The solar neighborhood, 1: Standard spectral types (K5-M8) for northern dwarfs within eight parsecs

Henry, Todd J.; Kirkpatrick, J. Davy; Simons, Douglas A.

doi:10.1086/117167

Cited by 213 publications

(188 citation statements)

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“…We started to fill the CARMENES database with the M dwarfs from the Research Consortium on Nearby Stars 2 , which catalogues all known stars with measured astrometric parallaxes that place them within 10 pc (e.g., Henry et al 1994;Kirkpatrick et al 1995;Riedel et al 2014;Winters et al 2015). The RECONS stellar compilation was next completed with the Palomar/Michigan State University survey catalogue of nearby stars (PMSU -Reid et al 1995Hawley et al 1996;Gizis et al 2002).…”

Section: Carmenes Samplementioning

confidence: 99%

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CARMENES input catalogue of M dwarfs

Alonso-Floriano¹,

Morales²,

Caballero³

et al. 2015

A&A

192

178

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Context. CARMENES is a stabilised, high-resolution, double-channel spectrograph at the 3.5 m Calar Alto telescope. It is optimally designed for radial-velocity surveys of M dwarfs with potentially habitable Earth-mass planets. Aims. We prepare a list of the brightest, single M dwarfs in each spectral subtype observable from the northern hemisphere, from which we will select the best planet-hunting targets for CARMENES. Methods. In this first paper on the preparation of our input catalogue, we compiled a large amount of public data and collected lowresolution optical spectroscopy with CAFOS at the 2.2 m Calar Alto telescope for 753 stars. We derived accurate spectral types using a dense grid of standard stars, a double least-squares minimisation technique, and 31 spectral indices previously defined by other authors. Additionally, we quantified surface gravity, metallicity, and chromospheric activity for all the stars in our sample. Results. We calculated spectral types for all 753 stars, of which 305 are new and 448 are revised. We measured pseudo-equivalent widths of Hα for all the stars in our sample, concluded that chromospheric activity does not affect spectral typing from our indices, and tabulated 49 stars that had been reported to be young stars in open clusters, moving groups, and stellar associations. Of the 753 stars, two are new subdwarf candidates, three are T Tauri stars, 25 are giants, 44 are K dwarfs, and 679 are M dwarfs. Many of the 261 investigated dwarfs in the range M4.0-8.0 V are among the brightest stars known in their spectral subtype. Conclusions. This collection of low-resolution spectroscopic data serves as a candidate target list for the CARMENES survey and can be highly valuable for other radial-velocity surveys of M dwarfs and for studies of cool dwarfs in the solar neighbourhood.

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Section: Carmenes Samplementioning

confidence: 99%

“…(c) With spectral types derived from spectroscopy in this work. (d) RECONS: Henry et al (1994Henry et al ( , 2006; Kirkpatrick et al (1995); Jao et al (2011);Riedel et al (2014); Winters et al (2015) and references therein.…”

Section: Carmenes Samplementioning

confidence: 99%

CARMENES input catalogue of M dwarfs

Alonso-Floriano¹,

Morales²,

Caballero³

et al. 2015

A&A

192

178

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“…HARPS or HARPS-N spectra were obtained for a sample of 33 stars with homogeneously derived spectral types in Kirkpatrick et al (1991) and Henry et al (1994). The sample contains stars with spectral types between K7V and M4.5V.…”

Section: Spectral Typesmentioning

confidence: 99%

Stellar parameters of early-M dwarfs from ratios of spectral features at optical wavelengths

Maldonado

Affer

Micela

et al. 2015

A&A

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Context. Low-mass stars have been recognised as promising targets in the search for rocky, small planets with the potential of supporting life. As a consequence, Doppler search programmes using high-resolution spectrographs like HARPS or HARPS-N are providing huge quantities of optical spectra of M dwarfs. However, determining the stellar parameters of M dwarfs using optical spectra has proven to be challenging. Aims. We aim to calibrate empirical relationships to determine accurate stellar parameters for early-M dwarfs (spectral types M0-M4.5) using the same spectra as those that are used for radial velocity determinations, without the necessity of acquiring IR spectra or relying on atmospheric models and/or photometric calibrations. Methods. Our methodology consists of using ratios of pseudo-equivalent widths of spectral features as a temperature diagnostic, a technique frequently used in solar-type stars. Stars with effective temperatures obtained from interferometric estimates of their radii are used as calibrators. Empirical calibrations for the spectral type are also provided. Combinations of features and ratios of features are used to derive calibrations for the stellar metallicity. Our methods are then applied to a large sample of M dwarfs that are currently being observed in the framework of the HARPS GTO search for extrasolar planets. The derived temperatures and metallicities are used together with photometric estimates of mass, radius, and surface gravity to calibrate empirical relationships for these parameters. Results. A long list of spectral features in the optical spectra of early-M dwarfs was identified. This list shows that the pseudoequivalent width of roughly 43% of the features is strongly anticorrelated with the effective temperature. The correlation with the stellar metallicity is weaker. A total of 112 temperature sensitive ratios were identified and calibrated over the range 3100−3950 K, providing effective temperatures with typical uncertainties of about 70 K. Eighty-two ratios of pseudo-equivalent widths of features were calibrated to derive spectral types within 0.5 subtypes for stars with spectral types between K7V and M4.5V. We calibrated 696 combinations of the pseudo-equivalent widths of individual features and temperature-sensitive ratios for the stellar metallicity over a metallicity range from −0.54 to +0.24 dex, with estimated uncertainties in the range of 0.07−0.10 dex. We provide our own empirical calibrations for stellar mass, radius, and surface gravity. These parameters depend on the stellar metallicity. For a given effective temperature, lower metallicities predict lower masses and radii as well as higher gravities.

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“…The M-dwarfs were selected from the samples of Henry et al (1994) and Kirkpatrick et al (1995Kirkpatrick et al ( , 1999 according to observability, magnitude, and spectral-type classification. The selection of the L-dwarf sample was described in T01.…”

Section: The Samplementioning

confidence: 99%

A low-resolution near-infrared spectral library of M-, L-, and T-dwarfs

Testi

2009

A&A

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We present complete near-infrared (0.85-2.45 μm), low-resolution (R ∼ 100) spectra of a sample of 54 disk M-, L-, and T-dwarfs with reliable optical or near infrared spectral-type classification from the literature. The observations were obtained with a prism-based optical element, the Amici device, which provides a complete spectrum of the source on the detector. Our observations indicate that low-resolution near-infrared spectroscopy can be used to determine the spectral classification of late-type field dwarfs in a fast but accurate way. We derive a set of near-infrared spectral indices that are useful to the classification of field dwarfs not seriously affected by reddening. Finally, we show that the comparison of Amici spectra with model atmospheres allows us to obtain a reliable estimate of the dwarf effective temperatures.

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The solar neighborhood, 1: Standard spectral types (K5-M8) for northern dwarfs within eight parsecs

Cited by 213 publications

References 0 publications

CARMENES input catalogue of M dwarfs

CARMENES input catalogue of M dwarfs

Stellar parameters of early-M dwarfs from ratios of spectral features at optical wavelengths

A low-resolution near-infrared spectral library of M-, L-, and T-dwarfs

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