2014

DOI: 10.1088/0004-6256/149/1/5

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The Solar Neighborhood. Xxxv. Distances to 1404 M Dwarf Systems Within 25 Pc in the Southern Sky

Jennifer G. Winters

¹

,

Todd J. Henry²,

³

et al.

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Introduction2

Carmenes Sample2

Survey Setup and Execution1

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Cited by 141 publications

(80 citation statements)

References 106 publications

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“…M-dwarf stars account for over 75% of the stars within 25 pc of the Sun (Winters et al 2015); and indeed, our nearest neighbour, Proxima Centauri, is an M5.5V star. Despite the prevalence of M-dwarfs, many aspects of their activity have remained less well characterised than more massive stars, mainly because of their inherent faintness.…”

Section: Introductionmentioning

confidence: 70%

Calculations of periodicity from Hαprofiles of Proxima Centauri

¹

,

²

,

³

2017

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We investigate retrieval of the stellar rotation signal for Proxima Centauri. We make use of high-resolution spectra taken with UVES and HARPS of Proxima Centauri over a 13-yr period as well as photometric observations of Proxima Centauri from ASAS and HST. We measure the Hα equivalent width and Hα index, skewness and kurtosis and introduce a method that investigates the symmetry of the line, the peak ratio, which appears to return better results than the other measurements. Our investigations return a most significant period of 82.6 ± 0.1 days, confirming earlier photometric results and ruling out a more recent result of 116.6 days which we conclude to be an alias induced by the specific HARPS observation times. We conclude that whilst spectroscopic Hα measurements can be used for period recovery, in the case of Proxima Centauri the available photometric measurements are more reliable. We make 2D models of Proxima Centauri to generate simulated Hα, finding that reasonable distributions of plage and chromospheric features are able to reproduce the equivalent width variations in observed data and recover the rotation period, including after the addition of simulated noise and flares. However the 2D models used fail to generate the observed variety of line shapes measured by the peak ratio. We conclude that only 3D models which incorporate vertical motions in the chromosphere can achieve this.

“…M-dwarf stars account for over 75% of the stars within 25 pc of the Sun (Winters et al 2015); and indeed, our nearest neighbour, Proxima Centauri, is an M5.5V star. Despite the prevalence of M-dwarfs, many aspects of their activity have remained less well characterised than more massive stars, mainly because of their inherent faintness.…”

Section: Introductionmentioning

confidence: 70%

Calculations of periodicity from Hαprofiles of Proxima Centauri

¹

,

²

,

³

2017

View full text Add to dashboard Cite

We investigate retrieval of the stellar rotation signal for Proxima Centauri. We make use of high-resolution spectra taken with UVES and HARPS of Proxima Centauri over a 13-yr period as well as photometric observations of Proxima Centauri from ASAS and HST. We measure the Hα equivalent width and Hα index, skewness and kurtosis and introduce a method that investigates the symmetry of the line, the peak ratio, which appears to return better results than the other measurements. Our investigations return a most significant period of 82.6 ± 0.1 days, confirming earlier photometric results and ruling out a more recent result of 116.6 days which we conclude to be an alias induced by the specific HARPS observation times. We conclude that whilst spectroscopic Hα measurements can be used for period recovery, in the case of Proxima Centauri the available photometric measurements are more reliable. We make 2D models of Proxima Centauri to generate simulated Hα, finding that reasonable distributions of plage and chromospheric features are able to reproduce the equivalent width variations in observed data and recover the rotation period, including after the addition of simulated noise and flares. However the 2D models used fail to generate the observed variety of line shapes measured by the peak ratio. We conclude that only 3D models which incorporate vertical motions in the chromosphere can achieve this.

“…The late-M subdwarf SSSPM J1444−2019 (Scholz et al 2004) with a parallax of 61.67 ± 2.12 mas (Schilbach et al 2009) should be added here. Jao et al (2008) reported in their Table 2 on some additional subdwarfs possibly falling in the 25 pc sample (with K s − M K s 2; see also Table 4 of Winters et al 2015). They also mentioned (in their Sect.…”

Section: Introductionmentioning

confidence: 91%

An ancient F-type subdwarf from the halo crossing the Galactic plane

¹

,

²

,

³

et al. 2015

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Aims. We selected the bluest object, WISE J0725−2351, from Luhman's new high proper motion (HPM) survey based on observations with the Wide-field Infrared Survey Explorer (WISE) for spectroscopic follow-up observations. Our aim was to unravel the nature of this relatively bright (V ∼ 12, J ∼ 11) HPM star (µ = 267 mas/yr). Methods. We obtained low-and medium-resolution spectra with the European Southern Observatory (ESO) New Technology Telescope (NTT)/EFOSC2 and Very Large Telescope (VLT)/X-Shooter instruments, investigated the radial velocity and performed a quantitative spectral analysis that allowed us to determine physical parameters. The fit of the spectral energy distribution based on the available photometry to low-metallicity model spectra and the similarity of our target to a metal-poor benchmark star (HD 84937) allowed us to estimate the distance and space velocity. Results. As in the case of HD 84937, we classified WISE J0725−2351 as sdF5: or a metal-poor turnoff star with [Fe/H] = −2.0 ± 0.2, T eff = 6250 ± 100 K, log g = 4.0 ± 0.2, and a possible age of about 12 Gyr. At an estimated distance of more than 400 pc, its proper motion translates to a tangential velocity of more than 500 km s −1 . Together with its constant (on timescales of hours, days, and months) and large radial velocity (about +240 km s −1 ), the resulting Galactic restframe velocity is about 460 km s −1 , implying a bound retrograde orbit for this extreme halo object that currently crosses the Galactic plane at high speed.

“…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%

“…(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,

et al. 2015

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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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