33 days, respectively. WASP-156b is a Super-Neptune orbiting a K type star (magV = 11.6). It has a mass of 0.128^+0.010^_-0.009_M_J_, a radius of 0.51^+0.02^_ -0.02 R_J_, a density of 1.0^+0.1^_-0.1_{rho}_J_, an equilibrium temperature of 970^+30^_-20_K and an orbital period of 3.83 days.
8139. WASP-68b, WASP-73b, WASP-88b transits
ID:
ivo://CDS.VizieR/J/A+A/563/A143
Title:
WASP-68b, WASP-73b, WASP-88b transits
Short Name:
J/A+A/563/A143
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery by the WASP transit survey of three new hot Jupiters, WASP-68 b, WASP-73 b and WASP-88 b. WASP-68 b has a mass of 0.95+/-0.03M_Jup_, a radius of 1.24_-0.06_^+0.10^R_Jup_, and orbits a V=10.7 G0-type star (1.24+/-0.03M_{sun}_, 1.69_-0.06_^+0.11^R_{sun}_, Teff=5911+/-60K) with a period of 5.084298+/-0.000015-days. Its size is typical of hot Jupiters with similar masses. WASP-73 b is significantly more massive (1.88_-0.06_^+0.07^M_Jup_) and slightly larger (1.16_-0.08_^+0.12^R_Jup_) than Jupiter. It orbits a V=10.5 F9-type star (1.34_-0.04_^+0.05^M_{sun}_, 2.07_-0.08_^+0.19^R_{sun}_, Teff=6036+/-120K) every 4.08722+/-0.00022-days. Despite its high irradiation (2.3*10^9^erg/s/cm^2^), WASP-73 b has a high mean density (1.20_-0.30_^+0.26^{rho}_Jup_) that suggests an enrichment of the planet in heavy elements. WASP-88 b is a 0.56+/-0.08M_Jup_ planet orbiting a V=11.4 F6-type star (1.45+/-0.05M_{sun}_, 2.08_-0.06_^+0.12^R_{sun}_, Teff=6431+/-130K) with a period of 4.954000+/-0.000019-days. With a radius of 1.70_-0.07_^+0.13^R_Jup_, it joins the handful of planets with super-inflated radii. The ranges of ages we determine through stellar evolution modeling are 4.5-7.0Gyr for WASP-68, 2.8-5.7Gyr for WASP-73 and 1.8-4.3Gyr for WASP-88. WASP-73 appears to be a significantly evolved star, close to or already in the subgiant phase. WASP-68 and WASP-88 are less evolved, although in an advanced stage of core H-burning.
8140. WASP-80b wavelength-binned light curves
ID:
ivo://CDS.VizieR/J/MNRAS/474/876
Title:
WASP-80b wavelength-binned light curves
Short Name:
J/MNRAS/474/876
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have performed ground-based transmission spectroscopy of the hot Jupiter orbiting the cool dwarf WASP-80 using the ACAM instrument on the William Herschel Telescope (WHT) as part of the Low-Resolution Ground-Based Exoplanet Atmosphere Survey using Transmission Spectroscopy programme. This is the third paper of a ground-based transmission spectroscopy survey of hot Jupiters using low-resolution grism spectrographs. We observed two transits of the planet and have constructed transmission spectra spanning a wavelength range of 4640-8840{AA}. Our transmission spectrum is inconsistent with a previously claimed detection of potassium in WASP-80b's atmosphere, and is instead most consistent with a haze. We also do not see evidence for sodium absorption at a resolution of 100{AA}.