- ID:
- ivo://CDS.VizieR/J/ApJ/726/52
- Title:
- HAT-P-18 and HAT-P-19 follow-up
- Short Name:
- J/ApJ/726/52
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of two new transiting extrasolar planets. HAT-P-18b orbits the V=12.759 K2 dwarf star GSC 2594-00646, with a period P=5.508023+/-0.000006 days, transit epoch T_c_=2454715.02174+/-0.00020(BJD), and transit duration 0.1131+/-0.0009 days. The host star has a mass of 0.77+/-0.03M_{sun}_, radius of 0.75+/-0.04R_{sun}_, effective temperature 4803+/-80K, and metallicity [Fe/H]=+0.10+/-0.08. The planetary companion has a mass of 0.197+/-0.013M_J_ and radius of 0.995+/-0.052R_J_, yielding a mean density of 0.25+/-0.04g/cm^3^. HAT-P-19b orbits the V=12.901 K1 dwarf star GSC 2283-00589, with a period P=4.008778+/-0.000006 days, transit epoch T_c_=2455091.53417+/-0.00034(BJD), and transit duration 0.1182+/-0.0014 days. The host star has a mass of 0.84+/-0.04M_{sun}_, radius of 0.82+/-0.05R_{sun}_, effective temperature 4990+/-130K, and metallicity [Fe/H]=+0.23+/-0.08. The planetary companion has a mass of 0.292+/-0.018M_J_ and radius of 1.132+/-0.072R_J_, yielding a mean density of 0.25+/-0.04g/cm^3^. The radial velocity residuals for HAT-P-19 exhibit a linear trend in time, which indicates the presence of a third body in the system. Comparing these observations with theoretical models, we find that HAT-P-18b and HAT-P-19b are each consistent with a hydrogen-helium-dominated gas giant planet with negligible core mass. HAT-P-18b and HAT-P-19b join HAT-P-12b and WASP-21b in an emerging group of low-density Saturn-mass planets, with negligible inferred core masses. However, unlike HAT-P-12b and WASP-21b, both HAT-P-18b and HAT-P-19b orbit stars with super-solar metallicity.
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/742/59
- Title:
- HAT-P-32 and HAT-P-33 follow-up
- Short Name:
- J/ApJ/742/59
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V=11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P=2.150008+/-0.000001d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (~80m/s). Assuming a circular orbit, the star has a mass of 1.16+/-0.04M_{sun}_ and radius of 1.22+/-0.02R_{sun}_, while the planet has a mass of 0.860+/-0.164M_J_ and a radius of 1.789+/-0.025R_J_. The second planet, HAT-P-33b, orbits the bright V=11.188 late-F dwarf star GSC 2461-00988, with a period P=3.474474+/-0.000001d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (~50m/s). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to ~35m/s. We find that the star has a mass of 1.38+/-0.04M_{sun}_ and a radius of 1.64+/-0.03R_{sun}_ while the planet has a mass of 0.762+/-0.101M_J_ and a radius of 1.686+/-0.045R_J_ for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.
- ID:
- ivo://CDS.VizieR/J/ApJ/735/24
- Title:
- HAT-P-30 follow-up photometry
- Short Name:
- J/ApJ/735/24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of HAT-P-30b, a transiting exoplanet orbiting the V=10.419 dwarf star GSC 0208-00722. The planet has a period P=2.810595+/-0.000005 days, transit epoch T_c_=2455456.46561+/-0.00037 (BJD), and transit duration 0.0887+/-0.0015 days. The host star has a mass of 1.24+/-0.04M_{sun}_, radius of 1.21+/-0.05R_{sun}_, effective temperature of 6304+/-88K, and metallicity [Fe/H]=+0.13+/-0.08. The planetary companion has a mass of 0.711+/-0.028M_J_ and radius of 1.340+/-0.065R_J_ yielding a mean density of 0.37+/-0.05g/cm^3^. We also present radial velocity measurements that were obtained throughout a transit that exhibit the Rossiter-McLaughlin effect. By modeling this effect, we measure an angle of {lambda}=73.5+/-9.0{deg} between the sky projections of the planet's orbit normal and the star's spin axis. HAT-P-30b represents another example of a close-in planet on a highly tilted orbit, and conforms to the previously noted pattern that tilted orbits are more common around stars with T_eff*_>~6250K.
- ID:
- ivo://CDS.VizieR/J/AJ/144/139
- Title:
- HAT-P-39, HAT-P-40, and HAT-P-41 follow-up
- Short Name:
- J/AJ/144/139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of three new transiting extrasolar planets orbiting moderately bright (V=11.1, 11.7, and 12.4) F stars. The planets HAT-P-39b through HAT-P-41b have periods of P=3.5439days, 4.4572days, and 2.6940days, masses of 0.60M_J_, 0.62M_J_, and 0.80M_J_, and radii of 1.57R_J_, 1.73R _J_, and 1.68R_J_, respectively. They orbit stars with masses of 1.40 M _{sun}_, 1.51 M_{sun}_, and 1.51 M_{sun}_, respectively. The three planets are members of an emerging population of highly inflated Jupiters with 0.4M_J_<M<1.5M_J_ and R>1.5R_J_.
- ID:
- ivo://CDS.VizieR/J/AJ/147/128
- Title:
- HAT-P-44, HAT-P-45, and HAT-P-46 follow-up
- Short Name:
- J/AJ/147/128
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery by the HATNet survey of three new transiting extrasolar planets orbiting moderately bright (V=13.2, 12.8, and 11.9) stars. The planets have orbital periods of 4.3012, 3.1290, and 4.4631 days, masses of 0.35, 0.89, and 0.49M_J_, and radii of 1.24, 1.43, and 1.28R_J_. The stellar hosts have masses of 0.94, 1.26, and 1.28M_{sun}_. Each system shows significant systematic variations in its residual radial velocities, indicating the possible presence of additional components. Based on its Bayesian evidence, the preferred model for HAT-P-44 consists of two planets, including the transiting component, with the outer planet having a period of 872 days, eccentricity of 0.494+/-0.081, and a minimum mass of 4.0M_J_. Due to aliasing we cannot rule out alternative solutions for the outer planet having a period of 220 days or 438 days. For HAT-P-45, at present there is not enough data to justify the additional free parameters included in a multi-planet model; in this case a single-planet solution is preferred, but the required jitter of 22.5+/-6.3m/s is relatively high for a star of this type. For HAT-P-46 the preferred solution includes a second planet having a period of 78 days and a minimum mass of 2.0M_J_, however the preference for this model over a single-planet model is not very strong. While substantial uncertainties remain as to the presence and/or properties of the outer planetary companions in these systems, the inner transiting planets are well characterized with measured properties that are fairly robust against changes in the assumed models for the outer planets. Continued radial velocity monitoring is necessary to fully characterize these three planetary systems, the properties of which may have important implications for understanding the formation of hot Jupiters.
- ID:
- ivo://CDS.VizieR/J/ApJ/749/134
- Title:
- HAT-P-17 radial velocities and light curves
- Short Name:
- J/ApJ/749/134
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of HAT-P-17b,c, a multi-planet system with an inner transiting planet in a short-period, eccentric orbit and an outer planet in a 4.4 yr, nearly circular orbit. The inner planet, HAT-P-17b, transits the bright V=10.54 early K dwarf star GSC 2717-00417, with an orbital period P=10.338523+/-0.000009 days, orbital eccentricity e=0.342+/-0.006, transit epoch T_c_=2454801.16943+/-0.00020 (BJD: barycentric Julian dates throughout the paper are calculated from Coordinated Universal Time (UTC)), and transit duration 0.1690+/-0.0009 days. HAT-P-17b has a mass of 0.534+/-0.018M_J_ and radius of 1.010+/-0.029R_J_ yielding a mean density of 0.64+/-0.05g/cm3. This planet has a relatively low equilibrium temperature in the range 780-927K, making it an attractive target for follow-up spectroscopic studies. The outer planet, HAT-P-17c, has a significantly longer orbital period P_2_=1610+/-20d and a minimum mass m_2_sini_2_=1.31^+0.18^_-0.15_M_J_. The orbital inclination of HAT-P-17c is unknown as transits have not been observed and may not be present. The host star has a mass of 0.86+/-0.04M_{sun}_, radius of 0.84+/-0.02R_{sun}_, effective temperature 5246+/-80K, and metallicity [Fe/H]=0.00+/-0.08. HAT-P-17 is the second multi-planet system detected from ground-based transit surveys.
- ID:
- ivo://CDS.VizieR/J/A+A/527/L11
- Title:
- HAT-P-6 radial velocity curve
- Short Name:
- J/A+A/527/L11
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We observed with the SOPHIE spectrograph (OHP, France) the transit of the HAT-P-6b exoplanet across its host star. The resulting stellar radial velocities display the Rossiter-McLaughlin anomaly and reveal a retrograde orbit: the planetary orbital spin and the stellar rotational spin point towards approximately opposite directions.
- ID:
- ivo://CDS.VizieR/J/A+A/580/A63
- Title:
- HATS-13b and HATS-14b light and RV curves
- Short Name:
- J/A+A/580/A63
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of HATS-13b and HATS-14b, two hot-Jupiter transiting planets discovered by the HATSouth survey. The host stars are quite similar to each other (HATS-13: V=13.9 mag, M*=0.96M_{sun}_, R*=0.89R_{sun}_, Teff=5500K, [Fe/H]=0.05; HATS-14: V=13.8mag, M*=0.97M_{sun}_, R*=0.93R_{sun}_, Teff=5350K, [Fe/H]=0.33) and both the planets orbit around them with a period of roughly 3 days and a separation of roughly 0.04 au. However, even though they are irradiated in a similar way, the physical characteristics of the two planets are very different. HATS-13b, with a mass of Mp=0.543M_Jup_ and a radius of Rp=1.212R_Jup_, appears as an inflated planet, while HATS-14b, having a mass of Mp=1.071M_Jup_ and a radius of Rp=1.039R_Jup_, is only slightly larger in radius than Jupiter.
- ID:
- ivo://CDS.VizieR/J/MNRAS/477/3406
- Title:
- HATS-39b, 40b, 41b and 42b transit data
- Short Name:
- J/MNRAS/477/3406
- Date:
- 04 Feb 2022 06:26:57
- Publisher:
- CDS
- Description:
- We report the discovery of four transiting hot Jupiters from the HATSouth survey: HATS-39b, HATS-40b, HATS-41b, and HATS-42b. These discoveries add to the growing number of transiting planets orbiting moderately bright (12.5<=V<=13.7) F dwarf stars on short (2-5d) periods. The planets have similar radii, ranging from 1.33^+0.29^_-0.20_R_J_ for HATS-41b to 1.58^+0.16^_-0.12_R_J_ for HATS-40b. Their masses and bulk densities, however, span more than an order of magnitude. HATS-39b has a mass of 0.63+/-0.13M_J_, and an inflated radius of 1.57+/-0.12R_J_, making it a good target for future transmission spectroscopic studies. HATS-41b is a very massive 9.7+/-1.6M_J_ planet and one of only a few hot Jupiters found to date with a mass over 5M_J_. This planet orbits the highest metallicity star ([Fe/H]=0.470+/-0.010) known to host a transiting planet and is also likely on an eccentric orbit. The high mass, coupled with a relatively young age (1.34^+0.31^_-0.51_Gyr) for the host star, is a factor that may explain why this planet's orbit has not yet circularized.
- ID:
- ivo://CDS.VizieR/J/AJ/155/119
- Title:
- HATSouth-K2 C7 transiting/eclipsing systems
- Short Name:
- J/AJ/155/119
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on the result of a campaign to monitor 25 HATSouth candidates using the Kepler space telescope during Campaign 7 of the K2 mission. We discover HATS-36b (EPIC 215969174b, K2-145b), an eccentric (e=0.105+/-0.028) hot Jupiter with a mass of 3.216+/-0.062 M_J_ and a radius of 1.235+/-0.043 R_J_, which transits a solar-type G0V star (V=14.386) in a 4.1752-day period. We also refine the properties of three previously discovered HATSouth transiting planets (HATS-9b, HATS-11b, and HATS-12b) and search the K2 data for TTVs and additional transiting planets in these systems. In addition, we also report on a further three systems that remain as Jupiter-radius transiting exoplanet candidates. These candidates do not have determined masses, however pass all of our other vetting observations. Finally, we report on the 18 candidates that we are now able to classify as eclipsing binary or blended eclipsing binary systems based on a combination of the HATSouth data, the K2 data, and follow-up ground-based photometry and spectroscopy. These range in periods from 0.7 day to 16.7 days, and down to 1.5 mmag in eclipse depths. Our results show the power of combining ground-based imaging and spectroscopy with higher precision space-based photometry, and serve as an illustration as to what will be possible when combining ground-based observations with TESS data.
