How many stars are being formed in the Orion Nebula?
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|---|---|
| We infer an age of ~4-5 Myr for NGC 1980 and estimate a cluster population of the order of 2000 stars, which makes it one of the most massive clusters in the entire Orion complex. | |
| Comparing our results with those relative to the Orion Nebula Cluster, we find that, by accounting for observational biases, the X-ray properties of NGC 1893 and the Orion ones are very similar. | |
| We confirm with high significance strong mass segregation of the five most massive stars in the Orion nebula cluster (ONC). | |
93 Citations | The system then looks exactly like a planetary nebula formed by a single star, except that it may show a more pronounced axial symmetry which reflects the fact that matter in the common envelope is ejected preferentially in the plane of the orbit. |
| The star-formation chronology we find in the Eagle Nebula does not support the hypothesis of a large-scale process triggered by OB stars in NGC 6611. | |
| Helium abundances and the N/O ratio in the outer envelope of this nebula are very high, therefore indicating that the nebula formed as the result of the evolution of an intermediate-mass star. | |
| Evidence from the Spitzer spectrum of IC 2448 supports previous claims that IC 2448 is an old nebula formed from a low-mass progenitor star. | |
| Based on their stellar parameters and kinematic properties, we identify 383 new candidate members of Orion A, most of which are diskless sources in areas of the region poorly studied by previous works. | |
100 Citations | These results establish the 30 Doradus Nebula as a prime region in which to investigate the formation and very early evolution of massive stars and multiple systems. |
| The filaments in Orion B apparently belong to a continuum which contains a few elements comparable to already studied star-forming filaments, for example in the IC 5146, Aquila or Taurus regions, as well as many lower density, gravitationally unbound structures. | |
| We present a new census of the Orion Nebula Cluster over a large field of view (≳30' × 30'), significantly increasing the known population of stellar and substellar cluster members with precisely determined properties. | |
| Finally, in our sample three disks are more massive than about 0.05 M_⊙, confirming that massive disks are present in the outer regions of the Orion nebula. | |
158 Citations | Our results suggest a lower dust depletion factor of oxygen than previous estimations for the Orion nebula. |
309 Citations | Our investigation corroborates and extends our previous results on the Orion Nebula Cluster. |
| Data indicate that the Orion Nebula is primarily a reflection nebula in the UV, so that morphology is determined by the distribution of dust with respect to the illuminating stars. | |
| We also propose that the central source enshrouded in the Orion KL/BN nebula has effective temperature and luminosity consistent with our model and is a possible candidate for such protostars growing under the high accretion rate. | |
| It is suggested that the Orion Nebula is a protrusion off the front edge of the dense molecular cloud whose central condensation is the Kleinmann-- Low nebula. | |
68 Citations | These results imply that (a) lambda4267 is produced mainly by recombination and provides a reliable method to determine the C/sup + +/ abundance, (b) the Orion nebula has a C/O ratio similar to the solar one, (c) planetary nebulae show freshly made carbon in their envelopes. |
| We suggest that the Orion A cloud is gravitationally collapsing on large scales, and is producing the Orion Nebula Cluster through the focusing effects of gravity acting within a finite cloud geometry. |
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