Tightening the belt: Constraining the mass and evolution in SDC335

Avison, A.; Peretto, N.; Fuller, G. A.; Duarte-Cabral, A.; Traficante, A.; Pineda, Jaime E.

doi:10.1051/0004-6361/201425041

Cited by 22 publications

(39 citation statements)

References 50 publications

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“…The selected highest peak surface density clumps could therefore correspond to a phase of compactness where 4 Our mass estimates for SDC335-MM1 can be reconciled with Peretto et al (2013) with a dust emissivity index of β ∼ 1.2 between 93 GHz and 345 GHz. A similarly low value of β is also suggested by Avison et al (2015). the large level of fragmentation to form a cluster has not yet developed.…”

Section: Limited Fragmentation From Clump To Core Scalementioning

confidence: 55%

ALMA survey of massive cluster progenitors from ATLASGAL

Csengeri

Bontemps²,

Wyrowski

et al. 2017

A&A

Self Cite

108

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The early evolution of massive cluster progenitors is poorly understood. We investigate the fragmentation properties from 0.3 pc to 0.06 pc scales of a homogenous sample of infrared-quiet massive clumps within 4.5 kpc selected from the ATLASGAL survey. Using the ALMA 7 m array we detect compact dust continuum emission towards all targets and find that fragmentation, at these scales, is limited. The mass distribution of the fragments uncovers a large fraction of cores above 40 M , corresponding to massive dense cores (MDCs) with masses up to ∼400 M . Seventyseven percent of the clumps contain at most 3 MDCs per clump, and we also reveal single clumps/MDCs. The most massive cores are formed within the more massive clumps and a high concentration of mass on small scales reveals a high core formation efficiency. The mass of MDCs highly exceeds the local thermal Jeans mass, and we lack the observational evidence of a sufficiently high level of turbulence or strong enough magnetic fields to keep the most massive MDCs in equilibrium. If already collapsing, the observed fragmentation properties with a high core formation efficiency are consistent with the collapse setting in at parsec scales.

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Section: Limited Fragmentation From Clump To Core Scalementioning

confidence: 55%

ALMA survey of massive cluster progenitors from ATLASGAL

Csengeri

Bontemps²,

Wyrowski

et al. 2017

A&A

Self Cite

108

View full text Add to dashboard Cite

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“…Such weak, compact radio continuum emission has been found towards low bolometric luminosity (L bol ≤ 5 × 10 4 L ⊙ ) MYSOs (see e.g. Guzmán et al 2010; Lumsden et al 2013; Avison et al 2015). They are likely associated with shockionisation from an early outflow activity (e.g.…”

Section: Tracers Of Embedded High-mass Starsmentioning

confidence: 97%

The ATLASGAL survey: The sample of young massive cluster progenitors

Csengeri

Bontemps

Wyrowski

et al. 2017

A&A

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Context. The progenitors of high-mass stars and clusters are still challenging to recognise. Only unbiased surveys, sensitive to compact regions of high dust column density, can unambiguously reveal such a small population of particularly massive and cold clumps. Aims. Here we use the ATLASGAL survey to identify a sample of candidate progenitors of massive clusters in the inner Galaxy. Methods. We characterise a flux limited sample of compact sources selected from the ATLASGAL survey. Sensitive mid-infrared data at 21−24 µm from the WISE and MIPSGAL surveys were explored to search for embedded objects, and complementary spectroscopic data were used to investigate their stability and their star formation activity. Results. We identify an unbiased sample of infrared-quiet massive clumps in the Galaxy that potentially represent the earliest stages of massive cluster formation. An important fraction of this sample consists of sources that have not been studied in detail before. We first find that clumps hosting more evolved embedded objects and infrared-quiet clumps exhibit similar physical properties in terms of mass and size, suggesting that the sources are not only capable of forming high-mass stars, but likely also follow a single evolutionary track leading to the formation of massive clusters. The majority of the clumps are likely not in virial-equilibrium, suggesting collapse on the clump scale. Conclusions. We identify the precursors of the most massive clusters in the Galaxy within our completeness limit, and argue that these objects are undergoing large-scale collapse. This is in line with the low number of infrared-quiet massive clumps and earlier findings that star formation, in particular for high-mass objects is a fast, dynamic process. We propose a scenario in which massive clumps start to fragment and collapse before their final mass is accumulated indicating that strong self-gravity and global collapse is needed to build up rich clusters and the most massive stars.

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“…For the purpose of this study, we selected six infrared dark clouds, all part of the Peretto & Fuller (2009) catalogue. One of these, SDC335, was already examined by our team in a series of studies (Peretto et al 2013;Avison et al 2015Avison et al , 2021. These six clouds have been selected to exhibit a well-defined hub morphology seen in extinction at 8 μm, with an easily identified filament convergence point (see Section 4.2 for more details on the hub classification).…”

Section: Sample Selectionmentioning

confidence: 99%

An ALMA study of hub-filament systems – I. On the clump mass concentration within the most massive cores

Anderson

Peretto

Ragan

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The physical processes behind the transfer of mass from parsec-scale clumps to massive-star-forming cores remain elusive. We investigate the relation between the clump morphology and the mass fraction that ends up in its most massive core (MMC) as a function of infrared brightness, i.e. a clump evolutionary tracer. Using ALMA 12 m and ACA we surveyed 6 infrared-dark hubs in 2.9 mm continuum at ∼3″ resolution. To put our sample into context, we also re-analysed published ALMA data from a sample of 29 high mass-surface density ATLASGAL sources. We characterise the size, mass, morphology, and infrared brightness of the clumps using Herschel and Spitzer data. Within the 6 newly observed hubs, we identify 67 cores, and find that the MMCs have masses between 15–911 M⊙ within a radius of 0.018–0.156 pc. The MMC of each hub contains 3–24 per cent of the clump mass (fMMC), becoming 5–36 per cent once core masses are normalised to the median core radius. Across the 35 clumps, we find no significant difference in the median fMMC values of hub and non-hub systems, likely the consequence of a sample bias. However, we find that fMMC is ∼7.9 times larger for infrared-dark clumps compared to infrared-bright ones. This factor increases up to ∼14.5 when comparing our sample of 6 infrared-dark hubs to infrared-bright clumps. We speculate that hub-filament systems efficiently concentrate mass within their MMC early on during its evolution. As clumps evolve, they grow in mass, but such growth does not lead to the formation of more massive MMCs.

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Tightening the belt: Constraining the mass and evolution in SDC335

Cited by 22 publications

References 50 publications

ALMA survey of massive cluster progenitors from ATLASGAL

ALMA survey of massive cluster progenitors from ATLASGAL

The ATLASGAL survey: The sample of young massive cluster progenitors

An ALMA study of hub-filament systems – I. On the clump mass concentration within the most massive cores

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