Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Lo, Nadia; Wiles, B.; Redman, M. P.; Cunningham, M. R.; Bains, Indra; Jones, P. A.; Burton, M. G.; Bronfman, L.

doi:10.1093/mnras/stv1880

Cited by 11 publications

(26 citation statements)

References 52 publications

(73 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The observational evidence presented by Lo et al (2015) for outflows from the three sources is robust. Outflows are ultimately powered by infall but the dynamical signature of infall is much harder to detect for several reasons.…”

Section: Observations Of G333mentioning

confidence: 77%

“…For further details of the observations, see Table 1 and references therein. For full details of the observational analyses and results, see Lo et al (2015). We will thus find a fit for the velocity structure, turbulence, and chemical abundance by restricting ourselves to models that reproduce the observed masses and temperatures.…”

Section: Observations Of G333mentioning

confidence: 99%

“…The y-axis is the intensity, T * A , in units of K and the x-axis is the v lsr velocity in km s −1 . For details of the full spectral dataset, including lines of H 13 CO + , N 2 H + , and CO isotopologues see Lo et al (2015). than the red wing; see for example Wu et al (2005) and Carolan et al (2008).…”

Section: Molecular Line Radiative Transfer Modelling Of Infallmentioning

confidence: 99%

“…Despite these complications, many physical parameters can be constrained from the observations. These data and their analysis are presented in full in Lo et al (2015). Here we reproduce the tables summarizing the major results in Table 2.…”

Section: Introductionmentioning

confidence: 99%

“…Here we reproduce the tables summarizing the major results in Table 2. We will constrain ourselves to models that are in agreement with the core and outflow properties determined by Lo et al (2015).…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

Three bright molecular line sources in G333 have recently been shown to exhibit signatures of infall. We describe a molecular line radiative transfer modelling process which is required to extract the infall signature from Mopra and Nanten2 data. The observed line profiles differ greatly between individual sources but are reproduced well by variations upon a common unified model where the outflow viewing angle is the most significant difference between the sources. The models and data together suggest that the observed properties of the high-mass star-forming regions such as infall, turbulence, and mass are consistent with scaled-up versions of the low-mass case with turbulent velocities that are supersonic and an order of magnitude larger than those found in low-mass star-forming regions. Using detailed radiative transfer modeling, we show that the G333 cores are essentially undergoing a scaled-up version of low mass star formation. This is an extension of earlier work in that the degree of infall and the chemical abundances are constrained by the RT modeling in a way that is not practical with a standard analysis of observational data. We also find high velocity infall and high infall mass rates, possibly suggesting accelerated collapse due to external pressure. Molecular depletion due to freeze-out onto dust grains in central regions of the cores is suggested by low molecular abundances of several species. Strong evidence for a local enhancement of 13 C-bearing species towards the outflow cloud cores is discussed, consistent with the presence of shocks caused by the supersonic motions within them.

show abstract

Section: Observations Of G333mentioning

confidence: 77%

Section: Observations Of G333mentioning

confidence: 99%

Section: Molecular Line Radiative Transfer Modelling Of Infallmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

show abstract

Fragmentation and filaments at the onset of star and cluster formation

Lin

Csengeri

Wyrowski

et al. 2019

A&A

View full text Add to dashboard Cite

Context. The structure formation of the dense interstellar material and the fragmentation of clumps into cores is a fundamental step to understand how stars and stellar clusters form. Aims. We aim to establish a statistical view of clump fragmentation at sub-parsec scales based on a large sample of massive clumps selected from the ATLASGAL survey. Methods. We used the APEX/SABOCA camera at 350 µm to image clumps at a resolution of 8. 5, corresponding to physical scales of <0.2 pc at a distance <5 kpc. The majority of the sample consists of massive clumps that are weak or in absorption at 24 µm. We resolve spherical and filamentary structures and identify the population of compact sources. Complemented with archival Herschel data, we derive the physical properties, such as dust temperature, mass and bolometric luminosity of clumps and cores. We use association with mid-infrared 22-24 µm and 70 µm point sources to pin down the star formation activity of the cores. We then statistically assess their physical properties, and the fragmentation characteristics of massive clumps. Results. We detect emission at 350 µm towards all targets and find that it typically exhibits a filamentary(-like) morphology and hosts a population of compact sources. Using Gaussclumps we identify 1120 compact sources and derive the physical parameters and star formation activity for 971 of these, 874 of which are associated with 444 clumps. We find a moderate correlation between the clump fragmentation levels with the clump gas density and the predicted number of fragments with pure Jeans fragmentation scenario. We find a strong correlation between the mass of the most massive fragment and the total clump mass, suggesting that the self-gravity may play an important role in the clumps' small scale structure formation. Finally, due to the improved angular resolution compared to ATLASGAL, we are able to identify 27 massive quiescent cores with M core > 100 M within 5 kpc; these are massive enough to be self-gravitating but do not yet show any sign of star-formation. This sample comprises, therefore, promising candidates of massive pre-stellar cores, or deeply embedded high-mass protostars. Conclusions. The submillimeter observations of the massive clumps that are weak or completely dark at 24 µm reveal rich filamentary structures and an embedded population of compact cores. The maximum core mass is likely determined by the self-gravity of the clump. The rarity of massive pre-stellar core candidates implies short collapse time-scales for dense structures.

show abstract

H II regions and high-mass starless clump candidates

Zhang

Zavagno

Yuan

et al. 2020

A&A

View full text Add to dashboard Cite

Context. The role of ionization feedback on high-mass (> 8 M ) star formation is still highly debated. Questions remain concerning the presence of nearby H ii regions changes the properties of early high-mass star formation and whether H ii regions promote or inhibit the formation of high-mass stars. Aims. To characterize the role of H ii regions on the formation of high-mass stars, we study the properties of a sample of candidates high-mass starless clumps (HMSCs), of which about 90% have masses larger than 100 M . These high-mass objects probably represent the earliest stages of high-mass star formation; we search if (and how) their properties are modified by the presence of an H ii region. Methods. We took advantage of the recently published catalog of HMSC candidates. By cross matching the HMSCs and H ii regions, we classified HMSCs into three categories: 1) The HMSCs associated with H ii regions both in the position in the projected plane of the sky and in velocity; 2) HMSCs associated in the plane of the sky, but not in velocity; and 3) HMSCs far away from any H ii regions in the projected sky plane. We carried out comparisons between associated and nonassociated HMSCs based on statistical analyses of multiwavelength data from infrared to radio. Results. We show that there are systematic differences of the properties of HMSCs in different environments. Statistical analyses suggest that HMSCs associated with H ii regions are warmer, more luminous, more centrally-peaked and turbulent. We also clearly show, for the first time, that the ratio of bolometric luminosity to envelope mass of HMSCs (L/M) could not be a reliable evolutionary probe for early massive star formation due to the external heating effects of the H ii regions. Conclusions. We show HMSCs associated with H ii regions present statistically significant differences from HMSCs far away from H ii regions, especially for dust temperature and L/M. More centrally peaked and turbulent properties of HMSCs associated with H ii regions may promote the formation of high-mass stars by limiting fragmentation. High-resolution interferometric surveys toward HMSCs are crucial to reveal how H ii regions impact the star formation process inside HMSCs.

show abstract

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Cited by 11 publications

References 52 publications

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Fragmentation and filaments at the onset of star and cluster formation

H II regions and high-mass starless clump candidates

Contact Info

Product

Resources

About

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Cited by 11 publications

References 52 publications

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Fragmentation and filaments at the onset of star and cluster formation

H II regions and high-mass starless clump candidates

Contact Info

Product

Resources

About

H II regions and high-mass starless clump candidates