The Distribution of Stellar Mass in the Pleiades

Converse, Joseph M.; Stahler, Steven W.

doi:10.1086/529431

Cited by 31 publications

(37 citation statements)

References 34 publications

(48 reference statements)

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“…This relationship between stellar mass and the spatial distribution of stars in a cluster has been reported for the Pleiades with a similar degree of segregation, using a star counting technique for the two-dimensional case of the cluster projected onto the plane of the sky (Converse & Stahler 2008).…”

Section: Sizesupporting

confidence: 72%

An updated maximum likelihood approach to open cluster distance determination

Palmer

Arenou

Luri

et al. 2014

A&A

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Aims. An improved method for estimating distances to open clusters is presented and applied to Hipparcos data for the Pleiades and the Hyades. The method is applied in the context of the historic Pleiades distance problem, with a discussion of previous criticisms of Hipparcos parallaxes. This is followed by an outlook for Gaia, where the improved method could be especially useful. Methods. Based on maximum likelihood estimation, the method combines parallax, position, apparent magnitude, colour, proper motion, and radial velocity information to estimate the parameters describing an open cluster precisely and without bias. Results. We find the distance to the Pleiades to be 120.3 ± 1.5 pc, in accordance with previously published work using the same dataset. We find that error correlations cannot be responsible for the still present discrepancy between Hipparcos and photometric methods. Additionally, the three-dimensional space velocity and physical structure of Pleiades is parametrised, where we find strong evidence of mass segregation. The distance to the Hyades is found to be 46.35 ± 0.35 pc, also in accordance with previous results. Through the use of simulations, we confirm that the method is unbiased, so will be useful for accurate open cluster parameter estimation with Gaia at distances up to several thousand parsec.

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Section: Sizesupporting

confidence: 72%

An updated maximum likelihood approach to open cluster distance determination

Palmer

Arenou

Luri

et al. 2014

A&A

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“…Extrapolating the observed frequency of visual companions assuming an overall Gaussian orbital period distribution, Gizis & Reid (1995) suggested that CF open cluster M⋆ 0.1 M ⊙ = 27 ± 16%. Photometric studies, which may be affected by a mass segregation selection effect, broadly support these results despite some significant scatter (Boudreault et al 2012, Converse & Stahler 2008, Lodieu et al 2007, Pinfield et al 2003.…”

Section: Multiplicity Frequencymentioning

confidence: 57%

“…Assuming a mass ratio distribution similar to that of field FGK dwarfs (γ ∼ 0), the total frequency is therefore CF open cluster 0.7−1.3 M ⊙ ∼ 65%. Independently, photometric studies have suggested multiplicity frequencies in the 65-70% range for solartype stars (Converse & Stahler 2008, Kähler 1999.…”

Section: Multiplicity Frequencymentioning

confidence: 99%

Stellar Multiplicity

Duchêne

Kraus

2013

Annu. Rev. Astron. Astrophys.

1,315

1,285

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Stellar multiplicity is an ubiquitous outcome of the star formation process. Characterizing the frequency and main characteristics of multiple systems and their dependencies on primary mass and environment is therefore a powerful tool to probe this process. While early attempts were fraught with selection biases and limited completeness, instrumentation breakthroughs in the last two decades now enable robust analyses. In this review, we summarize our current empirical knowledge of stellar multiplicity for Main Sequence stars and brown dwarfs, as well as among populations of Pre-Main Sequence stars and embedded protostars. Clear trends as a function of both primary mass and stellar evolutionary stage are identified that will serve as a comparison basis for numerical and analytical models of star formation.

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“…Its approximately 1245 member stars have a total mass of about 740 M (Converse & Stahler 2008;Pinfield et al 1998) and its half-mass radius is 2 pc (Raboud & Mermilliod 1998). Dynamical models of the Pleiades show that the IMF of the Pleiades might have been similar to the Galactic field-star (i.e.…”

Section: Pleiadesmentioning

confidence: 99%

Inverse dynamical population synthesis

Marks

Kroupa

2012

A&A

253

302

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Binary populations in young star clusters show multiplicity fractions both lower and up to twice as high as those observed in the Galactic field. We follow the evolution of a population of binary stars in dense and loose star clusters starting with an invariant initial binary population and a formal multiplicity fraction of unity, and demonstrate that these models can explain the observed binary properties in Taurus, ρ Ophiuchus, Chamaeleon, Orion, IC 348, Upper Scorpius A, Praesepe, and the Pleiades. The model needs to consider solely different birth densities for these regions. The evolved theoretical orbital-parameter distributions are highly probable parent distributions for the observed ones. We constrain the birth conditions (stellar mass, M ecl , and half-mass radius, r h ) for the derived progenitors of the star clusters and the overall present-day binary fractions allowed by the present model. The results compare very well with properties of molecular cloud clumps on the verge of star formation. Combining these with previously and independently obtained constraints on the birth densities of globular clusters, we identify a weak stellar mass -half-mass radius correlation for cluster-forming cloud clumps, r h /pc ∝ (M ecl /M ) 0.13 ± 0.04 . The ability of the model to reproduce the binary properties in all the investigated young objects, covering present-day densities from 1−10 stars pc −3 (Taurus) to 2 × 10 4 stars pc −3 (Orion), suggests that environment-dependent dynamical evolution plays an important role in shaping the present-day properties of binary populations in star clusters, and that the initial binary properties may not vary dramatically between different environments.

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The Distribution of Stellar Mass in the Pleiades

Cited by 31 publications

References 34 publications

An updated maximum likelihood approach to open cluster distance determination

An updated maximum likelihood approach to open cluster distance determination

Stellar Multiplicity

Inverse dynamical population synthesis

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