Different Evolutionary Stages in the Massive Star-Forming Region W3 Main Complex

Wang, Y.; Beuther, H.; Zhang, Qizhou; Bik, Arjan; Rodón, J. A.; Jiang, Zhibo; Fallscheer, Cassandra

doi:10.1088/0004-637x/754/2/87

Cited by 18 publications

(40 citation statements)

References 76 publications

(165 reference statements)

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“…More emission peaks may be present in the diffuse surroundings, which requires better sensitivity, angular resolution, and image fidelity for confirmation. The total flux density recorded by the SMA is about 2.5 Jy which is about 6% of the flux contained in the SCUBA image at 850 µm (Wang et al 2012). To derive the positions and flux densities of the emission peaks, we fitted the data with five point sources in the visibility domain (Fig.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Therefore, we do not aim to model this extended emission, but instead refer to the SCUBA 850 µm emission to trace this component. Table 1 lists the cm-wave, (sub)mm and IR sources associated with SMM1-5 (Claussen et al 1994;Wilson et al 2003;van der Tak et al 2005;Megeath et al 2005;Rodón et al 2008;Wang et al 2012). In Fig.…”

Section: Continuum Emissionmentioning

confidence: 99%

“…The detection of near-IR and X-ray emission toward W3 IRS5 (Megeath et al 2005;Hofner et al 2002) likely benefits from an outflow oriented near the line of sight. A velocity gradient in the NW-SE direction on scales of a few arcseconds is seen in SO 2 , which may indicate rotation of the common envelope of NIR1 and NIR2 (Rodón et al 2008;Wang et al 2012). At 14 resolution, many molecular species are detected toward W3 IRS5, especially sulfur-bearing molecules (Helmich et al 1994;Helmich & van Dishoeck 1997), implying active hot-core chemistry (e.g.…”

Section: Introductionmentioning

confidence: 98%

“…Multiple bipolar outflows with various orientations are reported via different tracers (e.g. Mitchell et al 1992;Ridge & Moore 2001;Gibb et al 2007;Rodón et al 2008;Wang et al 2012). Although the outflow driving sources are not determined unambiguously, the infrared pair NIR1 and NIR2 (Megeath et al 2005) are likely candidates.…”

Section: Introductionmentioning

confidence: 99%

“…Pineau des Forets et al 1993). The sulfur-bearing species SO and SO 2 peak near NIR1/NIR2, while complex organic molecules such as CH 3 CN and CH 3 OH peak at offset positions (Rodón et al 2008;Wang et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Dense molecular cocoons in the massive protocluster W3 IRS5: a test case for models of massive star formation

Wang

Bourke

Hogerheijde

et al. 2013

A&A

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Context. Two competing models describe the formation of massive stars in objects like the Orion Trapezium. In the turbulent core accretion model, the resulting stellar masses are directly related to the mass distribution of the cloud condensations. In the competitive accretion model, the gravitational potential of the protocluster captures gas from the surrounding cloud for which the individual cluster members compete. Aims. With high resolution submillimeter observations of the structure, kinematics, and chemistry of the proto-Trapezium cluster W3 IRS5, we aim to determine which mode of star formation dominates. Methods. We present 354 GHz Submillimeter Array observations at resolutions of 1 -3 (1800-5400 AU) of W3 IRS5. The dust continuum traces the compact source structure and masses of the individual cores, while molecular lines of CS, SO, SO 2 , HCN, H 2 CS, HNCO, and CH 3 OH (and isotopologues) reveal the gas kinematics, density, and temperature. Results. The observations show five emission peaks (SMM1-5). SMM1 and SMM2 contain massive embedded stars (∼20 M ); SMM3-5 are starless or contain low-mass stars (<8 M ). The inferred densities are high, ≥10 7 cm −3 , but the core masses are small, 0.2−0.6 M . The detected molecular emission reveals four different chemical zones. Abundant (X ∼ few 10 −7 to 10 −6 ) SO and SO 2 are associated with SMM1 and SMM2, indicating active sulfur chemistry. A low abundance (5 × 10 −8 ) of CH 3 OH concentrated on SMM3/4 suggest the presence of a hot core that is only just turning on, possibly by external feedback from SMM1/2. The gas kinematics are complex with contributions from a near pole-on outflow traced by CS, SO, and HCN; rotation in SO 2 , and a jet in vibrationally excited HCN. Conclusions. The proto-Trapezium cluster W3 IRS5 is an ideal test case to discriminate between models of massive star formation. Either the massive stars accrete locally from their local cores; in this case the small core masses imply that W3 IRS5 is at the very end stages (1000 yr) of infall and accretion, or the stars are accreting from the global collapse of a massive, cluster forming core. We find that the observed masses, densities and line widths observed toward W3 IRS 5 and the surrounding cluster forming core are consistent with the competitive accretion of gas at rates ofṀ ∼10 −4 M yr −1 by the massive young forming stars. Future mapping of the gas kinematics from large to small scales will determine whether large-scale gas inflow occurs and how the cluster members compete to accrete this material.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Continuum Emissionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Dense molecular cocoons in the massive protocluster W3 IRS5: a test case for models of massive star formation

Wang

Bourke

Hogerheijde

et al. 2013

A&A

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Age Spread in Galactic Star Forming Region W3 Main

Bik

Henning

Stolte

et al. 2014

The Labyrinth of Star Formation

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Formation of Very Young Massive Clusters and Implications for Globular Clusters

Banerjee¹,

Kroupa²

2017

The Birth of Star Clusters

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How Very Young Massive star Clusters (VYMCs; also known as "starburst" clusters), which typically are of 10 4 M and are a few Myr old, form out of Giant Molecular Clouds is still largely an open question. Increasingly detailed observations of young star clusters and star-forming molecular clouds and computational studies provide clues about their formation scenarios and the underlying physical processes involved. This chapter is focused on reviewing the decadelong studies that attempt to computationally reproduce the well-observed nearby VYMCs, such as the Orion Nebula Cluster, R136 and NGC 3603 young cluster, thereby shedding light on birth conditions of massive star clusters, in general. On this regard, focus is given on direct N-body modeling of real-sized massive star clusters, with a monolithic structure and undergoing residual gas expulsion, which have consistently reproduced the observed characteristics of several VYMCs and also of young star clusters, in general. The connection of these relatively simplified model calculations with the structural richness of dense molecular clouds and the complexity of hydrodynamic calculations of star cluster formation is presented in detail. Furthermore, the connections of such VYMCs with globular clusters, which are nearly as old as our Universe, is discussed. The chapter is concluded by addressing long-term deeply gas-embedded (at least apparently) and substructured systems like W3 Main. While most of the results are quoted from existing and up-to-date literature, in an integrated fashion, several new insights and discussions are provided.

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Different Evolutionary Stages in the Massive Star-Forming Region W3 Main Complex

Cited by 18 publications

References 76 publications

Dense molecular cocoons in the massive protocluster W3 IRS5: a test case for models of massive star formation

Dense molecular cocoons in the massive protocluster W3 IRS5: a test case for models of massive star formation

Age Spread in Galactic Star Forming Region W3 Main

Formation of Very Young Massive Clusters and Implications for Globular Clusters

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