Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics★

Montes, D.; González-Peinado, R.; Tabernero, H. M.; Caballero, J. A.; Marfil, E.; Alonso-Floriano, F. J.; Cortés-Contreras, M.; Hernández, J. I. González; Klutsch, A.; Moreno-Jodar, Carlos

doi:10.1093/mnras/sty1295

Cited by 73 publications

(80 citation statements)

References 211 publications

(246 reference statements)

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“…Finally, the colour-colour diagrams with near-infrared 2MASS and AllWISE data (specially W3 and W4) are very sensitive to T eff variations at the L spectral types, but quite insensitive in the late-K and M dwarf domain. However, their sensitivity to metallicity must be investigated in detail with, for example, resolved photometry of M-dwarf wide common proper motion companions to FGKtype stars with well-determined stellar astrophysical parameters (Montes et al 2018;Espada 2019).…”

Section: Colour-colourmentioning

confidence: 99%

“…Determining precise stellar parameters of M dwarfs and how their uncertainties propagate to those of their planets is, therefore, of paramount importance. Many efforts have been undertaken in this respect, including empirical determination of masses, radii, and their relation to luminosity (Veeder 1974;Henry & McCarthy 1993;Chabrier & Baraffe 1997;Delfosse et al 2000;Bonfils et al 2005;Mann et al 2015Mann et al , 2019Terrien et al 2015;Benedict et al 2016;Schweitzer et al 2019), effective temperature, surface gravity, and metallicity (Casagrande et al 2008;Rojas-Ayala et al 2013;Montes et al 2018;Passegger et al 2018Passegger et al , 2019Rajpurohit et al 2018a), or activity and rotation periods (Stauffer & Hartmann 1986;Reid et al 1995;Hawley et al 1996Hawley et al , 2014Morales et al 2008;Newton et al 2015;Jeffers et al 2018;Díez Alonso et al 2019;Schöfer et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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CARMENES input catalogue of M dwarfs

Cifuentes

Caballero

Cortés-Contreras

et al. 2020

A&A

142

126

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Context. The relevance of M dwarfs in the search for potentially habitable Earth-sized planets has grown significantly in the last years. Aims. In our on-going effort to comprehensively and accurately characterise confirmed and potential planet-hosting M dwarfs, in particular for the CARMENES survey, we have carried out a comprehensive multi-band photometric analysis involving spectral energy distributions, luminosities, absolute magnitudes, colours, and spectral types, from which we have derived basic astrophysical parameters. Methods. We have carefully compiled photometry in 20 passbands from the ultraviolet to the mid-infrared, and combined it with the latest parallactic distances and close-multiplicity information, mostly from Gaia DR2, of a sample of 2479 K5 V to L8 stars and ultracool dwarfs, including 2210 nearby, bright M dwarfs. For this, we made extensive use of Virtual Observatory tools. Results. We have homogeneously computed accurate bolometric luminosities and effective temperatures of 1843 single stars, derived their radii and masses, studied the impact of metallicity, and compared our results with the literature. The over 40 000 individually inspected magnitudes, together with the basic data and derived parameters of the stars, individual and averaged by spectral type, have been made public to the astronomical community. In addition, we have reported 40 new close multiple systems and candidates (ρ < 3.3 arcsec) and 36 overluminous stars that are assigned to young Galactic populations. Conclusions. In the new era of exoplanet searches around M dwarfs via transit (e.g. TESS, PLATO) and radial velocity (e.g. CARMENES, NIRPS+HARPS), this work is of fundamental importance for stellar and therefore planetary parameter determination.

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Section: Colour-colourmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

CARMENES input catalogue of M dwarfs

Cifuentes

Caballero

Cortés-Contreras

et al. 2020

A&A

142

126

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“…Mann et al 2019;Schweitzer et al 2019) but also to characterise the habitable zones around planet-harbouring stars (Kasting et al 1993;Kopparapu et al 2013). Furthermore, correlations between the stellar metallicity and planet occurrence rates are now well established and shed light on planet formation mechanisms (Adibekyan et al 2014;Montes et al 2018;Delgado Mena et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Marfil

Tabernero

Montes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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With the purpose of assessing classic spectroscopic methods on high-resolution and high signal-to-noise ratio spectra in the near-infrared wavelength region, we selected a sample of 65 F-, G-, and K-type stars observed with CARMENES, the new, ultrastable, double-channel spectrograph at the 3.5 m Calar Alto telescope. We computed their stellar atmospheric parameters (T eff , log g, ξ, and [Fe/H]) by means of the StePar code, a Python implementation of the equivalent width method that employs the 2017 version of the MOOG code and a grid of MARCS model atmospheres. We compiled four Fe i and Fe ii line lists suited to metal-rich dwarfs, metal-poor dwarfs, metal-rich giants, and metal-poor giants that cover the wavelength range from 5 300 to 17 100Å, thus substantially increasing the number of identified Fe i and Fe ii lines up to 653 and 23, respectively. We examined the impact of the near-infrared Fe i and Fe ii lines upon our parameter determinations after an exhaustive literature search, placing special emphasis on the 14 Gaia benchmark stars contained in our sample. Even though our parameter determinations remain in good agreement with the literature values, the increase in the number of Fe i and Fe ii lines when the near-infrared region is taken into account reveals a deeper T eff scale that might stem from a higher sensitivity of the near-infrared lines to T eff .

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“…In this paper, we study planet-disc alignment in HD 113337 and HD 38529, which both host multiple giant planets (Fischer et al 2003;Borgniet et al 2019a), debris discs (Moro-Martín et al 2007b;Rhee et al 2007), and wide M-type stellar companions (Montes et al 2018). In both systems, the outer planets detected by radial velocity (RV) have masses ( ) and semimajor axes ( ) comparable to directly imaged planets like Pic b ( ∼ 13 Jup and ∼ 11 au, Gravity Collaboration et al 2020): HD 113337 c has sin ∼ 7 Jup and ∼ 4.8 au (Borgniet et al 2019a), while HD 38529 c has sin ∼ 13 Jup and ∼ 3.6 au (Fischer et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529

Xuan

Kennedy

Wyatt

et al. 2020

Monthly Notices of the Royal Astronomical Society

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HD 113337 and HD 38529 host pairs of giant planets, a debris disc, and wide M-type stellar companions. We measure the disc orientation with resolved images from Herschel and constrain the three-dimensional orbits of the outer planets with Gaia DR2 and Hipparcos astrometry. Resolved disc modelling leaves degeneracy in the disc orientation, so we derive four separate planet-disc mutual inclination (ΔI) solutions. The most aligned solutions give ΔI = 17 − 32○ for HD 113337 and ΔI = 21 − 45○ for HD 38529 (both 1σ). In both systems, there is a small probability (<0.3 per cent) that the planet and disc are nearly aligned (ΔI < 3○). The stellar and planetary companions cause the orbits of disc material to precess about a plane defined by the forced inclination. We determine this as well as the precession time-scale to interpret the mutual inclination results. We find that the debris discs in both systems could be warped via joint influences of the outer planet and stellar companion, potentially explaining the observed misalignments. However, this requires HD 113337 to be old (0.8-1.7 Gyr), whereas if young (14-21 Myr), the observed misalignment in HD 113337 could be inherited from the protoplanetary disc phase. For both systems, the inclination of the stellar spin axis is consistent with the disc and outer planet inclinations, which instead supports system-wide alignment or near alignment. High-resolution observations of the discs and improved constraints on the planetary orbits would provide firmer conclusions about the (mis)alignment status.

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Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics★

Cited by 73 publications

References 211 publications

CARMENES input catalogue of M dwarfs

CARMENES input catalogue of M dwarfs

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529

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