- ID:
- ivo://CDS.VizieR/J/MNRAS/434/1300
- Title:
- WASP-15 and WASP-16 light curves
- Short Name:
- J/MNRAS/434/1300
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new photometric observations of WASP-15 and WASP-16, two transiting extrasolar planetary systems with measured orbital obliquities but without photometric follow-up since their discovery papers. Our new data for WASP-15 comprise observations of one transit simultaneously in four optical passbands using GROND on the MPG/European Southern Observatory (ESO) 2.2m telescope, plus coverage of half a transit from DFOSC on the Danish 1.54m telescope, both at ESO La Silla. For WASP-16 we present observations of four complete transits, all from the Danish telescope. We use these new data to refine the measured physical properties and orbital ephemerides of the two systems. Whilst our results are close to the originally determined values for WASP-15, we find that the star and planet in the WASP-16 system are both larger and less massive than previously thought.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/586/A93
- Title:
- WASP41 and WASP47 photometric and RV data
- Short Name:
- J/A+A/586/A93
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of two additional planetary companions to WASP-41 and WASP-47. WASP-41c is a planet of minimum mass 3.18+/-0.20M_Jup_ and eccentricity 0.29+/-0.02, and it orbits in 421+/-2-days. WASP-47c is a planet of minimum mass 1.24+/-0.22M_Jup_ and eccentricity 0.13+/-0.10, and it orbits in 572+/-7-days. Unlike most of the planetary systems that include a hot Jupiter, these two systems with a hot Jupiter have a long-period planet located at only about 1AU from their host star. WASP-41 is a rather young star known to be chromospherically active. To differentiate its magnetic cycle from the radial velocity effect induced by the second planet, we used the emission in the Halpha line and find this indicator well suited to detecting the stellar activity pattern and the magnetic cycle. The analysis of the Rossiter-McLaughlin effect induced by WASP-41b suggests that the planet could be misaligned, though an aligned orbit cannot be excluded. WASP-47 has recently been found to host two additional transiting super Earths. With such an unprecedented architecture, the WASP-47 system will be very important for understanding planetary migration.
- 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.
- 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.
- 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.
- 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.
- 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.
- 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.
- 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.
- 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.
