- ID:
- ivo://CDS.VizieR/J/ApJ/725/2017
- Title:
- Sloan i-band light curve of HAT-P-24
- Short Name:
- J/ApJ/725/2017
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of HAT-P-24b, a transiting extrasolar planet orbiting the moderately bright V=11.818 F8 dwarf star GSC 0774-01441, with a period P=3.3552464+/-0.0000071 days, transit epoch T_c_=2455216.97669+/-0.00024(BJD), and transit duration 3.653+/-0.025hr. The host star has a mass of 1.191+/-0.042M_{sun}_, radius of 1.317+/-0.068R_{sun}_, effective temperature 6373+/-80K, and a low metallicity of [Fe/H]=-0.16+/-0.08. The planetary companion has a mass of 0.681+/-0.031M_J_ and radius of 1.243+/-0.072R_J_ yielding a mean density of 0.439+/-0.069g/cm^3^. By repeating our global fits with different parameter sets, we have performed a critical investigation of the fitting techniques used for previous Hungarian-made Automated Telescope planetary discoveries. We find that the system properties are robust against the choice of priors.
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- ID:
- ivo://CDS.VizieR/J/AJ/152/127
- Title:
- Sloan i follow-up light curves of HATS-18
- Short Name:
- J/AJ/152/127
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery by the HATSouth network of HATS-18b: a 1.980+/-0.077M_J_, 1.337_-0.049_^+0.102^R_J_ planet in a 0.8378day orbit, around a solar analog star (mass 1.037+/-0.047M_{Sun}_ and radius 1.020_-0.031_^+0.057^R_{Sun}_) with V=14.067+/-0.040mag. The high planet mass, combined with its short orbital period, implies strong tidal coupling between the planetary orbit and the star. In fact, given its inferred age, HATS-18 shows evidence of significant tidal spin up, which together with WASP-19 (a very similar system) allows us to constrain the tidal quality factor for Sun-like stars to be in the range of 6.5<~log_10_(Q^*^/k_2_)<~7 even after allowing for extremely pessimistic model uncertainties. In addition, the HATS-18 system is among the best systems (and often the best system) for testing a multitude of star-planet interactions, be they gravitational, magnetic, or radiative, as well as planet formation and migration theories.
- ID:
- ivo://CDS.VizieR/J/ApJ/696/1950
- Title:
- Sloan iz light curves of HAT-P-10
- Short Name:
- J/ApJ/696/1950
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on the discovery of HAT-P-10b, one of the lowest mass (0.487+/-0.018M_J_) transiting extrasolar planets (TEPs) discovered to date by transit searches. HAT-P-10b orbits the moderately bright V=11.89 K dwarf GSC 02340-01714, with a period P=3.7224747+/-0.0000065d, transit epoch T_c_=2454759.68683+/-0.00016(BJD), and duration 0.1090+/-0.0008d. HAT-P-10b has a radius of 1.005^+0.032^_-0.027_R_J_ yielding a mean density of 0.594+/-0.052g/cm^3^. Comparing these observations with recent theoretical models we find that HAT-P-10b is consistent with a ~4.5Gyr, almost pure hydrogen and helium gas giant planet with a 10M_{earth}_ core. With an equilibrium temperature of T_eq_=1020+/-17K, HAT-P-10b is one of the coldest TEPs. Curiously, its Safronov number {Theta}=0.053+/-0.002 falls close to the dividing line between the two suggested TEP populations.
- ID:
- ivo://CDS.VizieR/J/A+A/628/A84
- Title:
- Slowly diffusing planetary solutions freq. analysis
- Short Name:
- J/A+A/628/A84
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Over short time-intervals, planetary ephemerides have traditionally been represented in analytical form as finite sums of periodic terms or sums of Poisson terms that are periodic terms with polynomial amplitudes. This representation is not well adapted for the evolution of planetary orbits in the solar system over million of years which present drifts in their main frequencies as a result of the chaotic nature of their dynamics. We aim to develop a numerical algorithm for slowly diffusing solutions of a perturbed integrable Hamiltonian system that will apply for the representation of chaotic planetary motions with varying frequencies. By simple analytical considerations, we first argue that it is possible to exactly recover a single varying frequency. Then, a function basis involving time-dependent fundamental frequencies is formulated in a semi-analytical way. Finally, starting from a numerical solution, a recursive algorithm is used to numerically decompose the solution into the significant elements of the function basis. Simple examples show that this algorithm can be used to give compact representations of different types of slowly diffusing solutions. As a test example, we show that this algorithm can be successfully applied to obtain a very compact approximation of the La2004 solution of the orbital motion of the Earth over 40Myr ([-35Myr,5Myr]). This example was chosen because this solution is widely used in the reconstruction of the past climates.
- ID:
- ivo://CDS.VizieR/J/ApJS/210/20
- Title:
- Small Kepler planets radial velocities
- Short Name:
- J/ApJS/210/20
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g/cm3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R_{oplus}_. Larger planets evidently contain a larger fraction of low-density material (H, He, and H_2_O).
- ID:
- ivo://CDS.VizieR/J/A+A/608/A135
- Title:
- Sodium detection in WASP-69b atmosphere
- Short Name:
- J/A+A/608/A135
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We analyze the transmission spectrum around the Na I doublet at 589nm of the extrasolar planet WASP-69b, and compare the analysis to that of the well-know hot Jupiter HD 189733b. We also present the analysis of the Rossiter-McLaughlin (RM) effect for WASP-69b. We observed two transits of WASP-69b with the HARPS-North spectrograph (R=115 000) at the TNG telescope. We perform a telluric contamination subtraction based on the comparison between the observed spectra and a telluric water model. Then, the common steps of the differential spectroscopy are followed to extract the transmission spectrum. The method is tested with archival transit data of the extensively studied exoplanet HD 189733b, obtained with the HARPS-South spectrograph at ESO 3.6m telescope, and then applied to WASP-69b data. For HD 189733b, we spectrally resolve the NaI doublet and measure line contrasts of 0.72+/-0.05% (D2) and 0.51+/-0.05% (D1), and FWHMs of 0.64+/-0.04{AA} (D2) and 0.60+/-0.06{AA} (D1), in agreement with previously published results. For WASP-69b only the contrast of the D2 line can be measured (5.8+/-0.3%). This corresponds to a detection at the 5sigma-level of excess absorption of 0.5+/-0.1% in a passband of 1.5{AA}. By measuring the RM effect, we get an angular rotation of 0.24^+0.02^_-0.01_rad/day and a sky-projected angle between the stellar rotation axis and the normal of orbit plane of 0.4^+2.0^_-1.9_{deg} FOR wasP-69b. Similar results to those previously presented in the literature are obtained for the RM analysis of HD 189733b.
- ID:
- ivo://CDS.VizieR/J/ApJS/181/351
- Title:
- Solar flux model in 30-1300nm wavelength range
- Short Name:
- J/ApJS/181/351
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Solar photon scattering probabilities (g values) have been calculated for discrete transitions in 12 species, in a format designed primarily to allow analysis of spacecraft observations from MESSENGER and BepiColombo at Mercury. The results support observations using the MESSENGER Ultraviolet and Visible Spectrometer spectrograph experiment operating over the spectral range 1150-6000{AA} and the BepiColombo spectrograph in the range 550-3150{AA}. Significant radial velocity dependence is shown for most of the emission lines, a critical factor for interpretation of the observed spectra. The g values have general application for solar system emission sources dominated by scattering of the solar flux.
- ID:
- ivo://CDS.VizieR/J/A+A/552/A78
- Title:
- Solar like stars radial velocities
- Short Name:
- J/A+A/552/A78
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In 1992 we began a precision radial velocity (RV) survey for planets around solar-like stars with the Coude Echelle Spectrograph and the Long Camera (CES LC) at the 1.4m telescope in La Silla (Chile). We have continued the survey with the upgraded CES Very Long Camera (VLC) and HARPS, both at the 3.6m telescope, until 2007. The observations for 31 stars cover a time span of up to 15 years and the RV precision permit a search for Jupiter analogues. We perform a joint analysis for variability, trends, periodicities, and Keplerian orbits and compute detection limits. Moreover, the HARPS RVs are analysed for correlations with activity indicators (CaII H&K and CCF shape). We achieve a long-term RV precision of 15m/s (CES+LC, 1992-1998), 9m/s (CES+VLC, 1999-2006), and 2.8m/s (HARPS, 2003-2009, including archive data), resp. This enables us to confirm the known planets around Iota Hor, HR 506, and HR 3259. A steady RV trend for Eps Ind A can be explained by a planetary companion. On the other hand, we find previously reported trends to be smaller for Beta Hyi and not present for Alp Men. The candidate planet Eps Eri b was not detected despite our better precision. Also the planet announced for HR 4523 cannot be confirmed. Long-term trends in several of our stars are compatible with known stellar companions. We provide a spectroscopic orbital solution for the binary HR 2400 and refined solutions for the planets around HR 506 and Iota Hor. For some other stars the variations could be attributed to stellar activity.
- ID:
- ivo://CDS.VizieR/J/A+A/615/A175
- Title:
- Solar system analogs with HARPS
- Short Name:
- J/A+A/615/A175
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The assessment of the frequency of planetary systems reproducing the solar system's architecture is still an open problem in exoplanetary science. Detailed study of multiplicity and architecture is generally hampered by limitations in quality, temporal extension and observing strategy, causing difficulties in detecting low-mass inner planets in the presence of outer giant planets. We present the results of high-cadence and high-precision HARPS observations on 20 solar-type stars known to host a single long-period giant planet in order to search for additional inner companions and estimate the occurence rate f_p_ of scaled solar system analogues - in other words, systems featuring lower-mass inner planets in the presence of long-period giant planets. We carried out combined fits of our HARPS data with literature radial velocities using differential evolution MCMC to refine the literature orbital solutions and search for additional inner planets. We then derived the survey detection limits to provide preliminary estimates of f_p_. We generally find better constrained orbital parameters for the known planets than those found in the literature; significant updates can be especially appreciated on half of the selected planetary systems. While no additional inner planet is detected, we find evidence for previously unreported long-period massive companions in systems HD 50499 and HD 73267. We finally estimate the frequency of inner low mass (10-30M_{earth}_) planets in the presence of outer giant planets as f_p_<9.84% for P<150-days. Our preliminary estimate of f_p_ is significantly lower than the literature values for similarly defined mass and period ranges; the lack of inner candidate planets found in our sample can also be seen as evidence corroborating the inwards-migration formation model for super-Earths and mini-Neptunes. Our results also underline the need for high-cadence and high-precision followup observations as the key to precisely determine the occurence of solar system analogues.
- ID:
- ivo://CDS.VizieR/J/AJ/142/19
- Title:
- Speckle observations of KOI
- Short Name:
- J/AJ/142/19
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first results from a speckle imaging survey of stars classified as candidate exoplanet host stars discovered by the Kepler mission. We use speckle imaging to search for faint companions or closely aligned background stars that could contribute flux to the Kepler light curves of their brighter neighbors. Background stars are expected to contribute significantly to the pool of false positive candidate transiting exoplanets discovered by the Kepler mission, especially in the case that the faint neighbors are eclipsing binary stars. Here, we describe our Kepler follow-up observing program, the speckle imaging camera used, our data reduction, and astrometric and photometric performance. Kepler stars range from R=8 to 16 and our observations attempt to provide background non-detection limits 5-6mag fainter and binary separations of ~0.05-2.0-arcsec. We present data describing the relative brightness, separation, and position angles for secondary sources, as well as relative plate limits for non-detection of faint nearby stars around each of 156 target stars. Faint neighbors were found near 10 of the stars.