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8111. WASP-64b and WASP-72b light curves
ID:
ivo://CDS.VizieR/J/A+A/552/A82
Title:
WASP-64b and WASP-72b light curves
Short Name:
J/A+A/552/A82
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery by the WASP transit survey of two new highly irradiated giant planets. WASP-64 b is slightly more massive (1.271+/-0.068M_Jup_) and larger (1.271+/-0.039R_Jup_) than Jupiter, and is in very-short (a=0.02648+/-0.00024AU, P=1.5732918+/-0.0000015-days) circular orbit around a V=12.3 G7-type dwarf (1.004+/-0.028M_{sun}_, 1.058+/-0.025R_{sun}_, Teff=5500+/-150K). Its size +0.059 is typical of hot Jupiters with similar masses. WASP-72 b has also a mass a bit higher than Jupiter's (1.461-0.056M_Jup_) and orbits very close (0.03708+/-0.00050AU, P=2.2167421+/-0.0000081days) to a bright (V=9.6) and moderately evolved F7-type star (1.386+/-0.055M_{sun}_, 1.98+/-0.24R_{sun}_, Teff=6250+/-100K). Despite its extreme irradiation (~5.5x10^9^erg/s/cm^2^), WASP-72 b has a moderate size (1.27+/-0.20R_Jup_) that could suggest a significant enrichment in heavy elements. Nevertheless, the errors on its physical parameters are still too high to draw any strong inference on its internal structure or its possible peculiarity.
8112. WASP-39b and WASP-43b light curves
ID:
ivo://CDS.VizieR/J/PASP/127/143
Title:
WASP-39b and WASP-43b light curves
Short Name:
J/PASP/127/143
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present photometric light-curves of the transiting extrasolar planets WASP-39b and WASP-43b obtained with three San Pedro Martir telescopes by using the defocused photometry technique.
8113. WASP-104b and WASP-106b photometry
ID:
ivo://CDS.VizieR/J/A+A/570/A64
Title:
WASP-104b and WASP-106b photometry
Short Name:
J/A+A/570/A64
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery from the WASP survey of two exoplanetary systems, each consisting of a Jupiter-sized planet transiting an 11th magnitude (V) main-sequence star. WASP-104b orbits its star in 1.75d, whereas WASP-106b has the fourth-longest orbital period of any planet discovered by means of transits observed from the ground, orbiting every 9.29d. Each planet is more massive than Jupiter (WASP-104b has a mass of 1.27+/-0.05M_Jup_, while WASP-106b has a mass of 1.93+/-0.08M_Jup_). Both planets are just slightly larger than Jupiter, with radii of 1.14+/-0.04 and 1.09+/-0.04R_Jup_ for WASP-104 and WASP-106 respectively. No significant orbital eccentricity is detected in either system, and while this is not surprising in the case of the short-period WASP-104b, it is interesting in the case of WASP-106b, because many otherwise similar planets are known to have eccentric orbits.
8114. WASP-20b and WASP-28b photometry and RV
ID:
ivo://CDS.VizieR/J/A+A/575/A61
Title:
WASP-20b and WASP-28b photometry and RV
Short Name:
J/A+A/575/A61
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of the planets WASP-20b and WASP-28b along with measurements of their sky-projected orbital obliquities. WASP-20b is an inflated, Saturn-mass planet (0.31M_Jup_; 1.46R_Jup_) in a 4.9-day, near-aligned (lambda=12.7+/-4.2{deg}) orbit around CD-24 102 (V=10.7; F9). Due to the low density of the planet and the apparent brightness of the host star, WASP-20 is a good target for atmospheric characterisation via transmission spectroscopy. WASP-28b is an inflated, Jupiter-mass planet (0.91M_Jup_; 1.21R_Jup_) in a 3.4-day, near-aligned (lambda=8+/-18{deg}) orbit around a V=12, F8 star. As intermediate-mass planets in short orbits around aged, cool stars (7^+2^_-1_Gyr and 6000+/-100K for WASP-20; 5^+3^_-2_Gyr and 6100+/-150K for WASP-28), their orbital alignment is consistent with the hypothesis that close-in giant planets are scattered into eccentric orbits with random alignments, which are then circularised and aligned with their stars' spins via tidal dissipation.
8115. WASP-147b, 160Bb, 164b, and 165b phot. and RV
ID:
ivo://CDS.VizieR/J/MNRAS/482/301
Title:
WASP-147b, 160Bb, 164b, and 165b phot. and RV
Short Name:
J/MNRAS/482/301
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of four transiting hot Jupiters, WASP-147, WASP-160B, WASP-164, and WASP-165 from the WASP survey. WASP-147b is a near Saturn-mass (Mp=0.28M_J_) object with a radius of 1.11R_J_ orbiting a G4 star with a period (of 4.6d. WASP-160Bb has a mass and radius (Mp=0.28M_J_, Rp=1.09R_J_) (near-identical to WASP-147b, but is less irradiated, orbiting a metal-rich ([Fe/H]*=0.27) K0 star with a period of 3.8d. WASP-160B is part of a near equal-mass visual binary with an on-sky separation of 28.5 arcsec. WASP-164b is a more massive (Mp=2.13M_J_, Rp=1.13R_J_) hot Jupiter, orbiting a G2 star on a close-in (P=1.8d), but tidally stable orbit. WASP-165b is a classical (Mp=0.66M_J_, Rp=1.26R_J_) hot Jupiter in a 3.5d period orbit around a metal-rich ([Fe/H]*=0.33) star. WASP-147b and WASP-160Bb are promising targets for atmospheric characterization through transmission spectroscopy, while WASP-164b presents a good target for emission spectroscopy.
8116. WASP-49b FORS2 multi-epoch spectra
ID:
ivo://CDS.VizieR/J/A+A/587/A67
Title:
WASP-49b FORS2 multi-epoch spectra
Short Name:
J/A+A/587/A67
Date:
21 Oct 2021
Publisher:
CDS
Description:
Transmission spectroscopy has proven to be a useful tool for the study of exoplanet atmospheres, because the absorption and scattering signatures of the atmosphere manifest themselves as variations in the planetary transit depth. Several planets have been studied with this technique, leading to the detection of a small number of elements and molecules (Na, K, H_2_O), but also revealing that many planets show flat transmission spectra consistent with the presence of opaque high-altitude clouds. We apply this technique to the Mp=0.40 M_jup_, Rp=1.20R_jup_, P=2.78d planet WASP-49b, aiming to characterize its transmission spectrum between 0.73 and 1um and search for the features of K and H_2_O. Owing to its density and temperature, the planet is predicted to possess an extended atmosphere and is thus a good target for transmission spectroscopy. Three transits of WASP-49b have been observed with the FORS2 instrument installed at the VLT/UT1 telescope at the ESO Paranal site. We used FORS2 in MXU mode with grism GRIS_600z, producing simultaneous multiwavelength transit light curves throughout the i' and z' bands. We combined these data with independent broadband photometry from the Euler and TRAPPIST telescopes to obtain a good measurement of the transit shape. Strong correlated noise structures are present in the FORS2 light curves, which are due to rotating flat-field structures that are introduced by inhomogeneities of the linear atmospheric dispersion corrector's transparency. We accounted for these structures by constructing common noise models from the residuals of light curves bearing the same noise structures and used them together with simple parametric models to infer the transmission spectrum. We present three independent transmission spectra of WASP-49b between 0.73 and 1.02um, as well as a transmission spectrum between 0.65 and 1.02um from the combined analysis of FORS2 and broadband data. The results obtained from the three individual epochs agree well. The transmission spectrum of WASP-49b is best fit by atmospheric models containing a cloud deck at pressure levels of 1mbar or lower.
8117. WASP-43b g'r'i'z'JHK light curves
ID:
ivo://CDS.VizieR/J/A+A/563/A40
Title:
WASP-43b g'r'i'z'JHK light curves
Short Name:
J/A+A/563/A40
Date:
21 Oct 2021
Publisher:
CDS
Description:
We observed one transit and one occultation of the hot Jupiter WASP-43b simultaneously in the g'r'i'z'JHK bands using the GROND instrument on the MPG/ESO 2.2-meter telescope. From the transit event, we have independently derived WASP-43's system parameters with high precision, and improved the period to be 0.81347437(13) days. No significant variation in transit depths is detected, with the largest deviations coming from the i', H, and K bands. Given the observational uncertainties, the broad-band transmission spectrum can be explained by either (i) a flat featureless straight line that indicates thick clouds, (ii) synthetic spectra with absorption signatures of atomic Na/K or molecular TiO/VO that in turn indicate cloud-free atmosphere, or (iii) a Rayleigh scattering profile that indicates high-altitude hazes. From the occultation event, we detected planetary dayside thermal emission in the K-band with a flux ratio of 0.197+/-0.042%, which confirms previous detections obtained in the 2.09 micron narrow band and Ks-band. The K-band brightness temperature 1878^+108^_-116_K favors an atmosphere with poor day- to nightside heat redistribution. We also have a marginal detection in the i'-band (0.037^+0.023^_-0.021_%), which is either a false positive, a signature of non-blackbody radiation at this wavelength, or an indication of reflective hazes at high altitude.
8118. WASP-46b g'r'i'z'JHK occultation light curves
ID:
ivo://CDS.VizieR/J/A+A/567/A8
Title:
WASP-46b g'r'i'z'JHK occultation light curves
Short Name:
J/A+A/567/A8
Date:
21 Oct 2021
Publisher:
CDS
Description:
We aim to construct a spectral energy distribution (SED) for the emission from the dayside atmosphere of the hot Jupiter WASP-46b and to investigate its energy budget. We observed a secondary eclipse of WASP-46b simultaneously in the g'r'i'z'JHK bands using the GROND instrument on the MPG/ESO 2.2m telescope. Eclipse depths of the acquired light curves were derived to infer the brightness temperatures at multibands that cover the SED peak. We report the first detection of the thermal emission from the dayside of WASP-46b in the K band at 4.2-sigma level and tentative detections in the H (2.5-sigma) and J (2.3-sigma) bands, with flux ratios of 0.253^+0.063^_-0.060_%, 0.194+/-0.078%, and 0.129+/-0.055%, respectively. The derived brightness temperatures (2306^+177^_-187_K, 2462^+245^_-302_K, and 2453^+198^_-258_K, respectively) are consistent with an isothermal temperature profile of 2386K, which is significantly higher than the dayside-averaged equilibrium temperature, indicative of very poor heat redistribution efficiency. We also investigate the tentative detections in the g'r'i' bands and the 3-sigma upper limit in the z' band, which might indicate the existence of reflective clouds if these tentative detections do not arise from systematics.
8119. WASP-71b light curve
ID:
ivo://CDS.VizieR/J/A+A/552/A120
Title:
WASP-71b light curve
Short Name:
J/A+A/552/A120
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery by the WASP transit survey of a highly-irradiated, massive (2.242+/-0.080M_Jup_) planet which transits a bright (V=10.6), evolved F8 star every 2.9-days. The planet, WASP-71b, is larger than Jupiter (1.46+/-0.13R_Jup_), but less dense (0.71+/-0.16{rho}_Jup_). We also report spectroscopic observations made during transit with the CORALIE spectrograph, which allow us to make a highly-significant detection of the Rossiter-McLaughlin effect. We determine the sky-projected angle between the stellar-spin and planetary-orbit axes to be {lambda}=20.1+/-9.7degrees, i.e. the system is "aligned", according to the widely-used alignment criteria that systems are regarded as misaligned only when {lambda} is measured to be greater than 10 degrees with 3-{sigma} confidence.
8120. WASP-19b light curves
ID:
ivo://CDS.VizieR/J/A+A/552/A2
Title:
WASP-19b light curves
Short Name:
J/A+A/552/A2
Date:
21 Oct 2021
Publisher:
CDS
Description:
The sample of hot Jupiters that have been studied in great detail is still growing. In particular, when the planet transits its host star, it is possible to measure the planetary radius and the planet mass (with radial velocity data). For the study of planetary atmospheres, it is essential to obtain transit and occultation measurements at multiple wavelengths. We aim to characterize the transiting hot Jupiter WASP-19b by deriving accurate and precise planetary parameters from a dedicated observing campaign of transits and occultations. We have obtained a total of 14 transit lightcurves in the r'-Gunn, I-Cousins, z'-Gunn, and I+z' filters and 10 occultation lightcurves in z'-Gunn using EulerCam on the Euler-Swiss telescope and TRAPPIST. We also obtained one lightcurve through the narrow-band NB1190 filter of HAWK-I on the VLT measuring an occultation at 1.19 micron. We performed a global MCMC analysis of all new data, together with some archive data in order to refine the planetary parameters and to measure the occultation depths in z'-band and at 1.19 micron. We measure a planetary radius of R_p_=1.376+/-0.046R_J_, a planetary mass of M_p_=1.165+/-0.068M_J_, and find a very low eccentricity of e=0.0077(-0.0032/+0.0068), compatible with a circular orbit. We have detected the z'-band occultation at 3 sigma significance and measure it to be delta_F_occ,z'=352+/-116ppm, more than a factor of 2 smaller than previously published. The occultation at 1.19 micron is only marginally constrained at delta_F_occ,NB1190=1711(-726/+745)ppm. We show that the detection of occultations in the visible range is within reach, even for 1m class telescopes if a considerable number of individual events are observed. Our results suggest an oxygen-dominated atmosphere of WASP-19b, making the planet an interesting test case for oxygen-rich planets without temperature inversion.