- ID:
- ivo://CDS.VizieR/J/ApJ/714/462
- Title:
- Inclination change of TrES-2b
- Short Name:
- J/ApJ/714/462
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- On 2009 June 15 UT the transit of TrES-2b was detected using the University of Arizona's 1.55m Kuiper Telescope with 2.0-2.5 millimag rms accuracy in the I band. We find a central transit time of T_c_=2454997.76286+/-0.00035HJD, an orbital period of P=2.4706127+/-0.0000009 days, and an inclination angle of i=83.92{deg}+/-0.05{deg}, which is consistent with our re-fit of the original I-band light curve of O'Donovan et al. where we find i=83.84{deg}+/-0.05{deg}. We calculate an insignificant inclination change of {Delta}i =-0.08{deg}+/-0.07{deg} over the last three years, and as such, our observations rule out, at the ~11{sigma} level, the apparent change of orbital inclination to i_predicted_=83.35{deg}+/-0.1{deg} as predicted by Mislis & Schmitt and Mislis et al. for our epoch. Moreover, our analysis of a recently published Kepler Space Telescope light curve for TrES-2b finds an inclination of i=83.91{deg}+/-0.03{deg} for a similar epoch. These Kepler results definitively rule out change in i as a function of time. Indeed, we detect no significant changes in any of the orbital parameters of TrES-2b.
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Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/144/42
- Title:
- Infrared photometry of 90 KOIs
- Short Name:
- J/AJ/144/42
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- All transiting planets are at risk of contamination by blends with nearby, unresolved stars. Blends dilute the transit signal, causing the planet to appear smaller than it really is, or produce a false-positive detection when the target star is blended with eclipsing binary stars. This paper reports on high spatial-resolution adaptive optics images of 90 Kepler planetary candidates. Companion stars are detected as close as 0.1" from the target star. Images were taken in the near-infrared (J and Ks bands) with ARIES on the MMT and PHARO on the Palomar Hale 200inch telescope. Most objects (60%) have at least one star within 6" separation and a magnitude difference of 9. Eighteen objects (20%) have at least one companion within 2" of the target star; six companions (7%) are closer than 0.5". Most of these companions were previously unknown, and the associated planetary candidates should receive additional scrutiny. Limits are placed on the presence of additional companions for every system observed, which can be used to validate planets statistically using the BLENDER method. Validation is particularly critical for low-mass, potentially Earth-like worlds, which are not detectable with current-generation radial velocity techniques. High-resolution images are thus a crucial component of any transit follow-up program.
- ID:
- ivo://CDS.VizieR/J/A+A/585/A126
- Title:
- 3 irradiated and bloated hot Jupiters RV and phot.
- Short Name:
- J/A+A/585/A126
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on three new transiting hot Jupiter planets, discovered from the WASP surveys, which we combine with radial velocities from OHP/SOPHIE and Euler/CORALIE and photometry from Euler and TRAPPIST. The planets WASP-76b, WASP-82b, and WASP-90b are all inflated, with radii of 1.7-1.8R_Jup_. All three orbit hot stars, of type F5-F7, with orbits of 1.8-3.9d, and all three stars have evolved, post-main-sequence radii (1.7-2.2R_{sun}_). Thus the three planets fit a known trend of hot Jupiters that receive high levels of irradiation, as a result of their being highly inflated. We caution, though, about the presence of a selection effect, in that non-inflated planets around ~2R_{sun}_ post-MS stars can often produce transits too shallow to be detected by the ground-based surveys that have found the majority of transiting hot Jupiters.
- ID:
- ivo://CDS.VizieR/J/AJ/155/184
- Title:
- Irregular planetary satellites colors & shapes
- Short Name:
- J/AJ/155/184
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- It is widely recognized that the irregular satellites of the giant planets were captured from initially heliocentric orbits. However, the mechanism of capture and the source region from which they were captured both remain unknown. We present an optical color survey of 43 irregular satellites of the outer planets conducted using the LRIS camera on the 10 m telescope at the Keck Observatory in Hawaii. The measured colors are compared to other planetary bodies in search for similarities and differences that may reflect upon the origin of the satellites. We find that ultrared matter (with color index B-R>=1.6), while abundant in the Kuiper Belt and Centaur populations, is depleted from the irregular satellites. We also use repeated determinations of the absolute magnitudes to make a statistical estimate of the average shape of the irregular satellites. The data provide no evidence that the satellites and the main-belt asteroids are differently shaped, consistent with collisions as the major agent shaping both.
- ID:
- ivo://CDS.VizieR/J/ApJS/191/96
- Title:
- IR spectra and optical constants of nitrile ices
- Short Name:
- J/ApJS/191/96
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Spectra and optical constants of nitrile ices known or suspected to be in Titan's atmosphere are presented from 2.0 to 333.3um (~5000-30/cm). These results are relevant to the ongoing modeling of Cassini CIRS observations of Titan's winter pole. Ices studied are: HCN, hydrogen cyanide; C2N2, cyanogen; CH3CN, acetonitrile; C2H5CN, propionitrile; and HC3N, cyanoacetylene. For each of these molecules, we also report new cryogenic measurements of the real refractive index, n, determined in both the amorphous and crystalline phases at 670nm. These new values have been incorporated into our optical constant calculations. Spectra were measured and optical constants were calculated for each nitrile at a variety of temperatures, including, but not limited to, 20, 35, 50, 75, 95, and 110K, in both the amorphous phase and the crystalline phase. This laboratory effort used a dedicated FTIR spectrometer to record transmission spectra of thin-film ice samples. Laser interference was used to measure film thickness during condensation onto a transparent cold window attached to the tail section of a closed-cycle helium cryostat. Optical constants, real (n) and imaginary (k) refractive indices, were determined using Kramers-Kronig analysis. Our calculation reproduces the complete spectrum, including all interference effects.
- ID:
- ivo://CDS.VizieR/J/AJ/152/182
- Title:
- iz follow-up photometry of HAT-P-65 and HAT-P-66
- Short Name:
- J/AJ/152/182
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the discovery of the transiting exoplanets HAT-P-65b and HAT-P-66b, with orbital periods of 2.6055 and 2.9721 days, masses of 0.527+/-0.083M_J_ and 0.783+/-0.057M_J_, and inflated radii of 1.89+/-0.13R_J_ and 1.59_-0.10_^+0.16^R_J_, respectively. They orbit moderately bright (V=13.145+/-0.029 and V=12.993+/-0.052) stars of mass 1.212+/-0.050M_{Sun}_ and 1.255_-0.054_^+0.107^M_{Sun}_. The stars are at the main-sequence turnoff. While it is well known that the radii of close-in giant planets are correlated with their equilibrium temperatures, whether or not the radii of planets increase in time as their hosts evolve and become more luminous is an open question. Looking at the broader sample of well-characterized close-in transiting giant planets, we find that there is a statistically significant correlation between planetary radii and the fractional ages of their host stars, with a false-alarm probability of only 0.0041%. We find that the correlation between the radii of planets and the fractional ages of their hosts is fully explained by the known correlation between planetary radii and their present-day equilibrium temperatures; however, if the zero-age main-sequence equilibrium temperature is used in place of the present-day equilibrium temperature, then a correlation with age must also be included to explain the planetary radii. This suggests that, after contracting during the pre-main-sequence, close-in giant planets are reinflated over time due to the increasing level of irradiation received from their host stars. Prior theoretical work indicates that such a dynamic response to irradiation requires a significant fraction of the incident energy to be deposited deep within the planetary interiors.
- ID:
- ivo://CDS.VizieR/J/A+A/608/A71
- Title:
- J,H,K spectroscopy of HD 106906 b
- Short Name:
- J/A+A/608/A71
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Directly imaged planets are ideal candidates for spectroscopic characterization of their atmospheres. The angular separations that are typically close to their host stars, however, reduce the achievable contrast and thus signal-to-noise ratios (S/N). We spectroscopically characterize the atmosphere of HD 106906 b, which is a young low-mass companion near the deuterium burning limit. The wide separation from its host star of 7.1" makes it an ideal candidate for high S/N and high-resolution spectroscopy. We aim to derive new constraints on the spectral type, effective temperature, and luminosity of HD 106906 b and also to provide a high S/N template spectrum for future characterization of extrasolar planets. We obtained 1.1-2.5um integral field spectroscopy with the VLT/SINFONI instrument with a spectral resolution of R~=2000-4000. New estimates of the parameters of HD 106906 b are derived by analyzing spectral features, comparing the extracted spectra to spectral catalogs of other low-mass objects, and fitting with theoretical isochrones.
- ID:
- ivo://CDS.VizieR/J/MNRAS/440/1470
- Title:
- Ji light curves of WTS-2
- Short Name:
- J/MNRAS/440/1470
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of WTS-2 b, an unusually close-in 1.02-d hot Jupiter (M_P_=1.12M_J_, R_P_=1.30R_J_) orbiting a K2V star, which has a possible gravitationally bound M-dwarf companion at 0.6-arcsec separation contributing ~20% of the total flux in the observed J-band light curve. The planet is only 1.5 times the separation from its host star at which it would be destroyed by Roche lobe overflow, and has a predicted remaining lifetime of just ~40Myr, assuming a tidal dissipation quality factor of Q'_*_=10^6^. Q'_*_ is a key factor in determining how frictional processes within a host star affect the orbital evolution of its companion giant planets, but it is currently poorly constrained by observations. We calculate that the orbital decay of WTS-2 b would correspond to a shift in its transit arrival time of T_shift_~17s after 15yr assuming Q'_*_=10^6^. A shift less than this would place a direct observational constraint on the lower limit of Q'_*_ in this system. We also report a correction to the previously published expected T_shift_ for WASP-18 b, finding that T_shift_=356s after 10yr for Q'_*_10^6^, which is much larger than the estimated 28s quoted in WASP-18 b discovery paper. We attempted to constrain Q'_*_ via a study of the entire population of known transiting hot Jupiters, but our results were inconclusive, requiring a more detailed treatment of transit survey sensitivities at long periods. We conclude that the most informative and straightforward constraints on Q'_*_ will be obtained by direct observational measurements of the shift in transit arrival times in individual hot Jupiter systems. We show that this is achievable across the mass spectrum of exoplanet host stars within a decade, and will directly probe the effects of stellar interior structure on tidal dissipation.
- ID:
- ivo://CDS.VizieR/J/A+A/410/343
- Title:
- Jovian mutual events at Lille Observatory
- Short Name:
- J/A+A/410/343
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have observed the four Galilean satellites of Jupiter during their mutual occultations and eclipses from February to April 2003 using a CCD camera attached to the 32.5cm refractor of the observatory of Lille. We have recorded 13 lightcurves of these events. We have performed a first astrometric reduction based on the method developed in Noyelles et al. (2003A&A...401.1159N). This analysis of the results and comparison with theory show that the observations are good; the residuals are about 0.03arcsec.
- ID:
- ivo://CDS.VizieR/J/A+A/604/A17
- Title:
- Jupiter decametric radio emissions over 26 years
- Short Name:
- J/A+A/604/A17
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Jupiter is a complex and at the same time very powerful radio source in the decameter wavelength range. The emission is anisotropic, intrinsically variable at millisecond to hour timescales, and also modulated by various external processes at much longer periods, ranging from ~10h to months or years (including Jovian day and year, solar activity and solar wind variations, and for ground-based observations, terrestrial day and year). As a consequence, long-term observations and their statistical study have proved to be necessary for disentangling and understanding the observed phenomena. We have built a database from the available 26yr of systematic, daily observations conducted at the Nancay Decameter Array and recorded in digital format. This database contains all observed Jovian decametric emissions, classified with respect to the time-frequency morphology, their dominant circular polarization, and maximum frequency. We present the results of the first statistical analysis of this database. We confirm the earlier classification of Jovian decameter emissions in Io-A, -A', -B, -C, -D and non-Io-A, -B, -C types, but we also introduce new emission types (Io-A'' and Io-B') and precise and characterize the non-Io-D type. We determine the contours of all emission types in the CML-{Phi}_Io_ plane (Central Meridian Longitude in Jupiter's System III coordinates versus Io Phase), provide representative examples of their typical time-frequency patterns, and the distribution of emission's maximum frequency as a function of {LAMBDA}_Io_ (Io's Longitude). Finally, we present a statistical analysis of the distributions of the occurrence rate, duration, intensity and polarization for each emission type. non-Io-DAM appears to be related to small-scale, possibly bursty auroral structures.