- ID:
- ivo://CDS.VizieR/J/ApJ/801/143
- Title:
- Extrasolar Kuiper belts from Herschel
- Short Name:
- J/ApJ/801/143
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The study of the planet-debris disk connection can shed light on the formation and evolution of planetary systems and may help "predict" the presence of planets around stars with certain disk characteristics. In preliminary analyses of subsamples of the Herschel DEBRIS and DUNES surveys, Wyatt et al. (2012MNRAS.424.1206W) and Marshall et al. (2014A&A...565A..15M) identified a tentative correlation between debris and the presence of low-mass planets. Here we use the cleanest possible sample out of these Herschel surveys to assess the presence of such a correlation, discarding stars without known ages, with ages <1Gyr, and with binary companions <100AU to rule out possible correlations due to effects other than planet presence. In our resulting subsample of 204 FGK stars, we do not find evidence that debris disks are more common or more dusty around stars harboring high-mass or low-mass planets compared to a control sample without identified planets.
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJ/795/166
- Title:
- Extrasolar planet HD 189733b whitelight curve
- Short Name:
- J/ApJ/795/166
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Spectroscopic observations of exoplanets are crucial to infer the composition and properties of their atmospheres. HD 189733b is one of the most extensively studied exoplanets and is a cornerstone for hot Jupiter models. In this paper, we report the dayside emission spectrum of HD 189733b in the wavelength range 1.1-1.7 {mu}m obtained with the Hubble Space Telescope Wide Field Camera 3 (WFC3) in spatial scan mode. The quality of the data is such that even a straightforward analysis yields a high-precision Poisson noise-limited spectrum: the median 1{sigma} uncertainty is 57 ppm per 0.02 {mu}m bin. We also build a white-light curve correcting for systematic effects and derive an absolute eclipse depth of 96+/-39 ppm. The resulting spectrum shows marginal evidence for water vapor absorption, but can also be well explained by a blackbody spectrum. However, the combination of these WFC3 data with previous Spitzer photometric observations is best explained by a dayside atmosphere of HD 189733b with no thermal inversion and a nearly solar or subsolar H_2_O abundance in a cloud-free atmosphere. Alternatively, this apparent subsolar abundance may be the result of clouds or hazes that future studies need to investigate.
- ID:
- ivo://CDS.VizieR/J/A+A/538/A113
- Title:
- Extrasolar planets. Radial velocities of eight stars
- Short Name:
- J/A+A/538/A113
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The mass domain where massive extrasolar planets and brown dwarfs lie is still poorly understood. Indeed, not even a clear dividing line between massive planets and brown dwarfs has been established yet. This is partly because these objects are very scarce in close orbits around solar-type stars, the so-called brown dwarf desert. Owing to this, it has proven difficult to set up a strong observational base with which to compare models and theories of formation and evolution. We search to increase the current sample of massive sub-stellar objects with precise orbital parameters, and to constrain the true mass of detected sub-stellar candidates
- ID:
- ivo://CDS.VizieR/J/A+A/545/A55
- Title:
- Extrasolar planets. Radial velocities of 5 stars
- Short Name:
- J/A+A/545/A55
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present radial-velocity measurements obtained in one of a number of programs underway to search for extrasolar planets with the spectrograph SOPHIE at the 1.93-m telescope of the Haute-Provence Observatory. Targets were selected from catalogs observed with ELODIE, which had been mounted previously at the telescope, in order to detect long-period planets with an extended database close to 15 years.
- ID:
- ivo://CDS.VizieR/J/ApJ/666/475
- Title:
- Extrasolar planet taxonomy
- Short Name:
- J/ApJ/666/475
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper we present the guidelines for an extrasolar planet taxonomy. The discovery of an increasing number of extrasolar planets showing a vast variety of planetary parameters, such as Keplerian orbital elements, and environmental parameters, such as stellar masses, spectral types, and metallicity, prompts the development of a planetary taxonomy. In this work, via principal component analysis followed by hierarchical clustering analysis, we report the definition of five robust groups of planets. We also discuss the physical relevance of such analysis, which may provide a valid basis for disentangling the role of the several physical parameters involved in the processes of planet formation and subsequent evolution. For instance, we were able to divide the hot Jupiters into two main groups on the basis of their stellar masses and metallicities. Moreover, for some groups, we find strong correlations among metallicity, semimajor axis, and eccentricity. The implications of these findings are discussed.
- ID:
- ivo://CDS.VizieR/J/A+A/311/710
- Title:
- Faint Jovian satellites ephemerides
- Short Name:
- J/A+A/311/710
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The observations of the faint satellites of Jupiter J6, J7, J8 and J9 have been collected. Numerical integrations have been performed and fitted to ancient and modern observations. Ephemerides of the equatorial jovicentric rectangular coordinates of the satellites are presented under the form of Poisson series, covering 150 years from 1900. Numerical tools (tables and softwares) are provided to the users for a practical reconstruction of the ephemerides.
- ID:
- ivo://CDS.VizieR/J/PASP/128/G4502
- Title:
- False alarms in Kepler planet candidate cat.
- Short Name:
- J/PASP/128/G4502
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a new automated method to identify instrumental features masquerading as small, long-period planets in the Kepler planet candidate catalog. These systematics, mistakenly identified as planet transits, can have a strong impact on occurrence rate calculations because they cluster in a region of parameter space where Kepler's sensitivity to planets is poor. We compare individual transit-like events to a variety of models of real transits and systematic events and use a Bayesian information criterion to evaluate the likelihood that each event is real. We describe our technique and test its performance on simulated data. Results from this technique are incorporated in the Kepler Q1-Q17 DR24 planet candidate catalog of Coughlin et al. (2016, Cat. J/ApJS/224/12)
- ID:
- ivo://CDS.VizieR/J/ApJ/738/170
- Title:
- False positive Kepler planet candidates
- Short Name:
- J/ApJ/738/170
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a framework to conservatively estimate the probability that any particular planet-like transit signal observed by the Kepler mission is in fact a planet, prior to any ground-based follow-up efforts. We use Monte Carlo methods based on stellar population synthesis and Galactic structure models, and report false positive probabilities (FPPs) for every Kepler Object of Interest, assuming a 20% intrinsic occurrence rate of close-in planets in the radius range 0.5R_{earth}_<R_p_<20R_{earth}_. Nearly 90% of the 1235 candidates have FPP<10%, and over half have FPP<5%. This probability varies with the magnitude and Galactic latitude of the target star, and with the depth of the transit signal - deeper signals generally have higher FPPs than shallower signals. We establish that a single deep high-resolution image will be an effective follow-up tool for the shallowest (Earth-sized) transits, providing the quickest route toward probabilistically validating the smallest candidates by potentially decreasing the FPP of an Earth-sized transit around a faint star from >10% to <1%. Since Kepler has detected many more planetary signals than can be positively confirmed with ground-based follow-up efforts in the near term, these calculations will be crucial to using the ensemble of Kepler data to determine population characteristics of planetary systems. We also describe how our analysis complements the Kepler team's more detailed BLENDER false positive analysis for planet validation.
- ID:
- ivo://CDS.VizieR/J/ApJ/822/86
- Title:
- False positive probabilities for Q1-Q17 DR24 KOIs
- Short Name:
- J/ApJ/822/86
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present astrophysical false positive probability calculations for every Kepler Object of Interest (KOI) --the first large-scale demonstration of a fully automated transiting planet validation procedure. Out of 7056 KOIs, we determine that 1935 have probabilities vespa (Morton T.D. 2015ascl.soft03011M), a publicly available Python package that is able to be easily applied to any transiting exoplanet candidate.
- ID:
- ivo://CDS.VizieR/J/A+A/415/1153
- Title:
- [Fe/H] for 98 extra-solar planet-host stars
- Short Name:
- J/A+A/415/1153
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present stellar parameters and metallicities, obtained from a detailed spectroscopic analysis, for a large sample of 98 stars known to be orbited by planetary mass companions (almost all known targets), as well as for a volume-limited sample of 41 stars not known to host any planet. For most of the stars the stellar parameters are revised versions of the ones presented in our previous work. However, we also present parameters for 18 stars with planets not previously published, and a compilation of stellar parameters for the remaining 4 planet-hosts for which we could not obtain a spectrum. A comparison of our stellar parameters with values of Teff, logg, and [Fe/H] available in the literature shows a remarkable agreement. In particular, our spectroscopic logg values are now very close to trigonometric logg estimates based on Hipparcos parallaxes. The derived [Fe/H] values are then used to confirm the previously known result that planets are more prevalent around metal-rich stars.