Pismis 24-1: The Stellar Upper Mass Limit Preserved*

@article{Apellaniz2006Pismis2T,
  title={Pismis 24-1: The Stellar Upper Mass Limit Preserved*},
  author={Jes'us Ma'iz Apell'aniz and Nolan R. Walborn and Nidia I. Morrell and Virpi S. Niemela and Edmund P. Nelan},
  journal={The Astrophysical Journal},
  year={2006},
  volume={660},
  pages={1480-1485}
}
Is there a stellar upper mass limit? Recent statistical work seems to indicate that there is and that it is in the vicinity of 150 M☉. In this paper we use HST and ground-based data to investigate the brightest members of the cluster Pismis 24, one of which (Pismis 24-1) was previously inferred to have a mass greater than 200 M☉, in apparent disagreement with that limit. We determine that Pismis 24-1 is composed of at least three objects, the resolved Pismis 24-1SW and the unresolved… Expand

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References

SHOWING 1-10 OF 31 REFERENCES
On the upper limit on stellar masses in the Large Magellanic Cloud cluster R136
A truncated power-law distribution is fitted to the 29 largest stellar masses known in R136. Two different statistical techniques are used, with comparable results. An upper limit to the massExpand
Statistical confirmation of a stellar upper mass limit
We derive the expectation value for the maximum stellar mass (mmax) in an ensemble of N stars, as a function of the initial mass function (IMF) upper mass cutoff (mup) and N. We statisticallyExpand
Evidence for a fundamental stellar upper mass limit from clustered star formation
The observed masses of the most massive stars do not surpass about 150 M ○. . This may either be a fundamental upper mass limit which is defined by the physics of massive stars and/or theirExpand
An upper limit to the masses of stars
TLDR
There is an absence of stars with initial masses greater than 130 M [circdot] in the Arches cluster, whereas the typical mass function predicts 18.5; it is concluded that this indicates a firm limit of 150‬M [ Circdot] for stars. Expand
Resolving OB Systems in the Carina Nebula with the Hubble Space Telescope Fine Guidance Sensor
We observed 23 OB stars in the Carina Nebula (NGC 3372) with the Hubble Space Telescope's Fine Guidance Sensor 1r (FGS1r) in its high angular resolution mode. Five of these OB stars are newlyExpand
WR 20a Is an Eclipsing Binary: Accurate Determination of Parameters for an Extremely Massive Wolf-Rayet System
We present a high-precision I-band light curve for the Wolf-Rayet binary WR 20a, obtained as a subproject of the Optical Gravitational Lensing Experiment. Rauw et al. have recently presentedExpand
The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. II. Results from 12 Galactic Clusters and OB Associations
In a previous paper on the Magellanic Clouds, we demonstrated that coeval clusters provide a powerful tool for probing the progenitor masses of Wolf-Rayet (W-R) stars and luminous blue variablesExpand
A new calibration of stellar parameters of Galactic O stars
We present new calibrations of stellar parameters of O stars at solar metallicity taking non-LTE, wind, and line-blanketing effects into account. Gravities and absolute visual magnitudes are derivedExpand
The Lyman-Continuum Fluxes and Stellar Parameters of O and Early B-Type Stars
Using the results of the most recent stellar atmosphere models applied to a sample of hot stars, we construct calibrations of effective temperature (T(sub eff)), and gravity (log(sub g)) with aExpand
WR 20a: a massive cornerstone binary system comprising two extreme early-type stars ⋆
We analyse spectroscopic observations of WR 20a revealing that this star is a massive early-type binary system with a most probable orbital period of ∼3.675 days. Our spectra indicate that bothExpand
...
1
2
3
4
...