The CARMENES search for exoplanets around M dwarfs. Stellar atmospheric parameters of target stars with SteParSyn

Marfil, Emilio; Tabernero, Hugo M.; Montes, David; Caballero, Jose A.; Lazaro, Francisco J.; Hernandez, Jonay I. Gonzalez; Nagel, Evangelos; Passegger, Vera M.; Schweitzer, Andreas; Ribas, Ignasi; Reiners, Ansgar; Quirrenbach, Andreas; Amado, Pedro J.; Cifuentes, Carlos; Cortes-Contreras, Miriam; Dreizler, Stefan; Duque-Arribas, Christian; Galadi-Enriquez, David; Henning, Thomas; Jeffers, Sandra V.; Kaminski, Adrian; Kurster, Martin; Lafarga, Marina; Lopez-Gallifa, Alvaro; Morales, Juan Carlos; Shan, Yutong; Zechmeister, Mathias

doi:10.48550/arxiv.2110.07329

Cited by 5 publications

(11 citation statements)

References 109 publications

(195 reference statements)

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“…We obtained the photospheric parameters T eff , log g and [Fe/H] of TOI-1759 following Passegger et al (2019) by fitting PHOENIX synthetic spectra to the combined (co-added) CARMENES VIS spectrum described in Section 2.2.1, which has a signal-to-noise ratio in the VIS channel of ≈ 200. We used v sin i = 2 km s −1 , which was measured by Marfil et al (2021) as an upper limit. We derived its luminosity following Cifuentes et al (2020) by using the latest parallactic distance from Gaia EDR3 (Gaia Collaboration et al 2021), and by integrating Gaia, 2MASS (Skrutskie et al 2006) and AllWISE (Cutri et al 2014) photometry covering the full spectral energy distribution with the Virtual Observatory Spectral energy distribution Analyser (Bayo et al 2008).…”

Section: Stellar Parametersmentioning

confidence: 99%

Section: Stellar Parametersmentioning

confidence: 99%

“…TOI-1759's pseudo equivalent width of the Hα line as defined by Schöfer et al (2019) is pEW (Hα) < −0.3 Å (Marfil et al 2021), classifying it as an Hα inactive star. Furthermore, Marfil et al (2021) assign it to the Galactic thin disc population, which has a maximum age of about 8 Gyr (Fuhrmann 1998). Using these two properties as age indicators, we conclude that its age is between 1 Gyr (the typical minimum age for field stars) and 8 Gyr without being able to be more precise.…”

Section: Stellar Parametersmentioning

confidence: 99%

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A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

Espinoza,

Pallé,

Kemmer

et al. 2022

Preprint

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We report the discovery and characterization of TOI-1759 b, a temperate (400 K) sub-Neptune-sized exoplanet orbiting the M dwarf TOI-1759 (TIC 408636441). TOI-1759 b was observed by TESS to transit on sectors 16, 17 and 24, with only one transit observed per sector, creating an ambiguity on the orbital period of the planet candidate. Ground-based photometric observations, combined with radial-velocity measurements obtained with the CARMENES spectrograph, confirm an actual period of 18.85019±0.00014 d. A joint analysis of all available photometry and radial velocities reveal a radius of 3.17 ± 0.10 R ⊕ and a mass of 10.8 ± 1.5 M ⊕ . Combining this with the stellar properties derived for TOI-1759 (R = 0.597 ± 0.015 R ; M = 0.606 ± 0.020 M ; T eff = 4065 ± 51 K), we compute a transmission spectroscopic metric (TSM) value of over 80 for the planet, making it a good target for transmission spectroscopy studies. TOI-1759 b is among the top five temperate, small exoplanets (T eq < 500 K, R p < 4 R ⊕ ) with the highest TSM discovered to date. Two additional signals with periods of 80 d and > 200 d seem to be present in our radial velocities. While our data suggest both could arise from stellar activity, the later signal's source and periodicity are hard to pinpoint given the ∼ 200 d baseline of our radial-velocity campaign with CARMENES. Longer baseline radial-velocity campaigns should be performed in order to unveil the true nature of this long period signal.

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Section: Stellar Parametersmentioning

confidence: 99%

Section: Stellar Parametersmentioning

confidence: 99%

Section: Stellar Parametersmentioning

confidence: 99%

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A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

Espinoza,

Pallé,

Kemmer

et al. 2022

Preprint

Self Cite

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“…Others attempt to fit spectral energy distributions (SEDs) on low to mid-resolution spectra (Mann et al 2013). More recently, advances in spectral modelling and the advent of new high-resolution spectrographs in the near-infrared (NIR) domain allowed some authors to perform direct fits of synthetic spectra on high-resolution ★ E-mail: paul.cristofari@irap.omp.eu (IRAP) spectroscopic observations (Passegger et al 2018;Schweitzer et al 2019;Marfil et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Estimating the atmospheric properties of 44 M dwarfs from SPIRou spectra

Cristofari

Donati

Masseron

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We describe advances on a method designed to derive accurate parameters of M dwarfs. Our analysis consists in comparing high-resolution infrared spectra acquired with the near-infrared spectro-polarimeter SPIRou to synthetic spectra computed from MARCS model atmospheres, in order to derive the effective temperature (Teff), surface gravity (log g), metallicity ($\rm {[M/H]}$) and alpha-enhancement ($\rm {[\alpha /Fe]}$) of 44 M dwarfs monitored within the SPIRou Legacy Survey (SLS). Relying on 12 of these stars, we calibrated our method by refining our selection of well modelled stellar lines, and adjusted the line list parameters to improve the fit when necessary. Our retrieved Teff, log g and $\rm {[M/H]}$ are in good agreement with literature values, with dispersions of the order of 50 K in Teff and 0.1 dex in log g and $\rm {[M/H]}$. We report that fitting $\rm {[\alpha /Fe]}$ has an impact on the derivation of the other stellar parameters, motivating us to extend our fitting procedure to this additional parameter. We find that our retrieved $\rm {[\alpha /Fe]}$ are compatible with those expected from empirical relations derived in other studies.

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“…It is thus reasonable to suspect that the giant planets in our sample have formed in particularly metal-rich environments that are not represented by the metallicity distribution of the synthetic systems. The reported values for the giant planet hosts mentioned above are 0.05 ± 0.2 dex or −0.11 ± 0.10 for Gl 876 b (Correia et al 2010;Marfil et al 2021), 0.36 ± 0.2 for Gl 317 (Anglada-Escudé et al 2012), 0.13 ± 0.16 or −0.17 ± 0.10 for GJ 1148 (Passegger et al 2018;Marfil et al 2021) and −0.07 ± 0.16 or −0.12 ± 0.16 for GJ 3512 (Morales et al 2019;Marfil et al 2021), leaving only Gl 317 with an enhanced metallicity. Although the uncertainties are large, the other targets are consistent with solar metallicity.…”

Section: Excess Of Giant Planets Around Late M Dwarfsmentioning

confidence: 91%

RV-detected planets around M dwarfs: Challenges for core accretion models

Schlecker,

Burn,

Sabotta

et al. 2022

Preprint

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Context. Planet formation is sensitive to the conditions in protoplanetary disks, for which scaling laws as a function of stellar mass are known. Aims. We aim to test whether the observed population of planets around low-mass stars can be explained by these trends, or if separate formation channels are needed. Methods. We address this question by confronting a state-of-the-art planet population synthesis model with a sample of planets around M dwarfs observed by the HARPS and CARMENES radial velocity (RV) surveys. To account for detection biases, we performed injection and retrieval experiments on the actual RV data to produce synthetic observations of planets that we simulated following the core accretion paradigm. Results. These simulations robustly yield the previously reported high occurrence of rocky planets around M dwarfs and generally agree with their planetary mass function. In contrast, our simulations cannot reproduce a population of giant planets around stars less massive than 0.5 solar masses. This potentially indicates an alternative formation channel for giant planets around the least massive stars that cannot be explained with current core accretion theories. We further find a stellar mass dependency in the detection rate of short-period planets. A lack of close-in planets around the earlier-type stars (M 0.4 M ) in our sample remains unexplained by our model and indicates dissimilar planet migration barriers in disks of different spectral subtypes. Conclusions. Both discrepancies can be attributed to gaps in our understanding of planet migration in nascent M dwarf systems. They underline the different conditions around young stars of different spectral subtypes, and the importance of taking these differences into account when studying planet formation.

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The CARMENES search for exoplanets around M dwarfs. Stellar atmospheric parameters of target stars with SteParSyn

Cited by 5 publications

References 109 publications

A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

A transiting, temperate mini-Neptune orbiting the M dwarf TOI-1759 unveiled by TESS

Estimating the atmospheric properties of 44 M dwarfs from SPIRou spectra

RV-detected planets around M dwarfs: Challenges for core accretion models

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