Is the Emerging Massive Cluster NGC 2244 a Twin Cluster?

Li, Jin Zeng

doi:10.1086/429399

Cited by 28 publications

(67 citation statements)

References 23 publications

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“…= +4°54′51″, where there is a concentration of Class II objects found by Balog et al (2007) with IRAC observations. This position is in good agreement with the center found in X-ray (Wang et al 2008) and 2MASS JHK S bands (Li 2005). The distance cutoff at 9′ is consistent with the radial profile of the cluster (Li 2005).…”

Section: Appendix B Membership Identification For Ngc 2244supporting

confidence: 87%

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The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation

Meng

Rieke

et al. 2017

ApJ

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We characterize the first 40 Myr of evolution of circumstellar disks through a unified study of the infrared properties of members of young clusters and associations with ages from 2 Myr up to ∼40 Myr: NGC 1333, NGC 1960, NGC 2232, NGC 2244, NGC 2362, NGC 2547, IC 348, IC 2395, Chamaeleon I, Orion OB1a and OB1b, Taurus, the β Pictoris Moving Group, ρ Ophiuchi, and the associations of Argus, Carina, Columba, Scorpius-Centaurus, and Tucana-Horologium. Our work features: (1) a filtering technique to flag noisy backgrounds; (2) a method based on the probability distribution of deflections, P(D), to obtain statistically valid photometry for faint sources; and (3) use of the evolutionary trend of transitional disks to constrain the overall behavior of bright disks. We find that the fraction of disks three or more times brighter than the stellar photospheres at 24 μm decays relatively slowly initially and then much more rapidly by ∼10 Myr. However, there is a continuing component until ∼35 Myr, probably due primarily to massive clouds of debris generated in giant impacts during the oligarchic/chaotic growth phases of terrestrial planets. If the contribution from primordial disks is excluded, the evolution of the incidence of these oligarchic/chaotic debris disks can be described empirically by a log-normal function with the peak at 12-20 Myr, including ∼13% of the original population, and with a postpeak mean duration of 10-20 Myr.

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Section: Appendix B Membership Identification For Ngc 2244supporting

confidence: 87%

“…This position is in good agreement with the center found in X-ray (Wang et al 2008) and 2MASS JHK S bands (Li 2005). The distance cutoff at 9′ is consistent with the radial profile of the cluster (Li 2005). Our final membership list in Table 4 includes 718 stars, of which 369 have IRAC detections ).…”

Section: Appendix B Membership Identification For Ngc 2244supporting

confidence: 84%

The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation

Meng

Rieke

et al. 2017

ApJ

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“…In this case (see Figure 12), one of the clusters (Hogg 12) seems to be undergoing extreme tidal distortion. A dramatic example of ongoing merger candidate is the case of the partially embedded massive young cluster NGC 2244 described by Li (2005) where two structures may be separated by just ∼7 pc. Figure 1) smaller than the cluster tidal radius are likely to merge but those born with wider separations are bound to evolve into the separated twins state.…”

Section: How Do These Results Compare With Actual Data?mentioning

confidence: 99%

The Evolution of Primordial Binary Open Star Clusters: Mergers, Shredded Secondaries, and Separated Twins

Marcos

2010

ApJ

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The properties of the candidate binary star cluster population in the Magellanic Clouds and Milky Way are similar. The fraction of candidate binaries is ∼10% and the pair separation histogram exhibits a bimodal distribution commonly attributed to their transient nature. However, if primordial pairs cannot survive for long as recognizable bound systems, how are they ending up? Here, we use simulations to confirm that merging, extreme tidal distortion, and ionization are possible depending on the initial orbital elements and mass ratio of the cluster pair. Merging is observed for initially close pairs but also for wider systems in nearly parabolic orbits. Its characteristic timescale depends on the initial orbital semi-major axis, eccentricity, and cluster pair mass ratio, becoming shorter for closer, more eccentric equal mass pairs. Shredding of the less massive cluster and subsequent separation is observed in all pairs with appreciably different masses. Wide pairs evolve into separated twins characterized by the presence of tidal bridges and separations of 200-500 pc after one Galactic orbit. Most observed binary candidates appear to be following this evolutionary path which translates into the dominant peak (25-30 pc) in the observed pair separation distribution. The secondary peak at smaller separations (10-15 pc) can be explained as due to close pairs in almost circular orbits and/or undergoing merging. Merged clusters exhibit both peculiar radial density and velocity dispersion profiles shaped by synchronization and gravogyro instabilities. Simulations and observations show that long-term binary open cluster stability is unlikely.

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“…The young open cluster NGC 2244 with an age of around 2 Myr is acknowledged to represent the oldest episode of recent cluster formation in the RMC (Li 2005). Clusters in the swept-up shells of the expanding H ii region are subsequently formed, possessing ages of >1 Myr, and are still closely associated with their birth sites (Li & Smith 2005b).…”

Section: K S Luminosity Functionmentioning

confidence: 99%

Multiseeded Multimode Formation of Embedded Clusters in the Rosette Molecular Complex: Structured Star Formation toward the Southeastern Boundary

Smith

2005

Astron J

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The Rosette Molecular Complex contains embedded clusters with diverse properties and origins. We have previously explored the shell mode of formation in the north (regions A and B) and the massive concentrations in the ridge (region C). Here we explore star formation toward the south of the complex, region D, based on data from the spatially complete Two Micron All Sky Survey. We find that stars are forming prolifically throughout this region in a highly structured mode, with both clusters and loose aggregates detected. The most prominent cluster (region D1) lies in the north-center. This cluster is over 20 pc to the south of the Monoceros Ridge, the interface of the emerging young OB cluster NGC 2244 with its ambient molecular clouds. In addition, there are several branches stemming from AFGL 961 in region C and extending to the southeastern boundary of the cloud. We invoke a tree model to interpret this pattern, corresponding to probable tracks of abrupt turbulent excitation and subsequent decay. Alternatively, we discuss gravoturbulent collapse scenarios based on numerical simulations. Relative stellar ages and gas flow directions will differentiate between these mechanisms.

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Is the Emerging Massive Cluster NGC 2244 a Twin Cluster?

Cited by 28 publications

References 23 publications

The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation

The First 40 Million Years of Circumstellar Disk Evolution: The Signature of Terrestrial Planet Formation

The Evolution of Primordial Binary Open Star Clusters: Mergers, Shredded Secondaries, and Separated Twins

Multiseeded Multimode Formation of Embedded Clusters in the Rosette Molecular Complex: Structured Star Formation toward the Southeastern Boundary

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