The CMC15, the last issue of the series “Carlsberg Meridian Catalogue, La Palma”

Muiños, J. L.; Evans, D. W.

doi:10.1002/asna.201312045

Cited by 32 publications

(22 citation statements)

References 7 publications

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“…To determine new stellar parameters, we first collected broadband photometry from several surveys covering the whole spectral energy distribution (SED) of all CARMENES GTO targets (Caballero et al 2016a). In order to determine the stellar luminosity L, we used the Virtual Observatory SED Analyzer (Bayo et al 2008), the Gaia parallactic distance, and photometry from the following catalogs: SDSS (Ahn et al 2012), UCAC4 (Zacharias et al 2013), Tycho-2 (Høg et al 2000), Gaia DR2 (Gaia Collaboration 2018), CMC15 (Muiños & Evans 2014), 2MASS (Skrutskie et al 2006), and AllWISE (Cutri & et al 2013). In the GALEX passbands (Bianchi et al 2011) and SDSS u, the M-dwarf photometry is dominated by chromospheric emission.…”

Section: Host Star Hd 180617 (Gj 752 A)mentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

Kaminski

Trifonov

Caballero

et al. 2018

A&A

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Despite their activity, low-mass stars are of particular importance for the search of exoplanets by the means of Doppler spectroscopy, as planets with lower masses become detectable. We report on the discovery of a planetary companion around HD 180617, a bright (J = 5.58 mag), low-mass (M = 0.45M⊙) star of spectral type M2.5 V. The star, located at a distance of 5.9 pc, is the primary of the high proper motion binary system containing vB 10, a star with one of the lowest masses known in most of the twentieth century. Our analysis is based on new radial velocity (RV) measurements made at red-optical wavelengths provided by the high-precision spectrograph CARMENES, which was designed to carry out a survey for Earth-like planets around M dwarfs. The available CARMENES data are augmented by archival Doppler measurements from HIRES and HARPS. Altogether, the RVs span more than 16 yr. The modeling of the RV variations, with a semi-amplitude of K = 2.85-0.25+0.16 m s-1, yields a Neptune-like planet with a minimum mass of 12.2-1.4+1.0 M⊕ on a 105.90-0.10+0.09 d circumprimary orbit, which is partly located in the host star’s habitable zone. The analysis of time series of common activity indicators does not show any dependence on the detected RV signal. The discovery of HD 180617 b not only adds information to a currently hardly filled region of the mass-period diagram of exoplanets around M dwarfs, but the investigated system becomes the third known binary consisting of M dwarfs and hosting an exoplanet in an S-type configuration. Its proximity makes it an attractive candidate for future studies.

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Section: Host Star Hd 180617 (Gj 752 A)mentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

Kaminski

Trifonov

Caballero

et al. 2018

A&A

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“…Comparisons have been done with respect to the following external photometric catalogues: Tycho 2 (Høg et al 2000), CMC15 (Muiños & Evans 2014), APASS (Henden et al 2015), and SDSS DR12 (Alam et al 2015). The results of these comparisons are shown in Fig.…”

Section: Comparisons With External Cataloguesmentioning

confidence: 99%

GaiaData Release 1

Evans

Riello

Angeli

et al. 2017

A&A

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Aims. The photometric validation of the Gaia DR1 release of the ESA Gaia mission is described and the quality of the data shown. Methods. This is carried out via an internal analysis of the photometry using the most constant sources. Comparisons with external photometric catalogues are also made, but are limited by the accuracies and systematics present in these catalogues. An analysis of the quoted errors is also described. Investigations of the calibration coefficients reveal some of the systematic effects that affect the fluxes.Results. The analysis of the constant sources shows that the early-stage photometric calibrations can reach an accuracy as low as 3 mmag.

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“…(1) Henry et al (2000); (2) ( Zacharias et al 2004), the Tycho-2 catalogue (Høg et al 2000), The Amateur Sky Survey (TASS, Droege et al 1997) and the Carlsberg Meridian Catalog 14 (Muiños & Evans 2014 Skrutskie et al 2006). The synthetic stellar spectra used for the numerical integration of the fluxes are from Kurucz (1993).…”

Section: 39mentioning

confidence: 99%

Comparison of gyrochronological and isochronal age estimates for transiting exoplanet host stars

Maxted

Serenelli

Southworth

2015

A&A

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Context. Tidal interactions between planets and their host stars are not well understood, but may be an important factor in their formation, structure, and evolution. Previous studies suggest that these tidal interactions may be responsible for discrepancies between the ages of exoplanet host stars estimated using stellar models (isochronal age estimates) and age estimates based on the stars' rotation periods (gyrochronological age estimates). Recent improvements in our understanding of the rotational evolution of single stars and a substantial increase in the number of exoplanet host stars with accurate rotation period measurements make it worthwhile to revisit this question. Aims. Our aim is to determine whether the gyrochronological age estimates for transiting exoplanet host stars with accurate rotation period measurements are consistent with their isochronal age estimates, and whether this is indicative of tidal interaction between the planets and their host stars. Methods. We have compiled a sample of 28 transiting exoplanet host stars with measured rotation periods, including two stars (HAT-P-21 and WASP-5) for which the rotation period based on the light curve modulation is reported here for the first time. We use our recently developed Bayesian Markov chain Monte Carlo method to determine the joint posterior distribution for the mass and age of each star in the sample. We extend our Bayesian method to include a calculation of the posterior distribution of the gyrochronological age estimate that accounts for the uncertainties in the mass and age, the strong correlation between these values, and the uncertainties in the mass-rotation-age calibration. Results. The gyrochronological age estimate (τ gyro ) is significantly lower than the isochronal age estimate for about half of the stars in our sample. Tidal interactions between the star and planet are a reasonable explanation for this discrepancy in some cases, but not all. The distribution of τ gyro values is evenly spread from very young ages up to a maximum value of a few Gyr, i.e. there is no obvious pileup of stars at very low or very high values of τ gyro as might be expected if some evolutionary or selection effect were biasing the age distribution of the stars in this sample. There is no clear correlation between τ gyro and the strength of the tidal force on the star due to the innermost planet. There is clear evidence that the isochronal age estimates for some K-type stars are too high, and this may also be the case for some G-type stars. This may be the result of magnetic inhibition of convection. The densities of HAT-P-11 and WASP-84 are too high to be reproduced by any stellar models within the observed constraints on effective temperature and metallicity. These stars may have strongly enhanced helium abundances. There is currently no satisfactory explanation for the discrepancy between the young age for CoRoT-2 estimated from either gyrochronology or its high lithium abundance, and the extremely old age for its K-type stellar companion...

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The CMC15, the last issue of the series “Carlsberg Meridian Catalogue, La Palma”

Cited by 32 publications

References 7 publications

The CARMENES search for exoplanets around M dwarfs

The CARMENES search for exoplanets around M dwarfs

GaiaData Release 1

Comparison of gyrochronological and isochronal age estimates for transiting exoplanet host stars

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