An updated maximum likelihood approach to open cluster distance determination

Palmer, M.; Arenou, Frédéric; Luri, X.; Masana, E.

doi:10.1051/0004-6361/201323037

Cited by 15 publications

(20 citation statements)

References 26 publications

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“…Our result of 134.8 ± 1.7 pc, based on Hipparcos parallaxes of field stars, disagrees with the value directly derived from Hipparcos parallaxes of Pleiades members (van Leeuwen 2007;Perryman 2008;van Leeuwen 2009;Palmer et al 2014) but it is in good agreement with the value provided by the model-based methods mentioned earlier (Pinsonneault et al 1998;Percival et al 2005;Valls-Gabaud 2007;Groenewegen et al 2007;Pan et al 2004;Melis et al 2014). Since most of these methods (except…”

Section: Discussioncontrasting

confidence: 78%

“…4 our Pleiades twin parallax with Hipparcos parallaxes of 54 Pleiades stars that are usually considered for the astrometric solution (e.g. Makarov 2002;van Leeuwen 2007;Palmer et al 2014). The bright stars (H < 7 mag) have accurate Hipparcos parallaxes with a low star-to-star scatter of 0.5 mas with an averaged parallax of 8.36 ± 0.09 mas (Fig.…”

Section: Parallax Of Individual Pleiades Starsmentioning

confidence: 99%

“…Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) Palmer et al 2014) while other methods mainly using theoretical modelling estimate a distance of approximately 134 pc, i.e. a parallax of about 7.46 mas.…”

Section: Introductionmentioning

confidence: 99%

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Stellar twins determine the distance of the Pleiades

Mädler

Jofré

Gilmore

et al. 2016

A&A

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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 10 to 15%. As accurate stellar distances are key to understanding stellar structure and evolution, this dilemma puts the validity of stellar evolution models into question. Using our model-independent method to determine parallaxes based on twin stars, we report individual parallaxes of 15 FGK type stars in the Pleiades in anticipation of the astrometric mission Gaia. These parallaxes give a mean cluster parallax of 7.42 ± 0.09 mas corresponding to a mean cluster distance of 134.8 ± 1.7 pc. This value agrees with the current results obtained from stellar evolution models.

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Section: Discussioncontrasting

confidence: 78%

Section: Parallax Of Individual Pleiades Starsmentioning

confidence: 99%

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Stellar twins determine the distance of the Pleiades

Mädler

Jofré

Gilmore

et al. 2016

A&A

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“…We then found the distance that gives U V W values consistent with the established value of the cluster (van Leeuwen 2009). We allowed for a variation of 1.2 km/s in the cluster value due to dispersion from internal kinematics (Palmer et al 2014). Accounting for this, as well as errors in the proper motion and RV, gave a distance of 45.7±3.3 pc.…”

Section: Stellar Parametersmentioning

confidence: 99%

Zodiacal Exoplanets in Time (Zeit). I. A Neptune-Sized Planet Orbiting an M4.5 Dwarf in the Hyades Star Cluster

Mann

Gaidos

Mace

et al. 2016

ApJ

196

206

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Studying the properties of young planetary systems can shed light on how the dynamics and structure of planets evolve during their most formative years. Recent K2 observations of nearby young clusters (10-800 Myr) havefacilitated the discovery of such planetary systems. Here we report the discovery of a Neptune-sized planet transiting an M4.5 dwarf (K2-25) in the Hyades cluster (650-800 Myr). The lightcurve shows a strong periodic signal at 1.88 days, which we attribute to spot coverage and rotation. We confirm thatthe planet host is a member of the Hyades by measuring the radial velocity of the system with the high-resolution near-infrared spectrograph Immersion Grating Infrared Spectrometer. This enables us to calculate a distance based on K2-25ʼs kinematics and membership to the Hyades, which in turn provides a stellar radius and mass to ;5%-10%, better than what is currently possible for most Kepler M dwarfs (12%-20%). We use the derived stellar density as a prior on fitting the K2 transit photometry, which provides weak constraints on eccentricity. Utilizing a combination of adaptive optics imaging and high-resolution spectra, we rule out the possibility that the signal is due to a bound or background eclipsing binary, confirming the transits' planetary origin. K2-25b has a radius (3.43 0.31 0.95 -+ R ⊕ ) much larger than older Kepler planets with similar orbital periods (3.485 days) and host-star masses (0.29 M e ). This suggests that close-in planets lose some of their atmospheres past the first few hundred million years. Additional transiting planets around the Hyades, Pleiades, and Praesepe clusters from K2 will help confirm whether this planet is atypical or representative of other close-in planets of similar age.

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“…The distances to objects in the Pleiades and Praesepe were assumed constant at 120 pc (e.g. Palmer et al 2014) and 182 pc (e.g. Boudreault et al 2012), respectively.…”

Section: Example 2: Nearby Spectroscopic Binariesmentioning

confidence: 99%

Gaia's potential for the discovery of circumbinary planets

Sahlmann

Triaud

Martin

2014

Monthly Notices of the Royal Astronomical Society

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The abundance and properties of planets orbiting binary stars -circumbinary planets -are largely unknown because they are difficult to detect with currently available techniques. Results from the Kepler satellite and other studies indicate a minimum occurrence rate of circumbinary giant planets of ∼10 %, yet only a handful are presently known. Here, we study the potential of ESA's Gaia mission to discover and characterise extrasolar planets orbiting nearby binary stars by detecting the binary's periodic astrometric motion caused by the orbiting planet. We expect that Gaia will discover hundreds of giant planets around binaries with FGK dwarf primaries within 200 pc of the Sun, if we assume that the giant planet mass distribution and abundance are similar around binaries and single stars. If on the other hand all circumbinary gas giants have masses lower than two Jupiter masses, we expect only four detections. Gaia is critically sensitive to the properties of giant circumbinary planets and will therefore make the detailed study of their population possible. Gaia's precision is such that the distribution in mutual inclination between the binary and planetary orbital planes will be obtained. It also possesses the capacity to establish the frequency of planets across the H-R diagram, both as a function of mass and of stellar evolutionary state from pre-main sequence to stellar remnants. Gaia's discoveries can reveal whether a second epoch of planetary formation occurs after the red-giant phase.

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An updated maximum likelihood approach to open cluster distance determination

Cited by 15 publications

References 26 publications

Stellar twins determine the distance of the Pleiades

Stellar twins determine the distance of the Pleiades

Zodiacal Exoplanets in Time (Zeit). I. A Neptune-Sized Planet Orbiting an M4.5 Dwarf in the Hyades Star Cluster

Gaia's potential for the discovery of circumbinary planets

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