Stellar twins determine the distance of the Pleiades

Mädler, Thomas; Jofré, P.; Gilmore, G.; Worley, C. C.; Soubiran, C.; Blanco-Cuaresma, S.; Hawkins, Keith; Casey, Andrew R.

doi:10.1051/0004-6361/201629091

Cited by 12 publications

(8 citation statements)

References 37 publications

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“…The method of double stars orbital modeling led to cluster's distance value of 138.0±1.5 pc (Groenewegen et al 2007). Recently, the twin stars method yielded the distance of 134.8 ± 1.7 pc to the Pleiades open cluster ( Mädler et al 2016). As can be noticed, majority of the distance estimates provide similar results, close to ∼135 pc.…”

Section: Introductionmentioning

confidence: 92%

The Pleiades apex and its kinematical structure

Elsanhoury¹,

Postnikova²,

Чупина³

et al. 2018

Astrophys Space Sci

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A study of cluster characteristics and internal kinematical structure of the middle-aged Pleiades open star cluster is presented. The individual star apexes and various cluster kinematical parameters including the velocity ellipsoid parameters are determined using both Hipparcos and Gaia data. Modern astrometric parameters were taken from the Gaia Data Release 1 (DR1) in combination with the Radial Velocity Experiment Fifth Data Release (DR5). The necessary set of parameters including parallaxes, proper motions and radial velocities are used for n=17 stars from Gaia DR1+RAVE DR5 and for n=19 stars from the Hipparcos catalog using SIMBAD data base. Single stars are used to improve accuracy by eliminating orbital movements. RAVE DR5 measurements were taken only for the stars with the radial velocity errors not exceeding 2 km/s. For the Pleiades stars taken from Gaia, we found mean heliocentric distance as 136.8 ± 6.4 pc, and the apex position is calculated as: A CP = 92 • .52 ± 1 • .72, D CP = −42 • .28 ± 2 • .56 by the convergent point method and A 0 = 95 • .59 ± 2 • .30 and D 0 = −50 • .90 ± 2 • .04 using AD-diagram method (n=17 in both cases). The results are compared with those obtained historically before the Gaia mission era.

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Section: Introductionmentioning

confidence: 92%

The Pleiades apex and its kinematical structure

Elsanhoury¹,

Postnikova²,

Чупина³

et al. 2018

Astrophys Space Sci

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show abstract

“…Yet the Hipparcos parallaxes were not without problems, perhaps the most significant of which was the aberrant distance to the Pleiades which the Hipparcos parallax placed at 120.2 ± 1.9 pc (van Leeuwen 2009) as compared to the broadly accepted distance of ≈135 pc from a variety of methods (e.g., Munari et al 2004;Zwahlen et al 2004;Soderblom et al 2005;Groenewegen et al 2007;Melis et al 2014;Mädler et al 2016, and others cited therein). Several of these recent determinations are formally highly precise (σ = 1.2-1.7 pc).…”

Section: Introductionmentioning

confidence: 99%

Eclipsing Binary Stars as Benchmarks for Trigonometric Parallaxes in the Gaia Era

2016

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We present fits to the broadband photometric spectral energy distributions (SEDs) of 158 eclipsing binaries (EBs) in the Tycho-2 catalog. These EBs were selected because they have highly precise stellar radii, effective temperatures, and in many cases metallicities previously determined in the literature, and thus have bolometric luminosities that are typically good to 10%. In most cases the available broadband photometry spans a wavelength range 0.4-10 µm, and in many cases spans 0.15-22 µm. The resulting SED fits, which have only extinction as a free parameter, provide a virtually model-independent measure of the bolometric flux at Earth. The SED fits are satisfactory for 156 of the EBs, for which we achieve typical precisions in the bolometric flux of ≈3%. Combined with the accurately known bolometric luminosity, the result for each EB is a predicted parallax that is typically precise to 5%. These predicted parallaxeswith typical uncertainties of 200 µas-are 4-5 times more precise than those determined by Hipparcos for 99 of the EBs in our sample, with which we find excellent agreement. There is no evidence among this sample for significant systematics in the Hipparcos parallaxes of the sort that notoriously afflicted the Pleiades measurement. The EBs are distributed over the entire sky, span more than 10 mag in brightness, reach distances of more than 5 kpc, and in many cases our predicted parallaxes should also be more precise than those expected from the Gaia first data release. The EBs studied here can thus serve as empirical, independent benchmarks for these upcoming fundamental parallax measurements.

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“…Due to the exquisite precision and accuracy of the Gaia data, the agreement between our derived values and the literature values are good. The adopted average distances for the Pleiades (Mädler et al 2016), α Per (van Leeuwen 2009), Hyades (van Leeuwen 2007) and LCC (de Zeeuw et al 1999) are 135 pc, 172 pc, 47 and 118 pc, respectively. In lower right panel, we show the mass distributions of the four groups, which all share a similar slope.…”

Section: Comparing To Nearby Cluster and Moving Group Membersmentioning

confidence: 99%

Fundamental Properties of Co-moving Stars Observed by Gaia

Bochanski

Faherty

Gagné

et al. 2018

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We have estimated fundamental parameters for a sample of co-moving stars observed by Gaia and identified by Oh et al. (2017b). We matched the Gaia observations to the 2MASS and WISE catalogs and fit MIST isochrones to the data, deriving estimates of the mass, radius, [Fe/H], age, distance and extinction to 9,754 stars in the original sample of 10,606 stars. We verify these estimates by comparing our new results to previous analyses of nearby stars, examining fiducial cluster properties, and estimating the power-law slope of the local present-day mass function. A comparison to previous studies suggests that our mass estimates are robust, while metallicity and age estimates are increasingly uncertain. We use our calculated masses to examine the properties of binaries in the sample, and show that separation of the pairs dominates the observed binding energies and expected lifetimes.

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Stellar twins determine the distance of the Pleiades

Cited by 12 publications

References 37 publications

The Pleiades apex and its kinematical structure

The Pleiades apex and its kinematical structure

Eclipsing Binary Stars as Benchmarks for Trigonometric Parallaxes in the Gaia Era

Fundamental Properties of Co-moving Stars Observed by Gaia

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