- ID:
- ivo://CDS.VizieR/J/A+A/613/A41
- Title:
- 5 exoplanet light and RV curves
- Short Name:
- J/A+A/613/A41
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The measurement of the orbital obliquity of hot Jupiters, with different physical characteristics, can provide clues to the mechanisms of migration and orbital evolution of this particular class of giant exoplanets. We aim to derive the degree of alignment between planetary orbit and stellar spin angular momentum vectors and look for possible links with other orbital and fundamental physical parameters of the star-planet system. Here we focus on the characterisation of five transiting planetary systems (HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60) and the determination of their sky-projected planet orbital obliquity through the measurement of the Rossiter-McLaughlin effect. We used HARPS-N high-precision radial velocity measurements, gathered during transit events, to measure the Rossiter-McLaughlin effect in the target systems and determine the sky-projected angle between the planetary orbital plane and the stellar equator. The characterisation of stellar atmospheric parameters was performed exploiting the HARPS-N spectra, using line equivalent width ratios, and spectral synthesis methods. Photometric parameters of the five transiting exoplanets were re-analysed through 17 new light curves, obtained with an array of medium-class telescopes, and other light curves from the literature. Survey-time-series photometric data were analysed for determining the rotation periods of the five stars and their spin inclination. From the analysis of the Rossiter-McLaughlin effect we derived a sky-projected obliquity of {lambda}=21.2+/-8.7{deg}, {lambda=-54^+41^_-13_{deg}, {lambda=-2.1+/-3.0{deg}, lambda=0+/-11{deg} and lambda=-129+/-17{deg} for HAT-P-3 b, HAT-P-12 b, HAT-P-22 b, WASP-39 b and WASP-60 b, respectively. The latter value indicates that WASP-60 b is moving on a retrograde orbit. These values represent the first measurements of {lambda} for the five exoplanetary systems under study. The stellar activity of HAT-P-22 indicates a rotation period of 28.7+/-0.4-days, which allowed us to estimate the true misalignment angle of HAT-P-22 b, {psi}=24+/-18{deg}. The revision of the physical parameters of the five exoplanetary systems returned values fully compatible with those existing in the literature, with the exception of the WASP-60 system, for which, based on higher quality spectroscopic and photometric data, we found a more massive and younger star, and a larger and hotter planet.
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Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/411/L46
- Title:
- Exoplanet magnetic fields
- Short Name:
- J/MNRAS/411/L46
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- An asymmetry between the ingress and egress times was observed in the near-UV light curve of the transit planet WASP-12b. Such asymmetry led us to suggest that the early ingress in the UV light curve of WASP-12b, compared to the optical observations, is caused by a shock around the planet, and that shocks should be a common feature in transiting systems. Here, we classify all the transiting systems known to date according to their potential for producing shocks that could cause observable light curve asymmetries.
- ID:
- ivo://CDS.VizieR/J/ApJ/733/68
- Title:
- Exoplanet masses derived from RVs
- Short Name:
- J/ApJ/733/68
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Exoplanet searches using radial velocity (RV) and microlensing (ML) produce samples of "projected" mass and orbital radius, respectively. We present a new method for estimating the probability density distribution (density) of the unprojected quantity from such samples. For a sample of n data values, the method involves solving n simultaneous linear equations to determine the weights of delta functions for the raw, unsmoothed density of the unprojected quantity that cause the associated cumulative distribution function (CDF) of the projected quantity to exactly reproduce the empirical CDF of the sample at the locations of the n data values. We smooth the raw density using nonparametric kernel density estimation with a normal kernel of bandwidth {sigma}. We calibrate the dependence of {sigma} on n by Monte Carlo experiments performed on samples drawn from a theoretical density, in which the integrated square error is minimized. We scale this calibration to the ranges of real RV samples using the Normal Reference Rule. The resolution and amplitude accuracy of the estimated density improve with n. For typical RV and ML samples, we expect the fractional noise at the PDF peak to be approximately 80n^-log2^. For illustrations, we apply the new method to 67 RV values given a similar treatment by Jorissen et al. (2001A&A...379..992J), and to the 308 RV values listed at exoplanets.org on 2010 October 20.
5864. Exoplanet Orbit Database
- ID:
- ivo://CDS.VizieR/J/PASP/123/412
- Title:
- Exoplanet Orbit Database
- Short Name:
- J/PASP/123/412
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a database of well determined orbital parameters of exoplanets, and their host stars' properties. This database comprises spectroscopic orbital elements measured for 427 planets orbiting 363 stars from radial velocity and transit measurements as reported in the literature. We have also compiled fundamental transit parameters, stellar parameters, and the method used for the planets discovery. This Exoplanet Orbit Database includes all planets with robust, well measured orbital parameters reported in peer-reviewed articles. The Database is available in a searcheable, filterable, and sortable form on the Web at http://exoplanets.org through the Exoplanets Data Explorer Table, and the data can be plotted and explored through the Exoplanet Data Explorer Plotter. We use the Data Explorer to generate publication-ready plots giving three examples of the signatures of exoplanet migration and dynamical evolution: We illustrate the character of the apparent correlation between mass and period in exoplanet orbits, the different selection biases between radial velocity and transit surveys, and that the multiplanet systems show a distinct semi-major axis distribution from apparently singleton systems.
5865. Exoplanet Orbit Database
- ID:
- ivo://nasa.heasarc/exoplanodb
- Title:
- Exoplanet Orbit Database
- Short Name:
- EXOPLANODB
- Date:
- 27 Sep 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Exoplanet Orbit Database is a database of well-determined orbital parameters of exoplanets, and their host stars' properties. This database comprises spectroscopic orbital elements measured for planets orbiting their host stars from radial velocity and transit measurements as reported in the literature. The authors have also compiled fundamental transit parameters, stellar parameters, and the method used for the planets discovery. This Exoplanet Orbit Database includes all planets with robust, well measured orbital parameters reported in peer-reviewed articles. In addition to this HEASARC representation, the database is available in a searchable, filterable, and sortable form online through the Exoplanets Data Explorer table at <a href="http://exoplanets.org">http://exoplanets.org</a>, and the data can be plotted and explored through the Exoplanet Data Explorer plotter which is available at that web site. In their paper, the authors use the Data Explorer to generate publication-ready plots, giving three examples of the signatures of exoplanet migration and dynamical evolution: They illustrate the character of the apparent correlation between mass and period in exoplanet orbits, the different selection biases between radial velocity and transit surveys, and that the multi-planet systems show a distinct semi-major-axis distribution from apparently singleton systems. This table was first created by the HEASARC in August 2012 based on a machine-readable version of the Exoplanet Orbit Database which was obtained from the authors' web site (<a href="http://exoplanets.org">http://exoplanets.org</a>), file exoplanets.csv. It is updated usually within a day of whenever the source file is updated. This is a service provided by NASA HEASARC .
- ID:
- ivo://CDS.VizieR/J/AJ/159/211
- Title:
- Exoplanet parameters from Kepler and K2
- Short Name:
- J/AJ/159/211
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present calculations of the occurrence rate of small close-in planets around low-mass dwarf stars using the known planet populations from the Kepler and K2 missions. Applying completeness corrections clearly reveals the radius valley in the maximum a posteriori occurrence rates as a function of orbital separation and planet radius. We measure the slope of the valley to be r_p,valley_{prop}F^-0.060{+/-}0.025^, which bears the opposite sign from that measured around Sun-like stars, thus suggesting that thermally driven atmospheric mass loss may not dominate the evolution of planets in the low stellar mass regime or that we are witnessing the emergence of a separate channel of planet formation. The latter notion is supported by the relative occurrence of rocky to non-rocky planets increasing from 0.5{+/-}0.1 around mid-K dwarfs to 8.5{+/-}4.6 around mid-M dwarfs. Furthermore, the center of the radius valley at 1.54{+/-}0.16R{earth} is shown to shift to smaller sizes with decreasing stellar mass, in agreement with physical models of photoevaporation, core-powered mass loss, and gas-poor formation. Although current measurements are insufficient to robustly identify the dominant formation pathway of the radius valley, such inferences may be obtained by the Transiting Exoplanet Survey Satellite with O(85000) mid-to-late M dwarfs observed with 2minutes cadence. The measurements presented herein also precisely designate the subset of planetary orbital periods and radii that should be targeted in radial velocity surveys to resolve the rocky to non-rocky transition around low-mass stars.
5867. Exoplanet radio emission
- ID:
- ivo://CDS.VizieR/J/ApJ/612/511
- Title:
- Exoplanet radio emission
- Short Name:
- J/ApJ/612/511
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We predict the radio flux densities of the extrasolar planets in the current census, making use of an empirical relation - the radiometric Bode's law - determined from the five "magnetic" planets in the solar system (the Earth and the four gas giants). Radio emission from these planets results from solar wind-powered electron currents depositing energy in the magnetic polar regions. We find that most of the known extrasolar planets should emit in the frequency range 10-1000 MHz and, under favorable circumstances, have typical flux densities as large as 1mJy. We also describe an initial, systematic effort to search for radio emission in low radio frequency images acquired with the Very Large Array (VLA). The limits set by the VLA images (~300mJy) are consistent with, but do not provide strong constraints on, the predictions of the model.
- ID:
- ivo://CDS.VizieR/J/AJ/161/36
- Title:
- 117 exoplanets in habitable zone with Kepler DR25
- Short Name:
- J/AJ/161/36
- Date:
- 09 Mar 2022 22:00:00
- Publisher:
- CDS
- Description:
- We present the occurrence rates for rocky planets in the habitable zones (HZs) of main-sequence dwarf stars based on the Kepler DR25 planet candidate catalog and Gaia-based stellar properties. We provide the first analysis in terms of star-dependent instellation flux, which allows us to track HZ planets. We define {eta}{Earth} as the HZ occurrence of planets with radii between 0.5 and 1.5 R{Earth} orbiting stars with effective temperatures between 4800 and 6300K. We find that {eta}{Earth} for the conservative HZ is between 0.37_-0.21_^+0.48^ (errors reflect 68% credible intervals) and 0.60_-0.36_^+0.90^ planets per star, while the optimistic HZ occurrence is between 0.58_-0.33_^+0.73^ and 0.88_-0.51_^+1.28^ planets per star. These bounds reflect two extreme assumptions about the extrapolation of completeness beyond orbital periods where DR25 completeness data are available. The large uncertainties are due to the small number of detected small HZ planets. We find similar occurrence rates between using Poisson likelihood Bayesian analysis and using Approximate Bayesian Computation. Our results are corrected for catalog completeness and reliability. Both completeness and the planet occurrence rate are dependent on stellar effective temperature. We also present occurrence rates for various stellar populations and planet size ranges. We estimate with 95% confidence that, on average, the nearest HZ planet around G and K dwarfs is ~6pc away and there are ~4 HZ rocky planets around G and K dwarfs within 10pc of the Sun.
- ID:
- ivo://CDS.VizieR/J/MNRAS/495/4924
- Title:
- Exoplanets in Southern open clusters
- Short Name:
- J/MNRAS/495/4924
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The scope of the project 'A PSF-based Approach to TESS High Quality data Of Stellar clusters' (PATHOS) is the extraction and analysis of high-precision light curves of stars in stellar clusters and young associations for the identification of candidate exoplanets and variable stars. The cutting-edge tools used in this project allow us to measure the real flux of stars in dense fields, minimizing the effects due to contamination by neighbour sources. We extracted about 200000 light curves of stars in 645 open clusters located in the Southern ecliptic hemisphere and observed by TESS during the first year of its mission. We searched for transiting signals and we found 33 objects of interest, 11 of which are strong candidate exoplanets. Because of the limited SNR, we did not find any Earth or super-Earth. We identified two Neptune-size planets orbiting stars with R*<1.5R_{sun}_, implying a frequency f*=1.3+/-0.95 per cent consistent with the frequency around field stars. The seven Jupiter candidates around stars with R*<1.5R_{sun}_ imply a frequency f*=0.19+/-0.07 per cent, which is smaller than in the field. more complete estimate of the survey completeness and false positive rate is needed to confirm these results. Light curves used in this work will be made available to the astronomical community on the Mikulski Archive for Space Telescope under the project PATHOS.
- ID:
- ivo://CDS.VizieR/J/A+A/615/A39
- Title:
- Exoplanets interior structures & Love numbers
- Short Name:
- J/A+A/615/A39
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Space missions such as CoRoT and Kepler have made the transit method the most successful technique in observing extrasolar planets. However, although the mean density of a planet can be derived from its measured mass and radius, no details about its interior structure, such as the density profile, can be inferred so far. If determined precisely enough, the shape of the transiting light curve might, in principle, reveal the shape of the planet, and in particular, its deviation from spherical symmetry. These deformations are caused, for instance, by the tidal interactions of the planet with the host star and by other planets that might orbit in the planetary system. The deformations depend on the interior structure of the planet and its composition and can be parameterized as Love numbers k_n_. This means that the diversity of possible interior models for extrasolar planets might be confined by measuring this quantity. We present results of a wide-ranging parameter study in planet mass, surface temperature, and layer mass fractions on such models for super-Earths and their corresponding Love numbers. Based on these data, we find that k_2_ is most useful in assessing the ratio of rocky material to iron and in ruling out certain compositional configurations for measured mass and radius values, such as a prominent core consisting of rocky material. Furthermore, we apply the procedure to exoplanets K2-3b and c and predict that K2-3c probably has a thick outer water layer.