- 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.
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Search Results
- ID:
- ivo://CDS.VizieR/J/AcA/71/223
- Title:
- HAT-P-36 T80, T100 light curves and O-C
- Short Name:
- J/AcA/71/223
- Date:
- 10 Dec 2021 00:45:52
- Publisher:
- CDS
- Description:
- We study the most precise light curves of the planet-host HAT-P-36 that we obtained from the ground primarily with a brand-new 80cm telescope (T80) very recently installed at Ankara University Kreiken Observatory (AUKR) of Turkey and also from the space with Transiting Exoplanet Survey Satellite (TESS). The main objective of the study is to analyze the Transit Timing Variations (TTV) observed in the hot-Jupiter type planet HAT-P-36 b, a strong candidate for orbital decay, based on our own observations as well as that have been acquired by professional and amateur observers since its discovery (Bakos et al., 2012AJ....144...19B, Cat. J/AJ/144/19). HAT-P-36 displays out-of-transit variability as well as light curve anomalies during the transits of its planet due to stellar spots. We collected and detrended all the complete transit light curves we had access to from these anomalies, which we modeled with EXOFAST (Eastman et al., 2013PASP..125...83E) and measured the mid-transit times forming a homogeneous data set for a TTV analysis. We found an increase in the orbital period of HAT-P-36 b at a rate of 0.014 seconds per year from the best fitting quadratic function, which is only found in the TTV constructed by making use of the mid-transit times measured from detrended light curves, against an expectation of an orbital decay based on its parameters. We refined the values of these system parameters by modelling the Spectral Energy Distribution of the host star, its archival radial velocity observations from multiple instruments, and most precise transit light curves from the space and the ground covering a wide range of wavelengths with EXOFASTv2 (Eastman, 2017, ascl, 1710, 003). We also analyzed the out-of-transit variability from TESS observations to search for potential rotational modulations through a frequency analysis. We report a statistically significant periodicity in the TESS light curve at 4.22+/-0.02 days, which might have been caused by instrumental systematics but should be tracked in the future observations of the target.
- 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/A+A/558/A55
- Title:
- HATS-2b griz light curves
- Short Name:
- J/A+A/558/A55
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of HATS-2b, the second transiting extrasolar planet detected by the HATSouth survey. HATS- 2b is moving on a circular orbit around a V=13.6mag, K-type dwarf star (GSC 6665-00236), at a separation of 0.0230+/-0.0003AU and with a period of 1.3541-days. The planetary parameters have been robustly determined using a simultaneous t of the HATSouth, MPG/ESO 2.2m/GROND, Faulkes Telescope South/Spectral transit photometry, and MPG/ESO 2.2m/FEROS, Euler 1.2m/CORALIE, AAT 3.9m/CYCLOPS radial-velocity measurements.
- 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.
- ID:
- ivo://CDS.VizieR/J/AJ/155/114
- Title:
- HAT-TR-318-007: a double-lined M dwarf binary
- Short Name:
- J/AJ/155/114
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery by the HATNet survey of HAT-TR-318-007, a P=3.34395390+/-0.00000020 day period detached double-lined M dwarf binary with total secondary eclipses. We combine radial velocity (RV) measurements from TRES/FLWO 1.5 m and time-series photometry from HATNet, FLWO 1.2 m, BOS 0.8 m, and NASA K2 Campaign 5, to determine the masses and radii of the component stars: M_A_=0.448+/-0.011 M_{sun}_^N^, M_B_=0.2721_-0.0042_^+0.0041^ M_{sun}_^N^, R_A_=0.4548_-0.0036_^+0.0035^ R_{sun}_^N^, and R_B_=0.2913_-0.0024_^+0.0023^ R_{sun}_^N^. We obtained a FIRE/Magellan near-infrared spectrum of the primary star during a total secondary eclipse, and we use this to obtain disentangled spectra of both components. We determine spectral types of ST_A_=M3.71+/-0.69 and ST_B_=M5.01+/-0.73 and effective temperatures of T_eff,A_=3190+/-110 K and T_eff,B_=3100+/-110 K for the primary and secondary star, respectively. We also measure a metallicity of [Fe/H]=+0.298+/-0.080 for the system. We find that the system has a small, but significant, nonzero eccentricity of 0.0136+/-0.0026. The K2 light curve shows a coherent variation at a period of 3.41315_-0.00032_^+0.00030^ days, which is slightly longer than the orbital period, and which we demonstrate comes from the primary star. We interpret this as the rotation period of the primary. We perform a quantitative comparison between the Dartmouth stellar evolution models and the seven systems, including HAT-TR-318-007, that contain M dwarfs with 0.2 M_{sun}_^N^<M<0.5 M_{sun}_^N^, have metallicity measurements, and have masses and radii determined to better than 5% precision. Discrepancies between the predicted and observed masses and radii are found for three of the systems.
- ID:
- ivo://CDS.VizieR/J/A+A/371/908
- Title:
- Havlen-Moffat No. 1 UBVRI photometry
- Short Name:
- J/A+A/371/908
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A deep CCD UBVRI photometric survey combined with UBVRI polarimetric observations of 21 bright stars was carried out in the region of the open cluster Havlen-Moffat No. 1. Our data reveal that the extinction law in this cluster es variable and that six cluster stars show very high polarisation values (>4%), probably because of the presence of a nearby small dust cloud. The cluster is at a distance of d=3300pc, it is 2-4Myr old and the initial mass function of its most massive stars (M>3M_{sun}_) has a flat slope of x about of 0.7. As an additional result, it was possible to reconcile the absolute magnitudes of the two WN7-type members using the R-values valid in the regions where they are located.
- ID:
- ivo://CDS.VizieR/J/ApJS/201/19
- Title:
- Hawaii Infrared Parallax Program. I.
- Short Name:
- J/ApJS/201/19
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Astrometry and photometry for 318 ultracool dwarfs in 265 systems that have measured trigonometric parallaxes. To be included in this tabulation, an object must have a spectral type >=M6 or a K-band absolute magnitude >8.5mag. Parallaxes, proper motions, and coordinates at a specified epoch are given for all objects. Photometric measurements in MKO, 2MASS, Spitzer, and WISE systems are given when available. Various other flags that provide additional information about the object or photometry are included.
- ID:
- ivo://CDS.VizieR/J/ApJ/833/96
- Title:
- Hawaii infrared parallax program. II. Ultracool dwarfs
- Short Name:
- J/ApJ/833/96
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a large, uniform analysis of young (~10-150Myr) ultracool dwarfs, based on new high-precision infrared (IR) parallaxes for 68 objects. We find that low-gravity (VL-G) late-M and L dwarfs form a continuous sequence in IR color-magnitude diagrams, separate from the field population and from current theoretical models. These VL-G objects also appear distinct from young substellar (brown dwarf and exoplanet) companions, suggesting that the two populations may have a different range of physical properties. In contrast, at the L/T transition, young, old, and spectrally peculiar objects all span a relatively narrow range in near-IR absolute magnitudes. At a given spectral type, the IR absolute magnitudes of young objects can be offset from ordinary field dwarfs, with the largest offsets occurring in the Y and J bands for late-M dwarfs (brighter than the field) and mid-/late-L dwarfs (fainter than the field). Overall, low-gravity (VL-G) objects have the most uniform photometric behavior, while intermediate gravity (INT-G) objects are more diverse, suggesting a third governing parameter beyond spectral type and gravity class. We examine the moving group membership for all young ultracool dwarfs with parallaxes, changing the status of 23 objects (including 8 previously identified planetary-mass candidates) and fortifying the status of another 28 objects. We use our resulting age-calibrated sample to establish empirical young isochrones and show a declining frequency of VL-G objects relative to INT-G objects with increasing age. Notable individual objects in our sample include high-velocity (>~100km/s) INT-G objects, very red late-L dwarfs with high surface gravities, candidate disk-bearing members of the MBM20 cloud and {beta} Pic moving group, and very young distant interlopers. Finally, we provide a comprehensive summary of the absolute magnitudes and spectral classifications of young ultracool dwarfs, using a combined sample of 102 objects found in the field and as substellar companions to young stars.
