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24491. WASP-42 and WASP-49 photometry and velocities
ID:
ivo://CDS.VizieR/J/A+A/544/A72
Title:
WASP-42 and WASP-49 photometry and velocities
Short Name:
J/A+A/544/A72
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of two new transiting planets from the WASP survey. WASP-42 b is a 0.500+/-0.035M_Jup_ planet orbiting a K1 star at a separation of 0.0548+/-0.0017AU with a period of 4.9816872+/-7.3x10^-6^days. The radius of WASP-42 b is 1.080+/-0.057R_Jup_ while its equilibrium temperature is T_eq_=995+/-34K. We detect some evidence for a small but non-zero eccentricity of e=0.060+/-0.013. WASP-49 b is a 0.378+/-0.027M_Jup_ planet around an old G6 star. It has a period of 2.7817387+/-5.6x10^-6^days and a separation of 0.0379+/-0.0011AU. This planet is slightly bloated, having a radius of 1.115+/-0.047R_Jup_ and an equilibrium temperature of T_eq_=1369+/-39K. Both planets have been followed up photometrically, and in total we have obtained 5 full and one partial transit light curves of WASP-42 and 4 full and one partial light curves of WASP-49 using the Euler-Swiss, TRAPPIST and Faulkes South telescopes.
24492. WASP-22 and WASP-26 photometry and velocities
ID:
ivo://CDS.VizieR/J/A+A/534/A16
Title:
WASP-22 and WASP-26 photometry and velocities
Short Name:
J/A+A/534/A16
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report on spectroscopic and photometric observations through transits of the exoplanets WASP-22b and WASP-26b, intended to determine the systems' spin-orbit angles. We combine these data with existing data to refine the system parameters. We measure a sky-projected spin-orbit angle of 22+/-16 degrees for WASP-22b, showing the planet's orbit to be prograde and, perhaps, slightly misaligned. We do not detect the Rossiter-McLaughlin effect of WASP-26b due to its low amplitude and observation noise. We place 3-sigma upper limits on orbital eccentricity of 0.063 for WASP-22b and 0.050 for WASP-26b. After refining the drift in the systemic velocity of WASP-22 found by Maxted et al. (2010AJ....140.2007M), we find the third body in the system to have a separation-scaled minimum-mass of 5.3+/-0.3M_Jup_ (a3/5AU)^2^, where a3 is the orbital separation of the third body.
24493. WASP78 and WASP79 RV and photometric data
ID:
ivo://CDS.VizieR/J/A+A/547/A61
Title:
WASP78 and WASP79 RV and photometric data
Short Name:
J/A+A/547/A61
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of WASP-78b and WASP-79b, two highly-bloated Jupiter-mass exoplanets orbiting F-type host stars. WASP-78b orbits its V=12.0 host star (TYC 5889-271-1) every 2.175 days and WASP-79b orbits its V=10.1 host star (CD-30 1812) every 3.662 days. Planetary parameters have been determined using a simultaneous fit to WASP and TRAPPIST transit photometry and CORALIE radial-velocity measurements. For WASP-78b a planetary mass of 0.89+/-0.08M_Jup_ and a radius of 1.70+/-0.11R_Jup_ is found. The planetary equilibrium temperature of T_P_=2350+/-80K for WASP-78b makes it one of the hottest of the currently known exoplanets. WASP-79b its found to have a planetary mass of 0.90+/-0.08M_Jup_, but with a somewhat uncertain radius due to lack of sufficient TRAPPIST photometry. The planetary radius is at least 1.70+/-0.11R_Jup_, but could be as large as 2.09+/-0.14R_Jup_, which would make WASP-79b the largest known exoplanet.
24494. WASP-18A, WASP-19, WASP-77A photometry
ID:
ivo://CDS.VizieR/J/A+A/636/A98
Title:
WASP-18A, WASP-19, WASP-77A photometry
Short Name:
J/A+A/636/A98
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present 22 new transit observations of the exoplanets WASP-18Ab, WASP-19b, and WASP-77Ab, from the Transit Monitoring in the South (TraMoS) project. We simultaneously model our newly collected transit light curves with archival photometry and radial velocity data to obtain refined physical and orbital parameters. We include TESS light curves of the three exoplanets to perform an extended analysis of the variations in their transit mid-time (TTV) and to refine their planetary orbital ephemeris. We did not find significant TTVRMS variations larger than 47, 65, and 86 seconds for WASP-18Ab, WASP-19b, and WASP-77Ab, respectively. Dynamical simulations were carried out to constrain the masses of a possible perturber. The observed mean square (RMS) could be produced by a perturber body with an upper limit mass of 9, 2.5, 11 and 4M_{Earth}_ in 1:2, 1:3, 2:1, and 3:1 resonances in the WASP-18Ab system. In the case of WASP-19b, companions with masses up to 0.26, 0.65, 1, and 2.8M_{Earth}_, in 1:2, 2:1, 3:1, and 5:3 resonances respectively, produce the RMS. For the WASP-77Ab system, this RMS could be produced by a planet with mass in the range of 1.5-9M_{Earth}_ in 1:2, 1:3, 2:1, 2:3, 3:1, 3:5, or 5:3 resonances. Comparing our results with RV variations, we discard massive companions with 350M_{Earth}_ in 17:5 resonance for WASP-18Ab, 95M_{Earth}_ in 4:1 resonance for WASP-19b, and 105M_{Earth}_ in 5:2 resonance for WASP-77Ab. Finally, using a Lomb-Scargle period search we find no evidence of a periodic trend on our TTV data for the three exoplanets.
24495. WASP-11b
ID:
ivo://CDS.VizieR/J/A+A/502/395
Title:
WASP-11b
Short Name:
J/A+A/502/395
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report the discovery of a sub-Jupiter mass exoplanet transiting a magnitude V=11.6 host star 1SWASP J030928.54+304024.7. ************************************************************************** * * * Sorry, but the author(s) never supplied the tabular material * * announced in the paper * * * **************************************************************************
24496. WASP-31b and host star radius compared with IMACS
ID:
ivo://CDS.VizieR/J/AJ/160/230
Title:
WASP-31b and host star radius compared with IMACS
Short Name:
J/AJ/160/230
Date:
10 Dec 2021
Publisher:
CDS
Description:
We present a new optical (400-950nm) transmission spectrum of the hot Jupiter WASP-31b (M=0.48M_Jup_; R=1.54R_Jup_; P=3.41days), obtained by combining four transit observations. These transits were observed with IMACS on the Magellan Baade Telescope at Las Campanas Observatory as part of the ACCESS project. We investigate the presence of clouds/hazes in the upper atmosphere of this planet, as well as the contribution of stellar activity on the observed features. In addition, we search for absorption features of the alkali elements NaI and KI, with particular focus on KI, for which there have been two previously published disagreeing results. Observations with Hubble Space Telescope (HST)/STIS detected KI, whereas ground-based low- and high- resolution observations did not. We use equilibrium and nonequilibrium chemistry retrievals to explore the planetary and stellar parameter space of the system with our optical data combined with existing near-IR observations. Our best-fit model is that with a scattering slope consistent with a Rayleigh slope ({alpha}=5.3_-3.1_^+2.9^), high-altitude clouds at a log cloud top pressure of -3.6_-2.1_^+2.7^bars, and possible muted H2O features. We find that our observations support other ground-based claims of no KI. Clouds are likely why signals like H2O are extremely muted and Na or K cannot be detected. We then juxtapose our Magellan/IMACS transmission spectrum with existing VLT/FORS2, HST/WFC3, HST/STIS, and Spitzer observations to further constrain the optical-to-infrared atmospheric features of the planet. We find that a steeper scattering slope ({alpha}=8.3{+/-}1.5) is anchored by STIS wavelengths blueward of 400nm and only the original STIS observations show significant potassium signal.
24497. WASP-12b and WASP-43b griz light curves
ID:
ivo://CDS.VizieR/J/A+A/630/A89
Title:
WASP-12b and WASP-43b griz light curves
Short Name:
J/A+A/630/A89
Date:
21 Oct 2021
Publisher:
CDS
Description:
The TESS and PLATO missions are expected to find vast numbers of new transiting planet candidates. However, only a fraction of these candidates will be legitimate planets, and the candidate validation will require a significant amount of follow-up resources. Radial velocity (RV) follow-up study can be carried out only for the most promising candidates around bright, slowly rotating, stars. Thus, before devoting RV resources to candidates, they need to be vetted using cheaper methods, and, in the cases for which an RV confirmation is not feasible, the candidate's true nature needs to be determined based on these alternative methods alone. We study the applicability of multicolour transit photometry in the validation of transiting planet candidates when the candidate signal arises from a real astrophysical source (transiting planet, eclipsing binary, etc.), and not from an instrumental artefact. Particularly, we aim to answer how securely we can estimate the true uncontaminated star-planet radius ratio when the light curve may contain contamination from unresolved light sources inside the photometry aperture when combining multicolour transit observations with a physics-based contamination model in a Bayesian parameter estimation setting. More generally, we study how the contamination level, colour differences between the planet host and contaminant stars, transit signal-to-noise ratio, and available prior information affect the contamination and true radius ratio estimates. The study is based on simulations and ground-based multicolour transit observations. The contamination analyses were carried out with a contamination model integrated into the PYTRANSIT V2 transit modelling package, and the observations were carried out with the MuSCAT2 multicolour imager installed in the 1.5m Telescopio Carlos Sanchez in the Teide Observatory, in Tenerife. We show that multicolour transit photometry can be used to estimate the amount of flux contamination and the true radius ratio. Combining the true radius ratio with an estimate for the stellar radius yields the true absolute radius of the transiting object, which is a valuable quantity in statistical candidate validation, and enough in itself to validate a candidate whose radius falls below the theoretical lower limit for a brown dwarf.
24498. 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.
24499. 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.
24500. 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.

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