The star-forming content of the W3 giant molecular cloud

Moore, T. J. T.; Bretherton, D. E.; Fujiyoshi, Takuya; Ridge, Naomi A.; Allsopp, J.; Hoare, M. G.; Lumsden, S. L.; Richer, J. S.

doi:10.1111/j.1365-2966.2007.11941.x

Cited by 59 publications

(114 citation statements)

References 32 publications

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“…The CFE errors mainly arise from the mass uncertainties of the compact sources. Compared with the existing results (5 − 80%, e.g., Motte et al 1998;Moore et al 2007;Bontemps et al 2010b;Eden et al 2012;Palau et al 2013;Louvet et al 2014), the range of 11 to 76% is acceptable.…”

Section: Core Formation Efficiencymentioning

confidence: 71%

Herschelobservations of the Galactic H ii region RCW 79

Liu

Figueira

Zavagno

et al. 2017

A&A

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Context. Triggered star formation around H ii regions could be an important process. The Galactic H ii region RCW 79 is a prototypical object for triggered high-mass star formation. Aims. We aim to obtain a census of the young stellar population observed at the edges of the H ii region and to determine the properties of the young sources in order to characterize the star formation processes that take place at the edges of this ionized region. Methods. We take advantage of Herschel data from the surveys HOBYS, "Evolution of Interstellar Dust", and Hi-Gal to extract compact sources. We use the algorithm getsources. We complement the Herschel data with archival 2MASS, Spitzer, and WISE data to determine the physical parameters of the sources (e.g., envelope mass, dust temperature, and luminosity) by fitting the spectral energy distribution. Results. We created the dust temperature and column density maps along with the column density probability distribution function (PDF) for the entire RCW 79 region. We obtained a sample of 50 compact sources in this region, 96% of which are situated in the ionization-compressed layer of cold and dense gas that is characterized by the column density PDF with a double-peaked lognormal distribution. The 50 sources have sizes of ∼ 0.1 − 0.4 pc with a typical value of ∼ 0.2 pc, temperatures of ∼ 11 − 26 K, envelope masses of ∼ 6 − 760 M , densities of ∼ 0.1 − 44 × 10 5 cm −3 , and luminosities of ∼ 19 − 12712 L . The sources are classified into 16 class 0, 19 intermediate, and 15 class I objects. Their distribution follows the evolutionary tracks in the diagram of bolometric luminosity versus envelope mass (L bol − Menv) well. A mass threshold of 140 M , determined from the L bol − Menv diagram, yields 12 candidate massive dense cores that may form high-mass stars. The core formation efficiency (CFE) for the 8 massive condensations shows an increasing trend of the CFE with density. This suggests that the denser the condensation, the higher the fraction of its mass transformation into dense cores, as previously observed in other high-mass star-forming regions.

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Section: Core Formation Efficiencymentioning

confidence: 71%

Herschelobservations of the Galactic H ii region RCW 79

Liu

Figueira

Zavagno

et al. 2017

A&A

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“…However, as no bump that is due to the blending of lower mass sources with the highest mass clumps is observed in the high-mass end of the CMF (Moore et al 2007;Reid et al 2010), we can assume that clumps at large distances do not alter the CMF and that these clumps are part of the same distribution.…”

Section: Discussion Of the Cmf And Relation With Imfmentioning

confidence: 99%

Source clustering in the Hi-GAL survey determined using a minimum spanning tree method

Beuret

Billot

Cambrésy

et al. 2017

A&A

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Aims. The aims are to investigate the clustering of the far-infrared sources from the Herschel infrared Galactic Plane Survey (Hi-GAL) in the Galactic longitude range of −71 to 67 deg. These clumps, and their spatial distribution, are an imprint of the original conditions within a molecular cloud. This will produce a catalogue of over-densities. Methods. The minimum spanning tree (MST) method was used to identify the over-densities in two dimensions. The catalogue was further refined by folding in heliocentric distances, resulting in more reliable over-densities, which are cluster candidates. Results. We found 1633 over-densities with more than ten members. Of these, 496 are defined as cluster candidates because of the reliability of the distances, with a further 1137 potential cluster candidates. The spatial distributions of the cluster candidates are different in the first and fourth quadrants, with all clusters following the spiral structure of the Milky Way. The cluster candidates are fractal. The clump mass functions of the clustered and isolated are statistically indistinguishable from each other and are consistent with Kroupa's initial mass function.

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“…In this work we present high resolution SMA interferometry observations as well as single-dish CO(2 − 1) observations of three subregions (W3 SMS1, W3 SMS2 and W3 SMS3) within the same environment, W3 Main (Ladd et al 1993;Tieftrunk et al 1998;Moore et al 2007;Megeath et al 2008). We study the evolution of the chemical and physical properties (outflows, rotation), ranging from potential starless cores to the most evolved ultracompact HII (UCHII) regions.…”

Section: Introductionmentioning

confidence: 99%

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

Wang

Beuther

Zhang

et al. 2012

ApJ

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We observed three high-mass star-forming regions in the W3 high-mass star formation complex with the Submillimeter Array and IRAM 30 m telescope. These regions, i.e. W3 SMS1 (W3 IRS5), SMS2 (W3 IRS4) and SMS3, are in different evolutionary stages and are located within the same large-scale environment, which allows us to study rotation and outflows as well as chemical properties in an evolutionary sense. While we find multiple mm continuum sources toward all regions, these three sub-regions exhibit different dynamical and chemical properties, which indicates that they are in different evolutionary stages. Even within each subregion, massive cores of different ages are found, e.g. in SMS2, sub-sources from the most evolved UCHII region to potential starless cores exist within 30 000 AU of each other. Outflows and rotational structures are found in SMS1 and SMS2. Evidence for interactions between the molecular cloud and the HII regions is found in the 13 CO channel maps, which may indicate triggered star formation.

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The star-forming content of the W3 giant molecular cloud

Cited by 59 publications

References 32 publications

Herschelobservations of the Galactic H ii region RCW 79

Herschelobservations of the Galactic H ii region RCW 79

Source clustering in the Hi-GAL survey determined using a minimum spanning tree method

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

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