Spatial Distribution of Embedded Clusters in the Rosette Molecular Cloud: Implications for Cluster Formation

Phelps, Randy L.; Lada, Elizabeth A.

doi:10.1086/303713

Cited by 81 publications

(136 citation statements)

References 18 publications

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“…Table 3 of RZL. The nine embedded clusters identified by Phelps & Lada (1998;PL) and Román-Zúñiga et al (2008b;REFL) in the Herschel field are also labelled.…”

Section: Discussionmentioning

confidence: 99%

“…The structure of material within the RMC has been previously examined by Williams et al (1995), Schneider et al (1998) and Dent et al (2009) using various CO observations. Alternatively, the populations of young stellar objects (YSOs) within the RMC have been studied by Phelps & Lada (1998), Li & Smith (2005), Poulton et al (2008), andRomán-Zúñiga et al (2008b) using infrared observations. Notably, these studies identified 10 embedded clusters within the RMC, i.e., PL01-07 and REFL08-10.…”

Section: Introductionmentioning

confidence: 99%

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Small-scale structure in the Rosette molecular cloud revealed by Herschel

Francesco

Sadavoy

Motte

et al. 2010

A&A

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We present a preliminary analysis of the small-scale structure found in new 70−520 μm continuum maps of the Rosette molecular cloud (RMC), obtained with the SPIRE and PACS instruments of the Herschel Space Observatory. We find 473 clumps within the RMC using a new structure identification algorithm, with sizes up to ∼1.0 pc in diameter. A comparison with recent Spitzer maps reveals that 371 clumps are "starless" (without an associated young stellar object), while 102 are "protostellar." Using the respective values of dust temperature, we determine the clumps have masses (M C ) over the range −0.75 ≤ log (M C /M ) ≤ 2.50. Linear fits to the high-mass tails of the resulting clump mass spectra (CMS) have slopes that are consistent with those found for high-mass clumps identified in CO emission by other groups.

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“…Table 3 of RZL. The nine embedded clusters identified by Phelps & Lada (1998;PL) and Román-Zúñiga et al (2008b;REFL) in the Herschel field are also labelled.…”

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Small-scale structure in the Rosette molecular cloud revealed by Herschel

Francesco

Sadavoy

Motte

et al. 2010

A&A

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“…Both nebulae are likely to have been formed by the interaction of the central cluster(s) of OB stars (NGC 2244 in the case of the Rosette nebula). Phelps & Lada (1997) also report the detection of a number of embedded compact clusters which they suggest result from the interaction of NGC 2244 with the host molecular cloud. Embedded cluster are also found in the environs of the young open clusters IC 1396 and IC 1805 (Clarke et al 2000 and references therein), although the hot star population inferred for the G305 complex is significantly in excess of the populations of any of these regions.…”

Section: Comparison With Other Star Forming Regionsmentioning

confidence: 89%

Triggered massive star formation in the vicinity of WR 48a

Clark

Porter

2004

A&A

114

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Abstract. We utilise Midcourse Space Experiment mid-IR imaging and published data to discuss the (massive) star formation region at galactic longitude ∼305 • , apparently associated with the Wolf Rayet WR 48a and the attendant clusters Danks 1 and 2. A spectacular three lobed wind blown bubble surrounds the aforementioned sources, for which we may infer a minimum age of ∼3 Myr from the presence of the WCL star. Near IR data reveals the presence of numerous embedded sources on the periphery of the wind blown bubble. The presence of coincindent H 2 O, OH and methanol maser emission is suggestive of ongoing massive star formation, which is suppported by the fluxes of the associated IR sources, and the requisite LyC flux required to support the emission from the subset that have associated ucH  regions. Consideration of the integrated radio flux of the complex implies that a minimum of 31 O7V stars must be present, under the assumption of no photon leakage. Given the age and morphology of the complex and in particular the observation that the central exciting clusters have entirely cleared their natal material, we expect this assumption will be violated, and hence that the true population of massive stars is likely to be significantly larger. If confirmed, the G305 complex represents one of the most massive regions of ongoing triggered star formation currently identified in the galaxy.

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“…5b) with the levels 3, 20, 25, and 40 arcmin −2 , meaning a cluster must have a star density excess greater than 3 arcmin −2 . Figure 6 shows the result with the clusters identification from Phelps & Lada (1997) and . The levels 20, 25, and 40 arcmin −2 are arbitrary chosen to split the connected clusters PL 04, PL 05, PL 06, and REFL 08 in accordance with .…”

Section: Cluster Characterizationmentioning

confidence: 99%

Young stellar clusters in the Rosette molecular cloud

Cambrésy

Márton

Fehér

et al. 2013

A&A

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Aims. We focus on characterizing the young stellar population in the Rosette complex to improve our understanding of the processes that regulate the star formation in this region. Methods. We propose an original method that relies on the joint analysis of the star color and density in the near-infrared. It leads to mapping the molecular cloud spatial distribution and detecting the embedded clusters with their characterization in terms of member number and age estimation. Results. We have identified 13 clusters, 2 of which are new discoveries, and we estimate that the total number of young stellar objects in the Rosette ranges between 4000 and 8000 members. We find that the age distribution of the young clusters is not consistent with a general triggered scenario for the star formation in this molecular cloud. Conclusions. This study proves that the Rosette complex evolution is not governed by the influence of its OB star population. It suggests that the simple morphological appearance of an active region is not sufficient to conclude much about the triggering role in the star formation process. Our method of constraining the cluster properties using UKIDSS and WISE data has proven efficient, and studies of other regions of the Galactic plane would definitely benefit from this approach.

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Spatial Distribution of Embedded Clusters in the Rosette Molecular Cloud: Implications for Cluster Formation

Cited by 81 publications

References 18 publications

Small-scale structure in the Rosette molecular cloud revealed by Herschel

Small-scale structure in the Rosette molecular cloud revealed by Herschel

Triggered massive star formation in the vicinity of WR 48a

Young stellar clusters in the Rosette molecular cloud

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