- 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.
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Search Results
- 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.
- 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.
- 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.
- ID:
- ivo://CDS.VizieR/J/MNRAS/446/2428
- Title:
- WASP-31b:HST/Spitzer transmission spectral survey
- Short Name:
- J/MNRAS/446/2428
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present Hubble Space Telescope optical and near-IR transmission spectra of the transiting hot-Jupiter WASP-31b. The spectrum covers 0.3-1.7 {mu}m at a resolution R~70, which we combine with Spitzer photometry to cover the full-optical to IR. The spectrum is dominated by a cloud deck with a flat transmission spectrum which is apparent at wavelengths >0.52{mu}m. The cloud deck is present at high altitudes and low pressures, as it covers the majority of the expected optical Na line and near-IR H_2_O features. While Na I absorption is not clearly identified, the resulting spectrum does show a very strong potassium feature detected at the 4.2{sigma} confidence level. Broadened alkali wings are not detected, indicating pressures below ~10 mbar. The lack of Na and strong K is the first indication of a sub-solar Na/K abundance ratio in a planetary atmosphere (ln[Na/K]=-3.3+/-2.8), which could potentially be explained by Na condensation on the planet's night side, or primordial abundance variations. A strong Rayleigh scattering signature is detected at short wavelengths, with a 4{sigma} significant slope. Two distinct aerosol size populations can explain the spectra, with a smaller sub-micron size grain population reaching high altitudes producing a blue Rayleigh scattering signature on top of a larger, lower lying population responsible for the flat cloud deck at longer wavelengths. We estimate that the atmospheric circulation is sufficiently strong to mix micron size particles upwards to the required 1-10 mbar pressures, necessary to explain the cloud deck. These results further confirm the importance of clouds in hot Jupiters, which can potentially dominate the overall spectra and may alter the abundances of key gaseous species.
- ID:
- ivo://CDS.VizieR/J/A+A/625/A136
- Title:
- WASP-18b HST/WFC3 spectroscopic phase curves
- Short Name:
- J/A+A/625/A136
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the analysis of a full-orbit, spectroscopic phase curve of the ultra hot Jupiter (UHJ) WASP-18b, obtained with the Wide Field Camera 3 aboard the Hubble Space Telescope. We measured the normalised day-night contrast of the planet as >0.96 in luminosity: the disc-integrated dayside emission from the planet is at 964+/-25ppm, corresponding to 2894+/-30K, and we place an upper limit on the nightside emission of <32ppm or 1430K at the 3{sigma}level. We also find that the peak of the phase curve exhibits a small, but significant oset in brightness of 4.5+/-0.5 degrees eastward. We compare the extracted phase curve and phase-resolved spectra to 3D global circulation models and find that broadly the data can be well reproduced by some of these models. We find from this comparison several constraints on the atmospheric properties of the planet. Firstly we find that we need ecient drag to explain the very inefficient day-night recirculation observed.We demonstrate that this drag could be due to Lorentz-force drag by a magnetic field as weak as 10 gauss. Secondly, we show that a high metallicity is not required to match the large day-night temperature contrast. In fact, the effect of metallicity on the phase curve is different from cooler gas-giant counterparts because of the high-temperature chemistry in the atmosphere of WASP-18b. Additionally, we compared the current UHJ spectroscopic phase curves, WASP-18b and WASP-103b, and show that these two planets provide a consistent picture with remarkable similarities in their measured and inferred properties. However, key differences in these properties, such as their brightness osets and radius anomalies, suggest that UHJ could be used to separate between competing theories for the inflation of gas-giant planets.
- ID:
- ivo://CDS.VizieR/J/A+A/530/A5
- Title:
- WASP-4b Ks-band detection of thermal emission
- Short Name:
- J/A+A/530/A5
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Secondary eclipses are a powerful tool to measure directly the thermal emission from extrasolar planets, and to constrain their type and physical parameters. We started a project to obtain reliable broad-band measurements of the thermal emission of transiting exoplanets. Ground-based high-cadence near-infrared relative photometry was used to obtain a sub-millimagnitude precision light curve of a secondary eclipse of WASP-4b -- a 1.12M_J_ hot Jupiter on a 1.34-day orbit around G7V star. The data show a clear ~10{sigma} detection of the planet's thermal emission at 2.2{mu}. The calculated thermal emission corresponds to a fractional eclipse depth of 0.185^+0.014^_-0.013_%, with a related brightness temperature in Ks of T_B_=1995+/-40K, centered at Tc=2455102.61162^+0.00071^_-0.00077_HJD. We could set a limit on the eccentricity of e*cos{omega}=0.0027+/-0.0018, compatible with a near-circular orbit. The calculated brightness temperature, and the specific models suggest a highly inefficient redistribution of heat from the day-side to the night-side of the planet, and a consequent emission mainly from the day-side. The high-cadence ground-based technique is capable of detecting the faint signal of the secondary eclipse of extrasolar planets, which makes it a valuable complement to space-based mid-IR observations.
- ID:
- ivo://CDS.VizieR/J/A+A/615/A86
- Title:
- WASP-48b Ks-band occultation lightcurves
- Short Name:
- J/A+A/615/A86
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report a detection of thermal emission from the hot Jupiter WASP-48b in the Ks-band. We used the Wide-field Infra-red Camera on the 3.6-m Canada-France Hawaii Telescope to observe an occultation of the planet by its host star. From the resulting occultation lightcurve we find a planet-to-star contrast ratio in the Ks-band of 0.136+/-0.014% , in agreement with the value of 0.109+/-0.027% previously determined. We fit the two Ks-band occultation lightcurves simultaneously with occultation lightcurves in the H-band and the Spitzer 3.6-um and 4.5-um bandpasses, radial velocity data, and transit lightcurves. From this, we revise the system parameters and construct the spectral energy distribution (SED) of the dayside atmosphere. By comparing the SED with atmospheric models, we find that both models with and without a thermal inversion are consistent with the data. We find the planet's orbit to be consistent with circular (e<0.072 at 3 sigma).
23039. 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.
23040. WASP-21b light curves
- ID:
- ivo://CDS.VizieR/J/MNRAS/497/5182
- Title:
- WASP-21b light curves
- Short Name:
- J/MNRAS/497/5182
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the optical transmission spectrum of the highly inflated Saturn- mass exoplanet WASP-21b, using three transits obtained with the ACAM instrument on the William Herschel Telescope through the LRG-BEASTS survey (Low Resolution Ground-Based Exoplanet Atmosphere Survey using Transmission Spectroscopy). Our transmission spectrum covers a wavelength range of 4635-9000{AA}, achieving an average transit depth precision of 197ppm compared to one atmospheric scale height at 246ppm. We detect NaI absorption in a bin width of 30{AA}, at >4{sigma} confidence, which extends over 100{AA}. We see no evidence of absorption from KI. Atmospheric retrieval analysis of the scattering slope indicates it is too steep for Rayleigh scattering from H_2, but is very similar to that of HD 189733b. The features observed in our transmission spectrum cannot be caused by stellar activity alone, with photometric monitoring of WASP-21 showing it to be an inactive star. We therefore conclude that aerosols in the atmosphere of WASP-21b are giving rise to the steep slope that we observe, and that WASP-21b is an excellent target for infra-red observations to constrain its atmospheric metallicity.
