G30.79 FIR 10: a gravitationally bound infalling high-mass star-forming clump

Cortés, Paulo C.; Parra, Rodrigo; Cortés, Juan R.; Hardy, Eduardo

doi:10.1051/0004-6361/200811137

Cited by 19 publications

(21 citation statements)

References 46 publications

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“…By using this value, we obtain the following molecular abundances: X( 12 CO) ∼ 3.4 × 10 −5 , X( 13 CO) ∼ 4.1 × 10 −7 , and X(HCO + ) ∼ (0.7 − 1) × 10 −10 . The obtained HCO + abundance is very similar to the values derived by Cortes et al (2010) and Cortes (2011) towards high-mass star-forming regions.…”

Section: Texsupporting

confidence: 86%

The molecular clump towards the eastern border of SNR G18.8+0.3

Paron

Ortega

Petriella

et al. 2012

A&A

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Aims. The eastern border of the SNR G18.8+0.3, close to an HII regions complex, is a very interesting region for studying the molecular gas that it is probably in contact with the supernova remnant (SNR) shock front. Methods. We observed this region using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12 CO J = 3-2, 13 CO J = 3-2, HCO + J = 4-3, and CS J = 7-6 lines with an angular resolution of 22 . To complement these observations, we analyzed infrared, submillimeter, and radio continuum archival data. Results. In this work, we clearly show that the radio continuum "protrusion" that was earlier thought to belong to the SNR is an HII region complex that is deeply embedded in a molecular clump. The new molecular observations reveal that this dense clump, belonging to an extended molecular cloud that surrounds the SNR's southeast border, is not physically in contact with SNR G18.8+0.3, suggesting that the SNR shock front has not yet reached it or that they may be located at different distances. We found some young stellar objects embedded in the molecular clump, suggesting that their formation should be approximately coeval with the SN explosion.

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Section: Texsupporting

confidence: 86%

The molecular clump towards the eastern border of SNR G18.8+0.3

Paron

Ortega

Petriella

et al. 2012

A&A

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“…A magnetic field of 20 µG × (n H 2 /10 3 cm −3 ) 0.3 is assumed for this model. These values are reasonable given what is known on the magnetic field in this region (Cortes et al 2010). Their exact choice, at this stage, is dictated by the reasonable agreement with the data on the SFR.…”

Section: Comparison To Statistical Models Of Star Formation Ratesupporting

confidence: 61%

The W43-MM1 mini-starburst ridge, a test for star formation efficiency models

Louvet¹,

Motte²,

Hennebelle³

et al. 2014

A&A

106

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Context. Star formation efficiency (SFE) theories are currently based on statistical distributions of turbulent cloud structures and a simple model of star formation from cores. They remain poorly tested, especially at the highest densities. Aims. We investigate the effects of gas density on the SFE through measurements of the core formation efficiency (CFE). With a total mass of ∼2 × 10 4 M , the W43-MM1 ridge is one of the most convincing candidate precursors of Galactic starburst clusters and thus one of the best places to investigate star formation. Methods. We used high-angular resolution maps obtained at 3 mm and 1 mm within the W43-MM1 ridge with the IRAM Plateau de Bure Interferometer to reveal a cluster of 11 massive dense cores, and, one of the most massive protostellar cores known. A Herschel column density image provided the mass distribution of the cloud gas. We then measured the "instantaneous" CFE and estimated the SFE and the star formation rate (SFR) within subregions of the W43-MM1 ridge. Results. The high SFE found in the ridge (∼6% enclosed in ∼8 pc 3 ) confirms its ability to form a starburst cluster. There is, however, a clear lack of dense cores in the eastern part of the ridge, which may be currently assembling. The CFE and the SFE are observed to increase with volume gas density, while the SFR per free fall time steeply decreases with the virial parameter, α vir . Statistical models of the SFR may describe the outskirts of the W43-MM1 ridge well, but struggle to reproduce its inner part, which corresponds to measurements at low α vir . It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models.

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“…It is expressed through the dimensionless magnetization parameter b = B/1 μG n H /1 cm 3 . We assumed a constant magnetic field strength over the shocked regions, equal to the one measured toward the W43-MM1 massive dense core: B ∼ 855 μG (Cortes et al 2010). Given the mean density of the W43-MM1 and W43-MM2 ridges listed in Table 3, we estimated n H = 2.33 × n H 2 3-6 × 10 4 cm −3 and thus, b 2.7-4.8.…”

Section: Theoretical Ability To Create Sio Molecules Through Low-velomentioning

confidence: 99%

LOW-VELOCITY SHOCKS TRACED BY EXTENDED SiO EMISSION ALONG THE W43 RIDGES: WITNESSING THE FORMATION OF YOUNG MASSIVE CLUSTERS

̃ên-Lu’o’ng¹,

Motte²,

Carlhoff³

et al. 2013

ApJ

100

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The formation of high-mass stars is tightly linked to that of their parental clouds. Here, we focus on the high-density parts of W43, a molecular cloud undergoing an efficient event of star formation. Using a column density image derived from Herschel continuum maps, we identify two high-density filamentary clouds, called the W43-MM1 and W43-MM2 ridges. Both have gas masses of 2.1 × 10 4 M and 3.5 × 10 4 M above >10 23 cm −2 and within areas of ∼6 and ∼14 pc 2 , respectively. The W43-MM1 and W43-MM2 ridges are structures that are coherent in velocity and gravitationally bound, despite their large velocity dispersion measured by the N 2 H + (1-0) lines of the W43-HERO IRAM large program. Another intriguing result is that these ridges harbor widespread (∼10 pc 2) bright SiO (2-1) emission, which we interpret to be the result of low-velocity shocks (10 km s −1). We measure a significant relationship between the SiO (2-1) luminosity and velocity extent and show that it distinguishes our observations from the high-velocity shocks associated with outflows. We use state-of-the-art shock models to demonstrate that a small percentage (10%) of Si atoms in low-velocity shocks, observed initially in gas phase or in grain mantles, can explain the observed SiO column density in the W43 ridges. The spatial and velocity overlaps between the ridges of high-density gas and the shocked SiO gas suggest that ridges could be forming via colliding flows driven by gravity and accompanied by low-velocity shocks. This mechanism may be the initial conditions for the formation of young massive clusters.

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G30.79 FIR 10: a gravitationally bound infalling high-mass star-forming clump

Cited by 19 publications

References 46 publications

The molecular clump towards the eastern border of SNR G18.8+0.3

The molecular clump towards the eastern border of SNR G18.8+0.3

The W43-MM1 mini-starburst ridge, a test for star formation efficiency models

LOW-VELOCITY SHOCKS TRACED BY EXTENDED SiO EMISSION ALONG THE W43 RIDGES: WITNESSING THE FORMATION OF YOUNG MASSIVE CLUSTERS

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