- ID:
- ivo://CDS.VizieR/J/ApJ/874/L31
- Title:
- Giant planet bulk and atmosphere metallicities
- Short Name:
- J/ApJ/874/L31
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Atmospheric characterization through spectroscopic analysis, an essential tool of modern exoplanet science, can benefit significantly from the context provided by the interior structure models. In particular, the planet's bulk metallicity, Zp, places an upper limit on the potential atmospheric metallicity. Here we construct interior structure models to derive Zp and atmospheric metallicity upper limits for 403 known transiting giant exoplanets. These limits are low enough that they can usefully inform atmosphere models. Additionally, we argue that comparing Zp to the observed atmospheric metallicity gives a useful measure of how well mixed metals are within the planet. This represents a new avenue for learning about planetary interiors. To aid in the future characterization of new planet discoveries we derive analytic prior predictions of atmosphere metallicity as a function of planet mass, and evaluate the effectiveness of our approach on Jupiter and Saturn. We include log-linear fits for approximating the metallicities of planets not in our catalog.
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/622/L7
- Title:
- GJ143 and HD23472 radial velocity curves
- Short Name:
- J/A+A/622/L7
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We aim at the discovery of new planetary systems by exploiting the transit light-curve results from observations made in TESS orbital observatory Sectors 1 and 2 and validating them with precise Doppler measurements obtained from archival HARPS data. Taking advantage of the reported TESS transit events around GJ 143 (TOI 186) and HD 23472 (TOI 174), we modeled their HARPS precise Doppler measurements and derived orbital parameters for these two systems. Results. For the GJ 143 system, TESS has reported only a single transit, and thus its period is unconstrained from photometry. Our radial velocity analysis of GJ 143 reveals the full Keplerian solution of the system, which is consistent with an eccentric planet with a mass almost twice that of Neptune and a period of P_b_=35.59+/-0.01-days. Our estimates of the GJ 143 b planet are fully consistent with the transit timing from TESS. We confirm the two-planet system around HD 23472, which according to our analysis is composed of two Neptune-mass planets in a possible 5:3 mean motion resonance.
- ID:
- ivo://CDS.VizieR/J/A+A/659/A17
- Title:
- GJ 3929 b RVs and activity indicators
- Short Name:
- J/A+A/659/A17
- Date:
- 02 Mar 2022 06:16:21
- Publisher:
- CDS
- Description:
- We report the discovery of GJ 3929 b, a hot Earth-sized planet orbiting the nearby M3.5 V dwarf star, GJ 3929 (G 180-18, TOI-2013). Joint modelling of photometric observations from TESS sectors 24 and 25 together with 73 spectroscopic observations from CARMENES and follow-up transit observations from SAINT-EX, LCOGT, and OSN yields a planet radius of R_b_=1.150+/-0.040R_e_, a mass of M_b_=1.21+/-0.42M_e_, and an orbital period of P_b_=2.6162745+/-0.0000030d. The resulting density of rho_b_=4.4+/-1.6g/cm^3^ is compatible with the Earth's mean density of about 5.5g/cm^3^. Due to the apparent brightness of the host star (J=8.7mag) and its small size, GJ 3929 b is a promising target for atmospheric characterisation with the JWST. Additionally, the radial velocity data show evidence for another planet candidate with P_[c]_=14.303+/-0.035d, which is likely unrelated to the stellar rotation period, P_rot_=122+/-13d, which we determined from archival HATNet and ASAS-SN photometry combined with newly obtained TJO data.
- ID:
- ivo://CDS.VizieR/J/MNRAS/484/3731
- Title:
- GJ 9827 HARPS-N RV data
- Short Name:
- J/MNRAS/484/3731
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Super-Earths belong to a class of planet not found in the Solar system, but which appear common in the Galaxy. Given that some super-Earths are rocky, while others retain substantial atmospheres, their study can provide clues as to the formation of both rocky and gaseous planets, and - in particular - they can help to constrain the role of photoevaporation in sculpting the exoplanet population. GJ 9827 is a system already known to host three super-Earths with orbital periods of 1.2, 3.6, and 6.2d. Here, we use new HARPS-N radial velocity measurements, together with previously published radial velocities, to better constrain the properties of the GJ 9827 planets. Our analysis cannot place a strong constraint on the mass of GJ 9827 c, but does indicate that GJ 9827 b is rocky with a composition that is probably similar to that of the Earth, while GJ 9827 d almost certainly retains a volatile envelope. Therefore, GJ 9827 hosts planets on either side of the radius gap that appears to divide super-Earths into pre-dominantly rocky ones that have radii below ~1.5R_{Earth}_, and ones that still retain a substantial atmosphere and/or volatile components, and have radii above ~2R_{Earth}_. That the less heavily irradiated of the three planets still retains an atmosphere, may indicate that photoevaporation has played a key role in the evolution of the planets in this system.
- ID:
- ivo://CDS.VizieR/J/A+A/648/A20
- Title:
- GJ 740 radial velocities
- Short Name:
- J/A+A/648/A20
- Date:
- 29 Nov 2021 07:26:47
- Publisher:
- CDS
- Description:
- M-dwarfs have proven to be ideal targets for planetary radial velocity (RV) searches due to their higher planet-star mass contrast, which favors the detection of low-mass planets. The abundance of super-Earth and Earth-like planets detected around this type of stars encourages us to continue this search on hosts without reported planetary companions. The HADES and CARMENES programs aim to carry out extensive searches of exoplanetary systems around M-type stars in the northern hemisphere, allowing us to address statistically the properties of the planets orbiting these objects. In this work, we performed a spectroscopic and photometric study on one of the program stars (GJ 740), which exhibits a short-period RV signal compatible with a planetary companion. We carried out a spectroscopic analysis based on 129 HARPS-N spectra taken over a time-span of 6 yr combined with 57 HARPS spectra taken over 4yr, and 32 CARMENES spectra taken during more than 1 yr, resulting in a dataset with a time coverage of 10yr. We also relied on 459 measurements from the public ASAS survey with a time-coverage of 8yr along with 5yr of photometric magnitudes from the EXORAP project taken in the V, B, R and I filters to carry out a photometric study. Both analyses were made using Markov Chain Monte Carlo (MCMC) simulations and Gaussian Process regression to model the activity of the star. We present the discovery of a short-period super-Earth with an orbital period of 2.37756^+0.00013^_-0.00011_d and a minimum mass of 2.96^+0.50^_-0.48_Me. We update the previously reported characterization of the magnetic cycle and rotation period of the star, obtaining values of Prot=35.563+/-0.071d and Pcycle=2800+/-150d. The RV time-series exhibits a possibly periodic long-term signal which might be related to a Saturn-mass planet of ~100Me.
- ID:
- ivo://CDS.VizieR/J/other/Sci/365.1441
- Title:
- GJ 3512 radial velocity and light curves
- Short Name:
- J/other/Sci/365.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.
- ID:
- ivo://CDS.VizieR/J/A+A/622/A153
- Title:
- GJ 4276 radial velocity curve
- Short Name:
- J/A+A/622/A153
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the detection of a Neptune-mass exoplanet around the M4.0 dwarf GJ 4276 (G 232-070) based on radial velocity (RV) observations obtained with the CARMENES spectrograph. The RV variations of GJ 4276 are best explained by the presence of a planetary companion with a minimum mass of m_b_sini~16M_{sun}_ on a P_b_=13.35-day orbit. The analysis of the activity indicators and spectral diagnostics exclude stellar induced RV perturbations and prove the planetary interpretation of the RV signal. We show that a circular single-planet solution can be excluded by means of a likelihood ratio test. Instead, we find that the RV variations can either be explained by an eccentric orbit or interpreted as a pair of planets on circular orbits near a period ratio of 2:1. Although the eccentric single-planet solution is slightly preferred, our statistical analysis indicates that none of these two scenarios can be rejected with high confidence using the RV time series obtained so far. Based on the eccentric interpretation, we find that GJ 4276 b is the most eccentric (e_b_=0.37) exoplanet around an M dwarf with such a short orbital period known today.
- ID:
- ivo://CDS.VizieR/J/A+A/649/L12
- Title:
- GJ 1151 radial velocity curve
- Short Name:
- J/A+A/649/L12
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- The interaction between Earth-like exoplanets and the magnetic field of low-mass host stars are considered to produce weak emission signals at radio frequencies. A study using LOFAR data announced the detection of radio emission from the mid M-type dwarf GJ 1151 that could potentially arise from a close-in terrestrial planet. Recently, the presence of a 2.5-M_{earth}_ planet orbiting GJ 1151 with a 2-day period has been claimed using 69 radial velocities (RVs) from the HARPS-N and HPF instruments. We have obtained 70 new high-precision RV measurements in the framework of the CARMENES M-dwarf survey and use these data to confirm the presence of the claimed planet and to place limits on possible planetary companions in the GJ 1151 system. We analysed the periodicities present in the combined RV data sets from all three instruments and calculated the detection limits for potential planets in short-period orbits. We cannot confirm the recently announced candidate planet and conclude that the 2-day signal in the HARPS-N and HPF data sets is most probably produced by a long-term RV variability, possibly arising from an outer planetary companion that has yet to be constrained. We calculate a 99.9% significance detection limit of 1.50m/s in the RV semi-amplitude, which places upper limits of 0.7M_{earth}_ and 1.2M_{earth}_ on the minimum masses of potential exoplanets with orbital periods of 1 and 5 days, respectively.
- ID:
- ivo://CDS.VizieR/J/A+A/642/A236
- Title:
- GJ 3473 (TOI-488) radial velocity curve
- Short Name:
- J/A+A/642/A236
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the confirmation and characterisation of GJ 3473 b (G 50-16, TOI-488.01), a hot Earth-sized planet orbiting an M4 dwarf star, whose transiting signal (P=1.1980035+/-0.0000018d) was first detected by the Transiting Exoplanet Survey Satellite (TESS). Through a joint modelling of follow-up radial velocity observations with CARMENES, IRD, and HARPS together with extensive ground-based photometric follow-up observations with LCOGT, MuSCAT, and MuSCAT2, we determined a precise planetary mass, M_b_=1.86+/-0.30M_{sun}_, and radius, R_b_=1.264+/-0.050R_{sun}_. Additionally, we report the discovery of a second, temperate, non-transiting planet in the system, GJ 3473 c, which has a minimum mass, M_c_sini=7.41+/-0.91M_{sun}_ and orbital period, P_c_=15.509+/-0.033d. The inner planet of the system, GJ 3473 b, is one of the hottest transiting Earth- sized planets known thus far, accompanied by a dynamical mass measurement, which makes it a particularly attractive target for thermal emission spectroscopy.
- ID:
- ivo://CDS.VizieR/J/A+A/618/A103
- Title:
- Gl617A and Gl96 radial velocity curves
- Short Name:
- J/A+A/618/A103
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the detection of two exoplanets and a further tentative candidate around the M-dwarf stars Gl96 and Gl617A, based on radial velocity measurements obtained with the SOPHIE spectrograph at the Observatoire de Haute-Provence. Both stars were observed in the context of the SOPHIE exoplanet consortium's dedicated M-dwarf subprogramme, which aims to detect exoplanets around nearby M-dwarf stars through a systematic survey. For Gl96 we present the discovery of a new exoplanet at 73.9d with a minimum mass of 19.66 earth masses. Gl96b has an eccentricity of 0.44, placing it among the most eccentric planets orbiting M stars. For Gl617A we independently confirm a recently reported exoplanet at 86.7d with a minimum mass of 31.29 earth masses. Both Gl96 b and Gl617Ab are potentially within the habitable zone, though the high eccentricity of Gl96 b may take it too close to the star at periapsis.
