CORE–HALO AGE GRADIENTS AND STAR FORMATION IN THE ORION NEBULA AND NGC 2024 YOUNG STELLAR CLUSTERS

@article{Getman2014COREHALOAG,
  title={CORE–HALO AGE GRADIENTS AND STAR FORMATION IN THE ORION NEBULA AND NGC 2024 YOUNG STELLAR CLUSTERS},
  author={Konstantin V. Getman and Eric D. Feigelson and Michael A. Kuhn},
  journal={The Astrophysical Journal},
  year={2014},
  volume={787}
}
We analyze age distributions of two nearby rich stellar clusters, the NGC 2024 (Flame Nebula) and Orion Nebula cluster (ONC) in the Orion molecular cloud complex. Our analysis is based on samples from the MYStIX survey and a new estimator of pre-main sequence (PMS) stellar ages, AgeJX, derived from X-ray and near-infrared photometric data. To overcome the problem of uncertain individual ages and large spreads of age distributions for entire clusters, we compute median ages and their confidence… 
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References

SHOWING 1-10 OF 77 REFERENCES
No wide spread of stellar ages in the Orion Nebula Cluster
The wide luminosity dispersion seen for stars at a given effective temperature in the Hertzsprung–Russell diagrams of young clusters and star-forming regions is often interpreted as due to
MASS AND LUMINOSITY EVOLUTION OF YOUNG STELLAR OBJECTS
A model of protostar mass and luminosity evolution in clusters gives new estimates of cluster age, protostar birthrate, accretion rate, and mean accretion time. The model assumes constant protostar
A CHANDRA STUDY OF THE ROSETTE STAR-FORMING COMPLEX. III. THE NGC 2237 CLUSTER AND THE REGION'S STAR FORMATION HISTORY
We present high spatial resolution Chandra X-ray images of the NGC 2237 young stellar cluster on the periphery of the Rosette Nebula. We detect 168 X-ray sources, 80% of which have stellar
A Chandra Study of the Rosette Star-forming Complex. I. The Stellar Population and Structure of the Young Open Cluster NGC 2244
We present the first high spatial resolution X-ray study of NGC 2244, the 2 Myr old stellar cluster in the Rosette Nebula, using Chandra. Over 900 X-ray sources are detected; 77% have optical or
Quantitative evidence of an intrinsic luminosity spread in the Orion nebula cluster
Aims. We study the distribution of stellar ages in the Orion nebula cluster (ONC) using accurate HST photometry taken from HST Treasury Program observations of the ONC utilizing the cluster distance
STAR FORMATION IN SPACE AND TIME: THE ORION NEBULA CLUSTER
We examine the pattern of star birth in the Orion Nebula cluster (ONC), with the goal of discerning the cluster's formation mechanism. Outside the Trapezium, the distribution of stellar masses is
The sequence of low- and high-mass star formation in the young stellar cluster IRAS 19343+2026
BVRIJHK photometry, Spitzer-GLIMPSE photometry and HK-band spectroscopy were used to study the stellar content of IRAS 19343+2026, a (proto)star/cluster candidate, located close to the Galactic
Overview of the Massive Young Star-Forming Complex Study in Infrared and X-ray (MYStIX) Project
The Massive Young Star-Forming Complex Study in Infrared and X-ray (MYStIX) seeks to characterize 20 OB-dominated young clusters and their environs at distances d ⩽ 4 kpc using imaging detectors on
The Elephant Trunk Nebula and the Trumpler 37 cluster: contribution of triggered star formation to the total population of an HII region
Rich young stellar clusters produce Hii regions whose expansion into the nearby molecular cloud is thought to trigger the formation of new stars. However, the importance of this mode of star
Star formation in bright-rimmed clouds and clusters associated with the W5 E H II region
The aim of this paper is to present the results of photometric investigations of the central cluster of the W5 E H II region as well as a follow-up study of the triggered star formation in and around
...
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