A VLBI resolution of the Pleiades distance controversy

  title={A VLBI resolution of the Pleiades distance controversy},
  author={Carl Melis and Mark J. Reid and Amy J. Mioduszewski and John R. Stauffer and Geoffrey C. Bower},
  pages={1029 - 1032}
Distance score settled for Seven Sisters Most of us have seen the Pleiades star cluster in the night sky, one of the few groups of physically related stars that are separately visible to the naked eye. In spite of its proximity to us, its distance has been disputed. Melis et al. settle the controversy with astrometric measurements from radio interferometry that reveal a distance of 136.2 parsecs (see the Perspective by Girardi). Other methods yielded similar values, but the trusted astrometry… 
Stellar twins determine the distance of the Pleiades
Since the release of the Hipparcos catalog in 1997, the distance to the Pleiades open cluster has been heavily debated. The distance obtained from Hipparcos and those by alternative methods differ by
A revised moving cluster distance to the Pleiades open cluster
Aims: We provide a new distance estimate for the Pleiades based on the moving cluster method, which will be useful to further discuss the so-called Pleiades distance controversy and compare it with
Pseudomagnitude Distances: Application to the Pleiades cluster
The concept of pseudomagnitude was recently introduced by Chelli et al. (2016), to estimate apparent stellar diameters using a strictly observational methodology. Pseudomagnitudes are distance
Young (125 Myr), populous (>1000 members), and relatively nearby, the Pleiades has provided an anchor for stellar angular momentum models for both younger and older stars. We used K2 to explore the
A 5D view of the α Per, Pleiades, and Praesepe clusters
Aims. Our scientific goal is to provide revised membership lists of the α Per, Pleiades, and Praesepe clusters exploiting the second data release of Gaia and produce five-dimensional maps (α, δ, π,
Dynamical Masses for the Pleiades Binary System HII-2147
We report our long-term spectroscopic monitoring of the Pleiades member HII-2147, which was previously spatially resolved at radio wavelengths in very long baseline interferometry (VLBI)
Long-term Spectroscopic Survey of the Pleiades Cluster: The Binary Population
We present the results of a spectroscopic monitoring program of the Pleiades region aimed at completing the census of spectroscopic binaries in the cluster, extending it to longer periods than
Beyond the Kepler/K2 bright limit: Variability in the seven brightest members of the Pleiades
The most powerful tests of stellar models come from the brightest stars in the sky, for which complementary techniques, such as astrometry, asteroseismology, spectroscopy, and interferometry can be
Reexamining the Lithium Depletion Boundary in the Pleiades and the Inferred Age of the Cluster
Moderate-dispersion (R ∼ 5400), optical spectroscopy of seven brown dwarf candidate members of the Pleiades was obtained using the Echellette Spectrograph and Imager on the Keck II telescope. The
High-Precision Radio and Infrared Astrometry of LSPM J1314+1320AB - I: Parallax, Proper Motions, and Limits on Planets
We present multi-epoch astrometric radio observations with the Very Long Baseline Array (VLBA) of the young ultracool-dwarf binary LSPM J1314+1320AB. The radio emission comes from the secondary star.


A distance of 133–137 parsecs to the Pleiades star cluster
The orbital parameters of the bright double star Atlas in the Pleiades are reported, using long-baseline optical/infrared interferometry, to derive a firm lower bound of D > 127’pc, with the most likely range being 133 < D < 137 pc.
The problem of the Pleiades distance - Constraints from Strömgren photometry of nearby field stars
The discrepancy between the Pleiades cluster distance based on Hipparcos parallaxes and main sequence tting is investigated on the basis of Stromgren photometry of F-type stars. Field stars with the
Toward a VLBI resolution of the Pleiades distance controversy
Abstract The Pleiades is the best-studied open cluster in the sky. It is one of the primary open clusters used to define the ‘zero-age main sequence,' and hence it serves as a cornerstone for
Parallaxes and proper motions for 20 open clusters as based on the new Hipparcos catalogue
Context. A new reduction of the astrometric data as produced by the Hipparcos mission has been published, claiming that the accuracies for nearly all stars brighter than magnitude Hp = 8 are
Eclipsing binaries as standard candles: HD 23642 and the distance to the Pleiades
We present a reanalysis of the light curves of HD 23642, a detached eclipsing binary star in the Pleiades open cluster, with emphasis on a detailed error analysis. We compare the masses and radii of
The distance to the Pleiades: Main sequence fitting in the near infrared
Hipparcos parallax measurements of stars in the Pleiades notoriously result in a cluster distance of 118 pc, which is approximately 10% shorter than the "classical" result obtained from earlier main
Confirmation of Errors in Hipparcos Parallaxes from Hubble Space Telescope Fine Guidance Sensor Astrometry of the Pleiades
We present absolute trigonometric parallaxes and relative proper motions for three members of the Pleiades, obtained with the Hubble Space Telescope's Fine Guidance Sensor 1r, a white-light
The Problem of Hipparcos Distances to Open Clusters. I. Constraints from Multicolor Main-Sequence Fitting
Parallax data from the Hipparcos mission allow the direct distance to open clusters to be compared with the distance inferred from main-sequence (MS) fitting. There are surprising differences between
The Pleiades, Map-based Trigonometric Parallaxes of Open Clusters. V.
The Multichannel Astrometric Photometer and Thaw Refractor (Thaw/MAP) of the University of Pittsburgh's Allegheny Observatory have been used to determine the trigonometric parallax of the Pleiades
The Pleiades eclipsing binary HD 23642 revisited
Context. HD 23642 is the only known eclipsing binary in the Pleiades, and therefore of importance in determining the distance to this cluster. Aims. To use new photometric and spectroscopic data in