Calibration of the Mass-Luminosity Relation, II: Data from the General Catalogue of Trigonometric Stellar Parallaxes, 1995

Altena, W. F. van; Lee, J. T.; Hoffleit, E. D.; Girard, Terrence M.; Horch, Elliott

doi:10.1007/978-94-009-1477-3_23

Cited by 12 publications

(15 citation statements)

References 4 publications

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“…In Table B2 we list heliocentric distances and proper motions of all the investigated stars, which we used for discarding optical (non-physical) pairs. First, we compiled parallactic distances in the following order from the Tycho-Gaia Astrometric Solution (TGAS -Gaia Collaboration et al 2016), the new (HIP2 -van Leeuwen 2007) and old (HIP1 - Perryman et al 1997) Hipparcos reductions, van Altena et al (1995), and Prieur et al (2014; only for µ 02 Her BC). All 193 primaries have parallactic distances, while only 52 companions do.…”

Section: Discussionmentioning

confidence: 99%

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

González-Peinado

Tabernero

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We investigated almost 500 stars distributed among 193 binary or multiple systems made of late-F, G-, or early-K primaries and late-K or M dwarf companion candidates. For all of them, we compiled or measured coordinates, J-band magnitudes, spectral types, distances, and proper motions. With these data, we established a sample of 192 physically bound systems. In parallel, we carried out observations with HERMES/Mercator and obtained highresolution spectra for the 192 primaries and five secondaries. We used these spectra and the automatic StePar code for deriving precise stellar atmospheric parameters: T eff , log g, ξ, and chemical abundances for 13 atomic species, including [Fe/H]. After computing Galactocentric space velocities for all the primary stars, we performed a kinematic analysis and classified them in different Galactic populations and stellar kinematic groups of very different ages, which match our own metallicity determinations and isochronal age estimations. In particular, we identified three systems in the halo and 33 systems in the young Local Association, Ursa Major and Castor moving groups, and IC 2391 and Hyades Superclusters. We finally studied the exoplanet-metallicity relation in our 193 primaries and made a list 13 M-dwarf companions with very high metallicity that can be the targets of new dedicated exoplanet surveys. All in all, our dataset will be of great help for future works on the accurate determination of metallicity of M dwarfs.

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Section: Discussionmentioning

confidence: 99%

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

González-Peinado

Tabernero

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…The RECONS survey (Henry et al 2006) has cataloged the population of stars within 10 pc and determined that 75% of nearby stars are M dwarfs. Supplementing the sample of stars within 10 pc with additional catalogs of stars with known parallaxes (van Altena et al 1995;Perryman et al 1997;Lépine 2005;Dittmann et al 2014) and assuming planet occurrence rates from Dressing & Charbonneau (2013) reveals that there should be approximately 80 transiting planets within 20 pc. Roughly 10 of those planets are likely to be potentially rocky planets orbiting within the habitable zone with the closest system located within 9 AE 3 pc and orbiting a star as bright as J ∼ 5:5 AE 0:9 mag (Dressing et al, 2014).…”

Section: Expected Number Of Targetsmentioning

confidence: 99%

Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST)

Beichman¹,

Benneke²,

Knutson³

et al. 2014

Publications of the Astronomical Society of the Pacific

279

207

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9down to "super-Earths" with diameters less than three times that of the Earth ).JWST will revolutionize our knowledge of the physical properties of dozens to possibly hundreds of exoplanets by making a variety of different types of observations. Here we focus on transits and phase curves; direct detection via coronagraphy was considered in a 2007 white paper (for all JWST white papers see http://www.stsci.edu/jwst/doc-archive/whitepapers) and will be revisited in the near future.JWST 's unique combination of high sensitivity and broad wavelength coverage enables the accurate measurement of transit and orbital parameters with high signal-to-noise (SNR). Most importantly, JWST will investigate planetary atmospheres, determine atomic and molecular compositions, probe vertical and horizontal structure, and follow dynamical evolution (i.e. exoplanet weather). It will do this for a diverse population of planets of varying masses and densities, in a wide variety of environments characterized by a range of host star masses and metallicities, orbital semi-major axes and eccentricities. 3The sensitivity of JWST over its wavelength range of 0.6 to 28 microns compared to other missions and ground-based facilities has been amply documented (http://www.stsci.edu/jwst/science/sensitivity) and JWST 's halo orbit around the Earth-Sun L2 point provides long, highly stable, uninterrupted observing sequences 3 Of particular interest for JWST will be small planets (R< 2−4R ⊕ ) located at a distance from their host stars such that their equilibrium temperatures could be comparable to that of our Earth. The range of the so-called "Habitable Zone" has been argued over by many authors since its original definition (Kasting et al. 1993). We take an agnostic approach to this question, referring loosely to planets whose stellar insolation is comparable to that of our own.-10compared with the ground or HST. JWST 's detectors are capable of much better than 100 parts per million (ppm) precision over time periods from hours to days. Its suite of four instruments and multiple operating modes provides a large range of choices in trading off spectral resolution (R between 4 -3000), photometric sensitivity, and observing time. Taken together, these characteristics will make JWST's transit and eclipse observations the best method for characterizing exoplanet atmospheres in the foreseeable future.

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“…Nevertheless, there are no PNe located close enough to allow the use of this method by means of traditional techniques ; for this reason, the method had not been successfully used previously, since the errors obtained imply nonsigniÐcant results (see, for example, van Altena, Lee, & Hoffleit 1995). But now, with the use of new instrumental techniques, such as CCD detectors, which allow the determination of parallaxes with errors of the order of ^0A .001 (Monet & Dahn 1983 ;Anguita & Ruiz 1988 ;Monet et al 1992), the distance of a PN located at 500 pc (parallax \ may be determined with an accuracy of 50% or 0A .002) better, as was recently demonstrated by Harris et al (1997, hereafter USNO97).…”

Section: èèèèèèèèèèèèèèèmentioning

confidence: 99%

Trigonometric Distances of Planetary Nebulae

Gutiérrez‐Moreno

Anguita

Loyola

et al. 1999

PUBL ASTRON SOC PAC

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ABSTRACT. Trigonometric parallaxes of three planetary nebulae (A21, A29, and He 2-11) have been determined. The method of observation and reduction is brieÑy presented. The results for A21 and A29 are within the formal errors of the values published by USNO Flagsta † Station. The trigonometric method is discussed in comparison with other methods generally used for distance determination. We have found that statistical distances show no correlation with trigonometric distances, while other methods, which do not involve any assumption about the central stars of the nebulae, give in general fairly good correlations.

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Calibration of the Mass-Luminosity Relation, II: Data from the General Catalogue of Trigonometric Stellar Parallaxes, 1995

Cited by 12 publications

References 4 publications

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★

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★

Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST)

Trigonometric Distances of Planetary Nebulae

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