On the kinematics of massive star forming regions: the case of IRAS 17233–3606

Leurini, S.; Codella, C.; Zapata, Luis A.; Beltrán, M. T.; Schilke, P.; Cesaroni, R.

doi:10.1051/0004-6361/201016190

Cited by 32 publications

(55 citation statements)

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“…The peak flux is ∼2.10 ± 0.04 Jy beam −1 , the integrated flux 6.69 Jy. The results agree very well with the continuum data at 230 GHz presented by Leurini et al (2011a). Figure 2 shows the emission of the SiO(5−4) line observed with the SMA and integrated over three different velocity ranges: the ambient velocity and the blue-and red-shifted velocities, which include emission at low (LV) and high velocities (HV).…”

Section: Sma Datasupporting

confidence: 79%

“…The prominent far-IR source IRAS 17233−3606 is one of the best laboratories for studing massive star formation because of its close distance (1 kpc, Leurini et al 2011a), high luminosity (∼1.7 × 10 4 L ), and relatively simple geometry. In a previous study in CO with the SMA (Leurini et al 2009, hereafter Paper I), we resolved multiple outflows with high collimation factors, extremely high velocity (EHV) emission (| − LSR | up to 200 km s −1 ), and flow parameters typical of massive YSOs.…”

Section: Introductionmentioning

confidence: 99%

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Evidence of a SiO collimated outflow from a massive YSO in IRAS 17233–3606

Leurini

Codella

Gusdorf

et al. 2013

A&A

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Studies of molecular outflows in high-mass young stellar objects reveal important information about the formation process of massive stars. We therefore selected the close-by IRAS 17233-3606 massive star-forming region to perform SiO observations with the SMA interferometer in the (5−4) line and with the APEX single-dish telescope in the (5−4) and (8-7) transitions. In this paper, we present a study of one of the outflows in the region, OF1, which shows several properties similar to jets driven by low-mass protostars, such as HH211 and HH212. It is compact and collimated, and associated with extremely high velocity CO emission, and SiO emission at high velocities. We used a state-of-the-art shock model to constrain the pre-shock density and shock velocity of OF1. The model also allowed us to self-consistently estimate the mass of the OF1 outflow. The shock parameters inferred by the SiO modelling are comparable with those found for low-mass protostars, only with higher pre-shock density values, yielding an outflow mass in agreement with those obtained for molecular outflows driven by early B-type young stellar objects. Our study shows that it is possible to model the SiO emission in high-mass star-forming regions in the same way as for shocks from low-mass young stellar objects.

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Section: Sma Datasupporting

confidence: 79%

Section: Introductionmentioning

confidence: 99%

Evidence of a SiO collimated outflow from a massive YSO in IRAS 17233–3606

Leurini

Codella

Gusdorf

et al. 2013

A&A

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“…dark clouds (TMC-1; Brown 1981), low-mass protostellar cores (IRAS 16293-2422;van Dishoeck et al 1995), hot cores/UC H ii regions (e.g. G34.3+0.15; MacDonald et al 1996), translucent clouds (Turner et al 1999), and outflows emanating from massive YSOs (IRAS 17233-3606; Leurini et al 2011). Zinchenko et al (2000 searched for HNCO emission towards a sample of 81 dense molecular cloud cores, and detected it in 57 (70%) of them.…”

Section: Hnco (Isocyanic Acid)mentioning

confidence: 99%

A MALT90 study of the chemical properties of massive clumps and filaments of infrared dark clouds

Miettinen

2014

A&A

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Context. Infrared dark clouds (IRDCs) provide a useful testbed in which to investigate the genuine initial conditions and early stages of massive-star formation. Aims. We attempt to characterise the chemical properties of a sample of 35 massive clumps of IRDCs through multi-molecular line observations. We also search for possible evolutionary trends among the derived chemical parameters.Methods. The clumps are studied using the MALT90 (Millimetre Astronomy Legacy Team 90 GHz) line survey data obtained with the Mopra 22 m telescope. The survey covers 16 different transitions near 90 GHz. The spectral-line data are used in concert with our previous LABOCA (Large APEX BOlometer CAmera) 870 μm dust emission data. Results. Eleven MALT90 transitions are detected towards the clumps at least at the 3σ level. Most of the detected species (SiO, C 2 H, HNCO, HCN, HCO + , HNC, HC 3 N, and N 2 H + ) show spatially extended emission towards many of the sources. Most of the fractional abundances of the molecules with respect to H 2 are found to be comparable to those determined in other recent similar studies of IRDC clumps. We found that the abundances of SiO, HNCO, and HCO + are higher in IR-bright clumps than in IR-dark sources, reflecting a possible evolutionary trend. A hint of this trend is also seen for HNC and HC 3 N. An opposite trend is seen for the C 2 H and N 2 H + abundances. Moreover, a positive correlation is found between the abundances of HCO + and HNC, and between those of HNC and HCN. The HCN and HNC abundances also appear to increase as a function of the N 2 H + abundance. The HNC/HCN and N 2 H + /HNC abundance ratios are derived to be near unity on average, while that of HC 3 N/HCN is ∼10%. The N 2 H + /HNC ratio appears to increase as the clump evolves, while the HNC/HCO + ratio shows the opposite behaviour. Conclusions. The detected SiO emission is probably caused by shocks driven by outflows in most cases, although shocks resulting from the cloud formation process could also play a role. Shock-origin for the HNCO, HC 3 N, and CH 3 CN emission is also plausible. The average HNC/HCN ratio is in good agreement with those seen in other IRDCs, but gas temperature measurements would be neeeded to study its temperature dependence. Our results support the finding that C 2 H can trace the cold gas, and not just the photodissociation regions. The HC 3 N/HCN ratio appears to be comparable to the values seen in other types of objects, such as T Tauri disks and comets.

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“…Hence, a temperature correction is neces- Sanna et al (2014) (g) Moisés et al (2011) ( †) We revised the spectrophotometric distance of 1.81 kpc by Moisés et al (2011). (h) Wu et al (2014) (i) Wu et al (2012) (j) Reid et al (2014) (k) Dutra et al (2003) (l) Straw et al (1987) (m) Xu et al (2011) (n) Sanna et al (2009) (o) Leurini et al (2011) (p) Kurayama et al (2011) (q) Russeil (2003) (r) Motogi et al (2011) (s) López et al (2011) ( ‡) Peretto et al (2013) adopts 3.25 kpc.…”

Section: Temperature Estimatesmentioning

confidence: 99%

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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On the kinematics of massive star forming regions: the case of IRAS 17233–3606

Cited by 32 publications

References 50 publications

Evidence of a SiO collimated outflow from a massive YSO in IRAS 17233–3606

Evidence of a SiO collimated outflow from a massive YSO in IRAS 17233–3606

A MALT90 study of the chemical properties of massive clumps and filaments of infrared dark clouds

The ATLASGAL survey: The sample of young massive cluster progenitors

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