- ID:
- ivo://CDS.VizieR/J/MNRAS/464/1247
- Title:
- VVV high proper motion stars. I. Ks<=13.5 stars
- Short Name:
- J/MNRAS/464/1247
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Knowledge of the stellar content near the Sun is important for a broad range of topics ranging from the search for planets to the study of Milky Way (MW) structure. The most powerful method for identifying potentially nearby stars is proper motion (PM) surveys. All old optical surveys avoid, or are at least substantially incomplete, near the Galactic plane. The depth and breadth of the 'VISTA Variables in Via Lactea' (VVV) near-IR survey significantly improves this situation. Taking advantage of the VVV survey data base, we have measured PMs in the densest regions of the MW bulge and southern plane in order to complete the census of nearby objects. We have developed a custom PM pipeline based on VVV catalogues from the Cambridge Astronomy Survey Unit, by comparing the first epoch of JHKs with the multi-epoch Ks bands acquired later. Taking advantage of the large time baseline between the Two Micron All Sky Survey (2MASS) and the VVV observations, we also obtained 2MASS-VVV PMs. We present a near-IR PM catalogue for the whole area of the VVV survey, which includes 3003 moving stellar sources. All of these have been visually inspected and are real PM objects. Our catalogue is in very good agreement with the PM data supplied in IR catalogues outside the densest zone of the MW. The majority of the PM objects in our catalogue are nearby M-dwarfs, as expected. This new data base allows us to identify 57 common PM binary candidates, among which are two new systems within 30 pcof the Sun.
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/572/A49
- Title:
- WASP-94AB photometry and radial velocities
- Short Name:
- J/A+A/572/A49
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of two hot-Jupiter planets, one orbiting each star of a wide binary system. WASP-94A (2MASS 20550794-3408079) is an F8 type star hosting a transiting planet with a radius of 1.72+/-0.06R_Jup_, a mass of 0.445+/ 0.026M_Jup_ and an orbital period of 3.95 days. The Rossiter-McLaughlin effect is clearly detected and the measured projected spin-orbit angle indicates that the planet occupies a retrograde orbit. WASP-94B (2MASS 20550915-3408078) is an F9 stellar companion at an angular separation of 15" (projected separation 2700AU), hosting a gas giant of minimum mass 0.617+/-0.028M_Jup_ with a period of 2.008-days, detected by Doppler measurements. The orbital planes of the two planets are inclined relative to each other, indicating that at least one of them is inclined relative to the plane of the stellar binary. These hot Jupiters in a binary system bring new insights into the formation of close-in giant planets and the role of stellar multiplicity.
- ID:
- ivo://CDS.VizieR/J/AcA/68/371
- Title:
- WASP and KELT planet transits
- Short Name:
- J/AcA/68/371
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Theoretical calculations and some indirect observations show that massive exoplanets on tight orbits must decay due to tidal dissipation within their host stars. This orbital evolution could be observationally accessible through precise transit timing over a course of decades. The rate of planetary in-spiraling may not only help us to understand some aspects of evolution of planetary systems, but also can be used as a probe of the stellar internal structure. In this paper we present results of transit timing campaigns organized for a carefully selected sample of the Northern hemisphere hot Jupiter-like planets which were found to be the best candidates for detecting planet-star tidal interactions. Among them, there is the WASP-12 system which is the best candidate for possessing an in-falling giant exoplanet. Our new observations support the scenario of orbital decay of WASP-12 b and allow us to refine its rate. The derived tidal quality parameter of the host star Q'*=(1.82+/-0.32)x10^5^ is in agreement with theoretical predictions for subgiant stars. For the remaining systems - HAT-P-23, KELT-1, KELT-16, WASP-33, and WASP-103 - our transit timing data reveal no deviations from the constant-period models, hence constraints on the individual rates of orbital decay were placed. The tidal quality parameters of host stars in at least four systems - HAT-P-23, KELT-1, WASP-33, and WASP-103 - were found to be greater than the value reported for WASP-12. This is in line with the finding that those hosts are main sequence stars, for which efficiency of tidal dissipation is predicted to be relatively weak.
- ID:
- ivo://CDS.VizieR/J/A+A/599/A3
- Title:
- WASP 127, 136 and 138 RV and light curves
- Short Name:
- J/A+A/599/A3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report three newly discovered exoplanets from the SuperWASP survey. WASP-127b is a heavily inflated super-Neptune of mass 0.18+/-0.02 M_J_ and radius 1.37+/-0.04 R_J_. This is one of the least massive planets discovered by the WASP project. It orbits a bright host star (Vmag=10.16) of spectral type G5 with a period of 4.17 days. WASP-127b is a low-density planet that has an extended atmosphere with a scale height of 2500+/-400km, making it an ideal candidate for transmission spectroscopy. WASP-136b and WASP-138b are both hot Jupiters with mass and radii of 1.51+/-0.08M_J_ and 1.38+/-0.16R_J_, and 1.22+/-0.08M_J_ and 1.09+/-0.05R_J_, respectively. WASP-136b is in a 5.22-day orbit around an F9 subgiant star with a mass of 1.41+/-0.07M_{sun}_ and a radius of 2.21+/-0.22R_{sun}_. The discovery of WASP-136b could help constrain the characteristics of the giant planet population around evolved stars. WASP-138b orbits an F7 star with a period of 3.63 days. Its radius agrees with theoretical values from standard models, suggesting the presence of a heavy element core with a mass of ~10M_{earth}_. The discovery of these new planets helps in exploring the diverse compositional range of short-period planets, and will aid our understanding of the physical characteristics of both gas giants and low-density planets.
- 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.
- 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/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/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/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.
