SiO in G34.26: Outflows and shocks in a high mass star   forming region

Hatchell, Jennifer; Fuller, G. A.; Millar, T. J.

doi:10.1051/0004-6361:20010468

Cited by 37 publications

(49 citation statements)

References 31 publications

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“…They show strong emission in the west region of the core (Fig. 5); this shocked region and the tracer velocity are in agreement with the results of the study of SiO in Hatchell et al (2001). Their emitting region corresponds to a cometary CH II region, which is called C in the literature (Mookerjea et al 2007).…”

Section: G34supporting

confidence: 87%

“…From radio continuum observations, this source shows two very condensed UCH II regions (called A and B), a more evolved CH II region with a cometary shape (called C) and an extended ringlike H II region (called D) (Reid & Ho 1985;Mookerjea et al 2007). There are several outflows in G34, as evidenced by SiO emission extending to the north-west, south-east and north-east of the CH II region (Hatchell, Fuller & Millar 2001).…”

Section: Sourcesmentioning

confidence: 99%

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Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Wang

Zhang

et al. 2017

Mon. Not. R. Astron. Soc.

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We present spectral line mapping observations towards four massive star-forming regionsCepheus A, DR21S, S76E and G34.26+0.15 -with the IRAM 30-m telescope at the 2 and 3 mm bands. In total, 396 spectral lines from 51 molecules, one helium recombination line, 10 hydrogen recombination lines and 16 unidentified lines were detected in these four sources. An emission line of nitrosyl cyanide (ONCN, 14 0, 14 -13 0, 13 ) was detected in G34.26+0.15, as the first detection in massive star-forming regions. We found that c-C 3 H 2 and NH 2 D show enhancement in shocked regions, as suggested by the evidence of SiO and/or SO emission. The column density and rotational temperature of CH 3 CN were estimated with the rotational diagram method for all four sources. Isotope abundance ratios of 12 C/ 13 C were derived using HC 3 N and its 13 C isotopologue, which were around 40 in all four massive star-forming regions and slightly lower than the local interstellar value (∼65). The 14 N/ 15 N and 16 O/ 18 O abundance ratios in these sources were also derived using the double isotopic method, which were slightly lower than in the local interstellar medium. Except for Cep A, the 33 S/ 34 S ratios in the other three targets were derived, which were similar to that in the local interstellar medium. The column density ratios of N(DCN)/N(HCN) and N(DCO + )/N(HCO + ) in these sources were more than two orders of magnitude higher than the elemental [D]/[H] ratio, which is 1.5 × 10 −5 . Our results show that the later stage sources, G34.26+0.15 in particular, present more molecular species than earlier stage sources. Evidence of shock activity is seen in all stages studied.

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Section: G34supporting

confidence: 87%

Section: Sourcesmentioning

confidence: 99%

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Wang

Zhang

et al. 2017

Mon. Not. R. Astron. Soc.

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“…This difference may arise due to the external influence of the nearby HII regions, or may reveal separate regions of chemical enrichment. The hot core is likely externally heated by stellar photons rather than by shocks, as SiO was not detected at the position of the hot core (Hatchell et al 2001). This source is also characterized by infall motions as suggested by observations of absorption components of NH 3 , CN, HCN and HCO + Liu et al 2013, Hajigholi et al in prep.…”

Section: Source Descriptionmentioning

confidence: 99%

Water deuterium fractionation in the high-mass star-forming region G34.26+0.15 based on Herschel/HIFI data

Coutens

Vastel

Hincelin

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Understanding water deuterium fractionation is important for constraining the mechanisms of water formation in interstellar clouds. Observations of HDO and H 18 2 O transitions were carried out towards the high-mass star-forming region G34.26+0.15 with the HIFI instrument onboard the Herschel Space Observatory, as well as with ground-based single-dish telescopes. Ten HDO lines and three H 18 2 O lines covering a broad range of upper energy levels (22-204 K) were detected. We used a non-LTE 1D analysis to determine the HDO/H 2 O ratio as a function of radius in the envelope. Models with different water abundance distributions were considered in order to reproduce the observed line profiles. The HDO/H 2 O ratio is found to be lower in the hot core (∼3.5 × 10 −4 -7.5 × 10 −4 ) than in the colder envelope (∼1.0 × 10 −3 -2.2 × 10 −3 ). This is the first time that a radial variation of the HDO/H 2 O ratio has been found to occur in a high-mass source. The chemical evolution of this source was modeled as a function of its radius and the observations are relatively well reproduced. The comparison between the chemical model and the observations leads to an age of ∼10 5 years after the infrared dark cloud stage.

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“…Our SO observations were centered on the cometary UC H ii region, component C. Hatchell et al (2001) reported a massive blueshifted outflow seen in several SiO transitions to the northwest of the UC H ii region, which is possibly driven by component B.…”

Section: G3426+015mentioning

confidence: 69%

A Survey of the SO J _K = 1 ₀ –0 ₁ Transition toward Massive Star‐forming Regions

Mateen

Höfner

Araya

2006

ASTROPHYS J SUPPL S

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We present the most extensive survey to date of the SO ground state transition J K ¼ 1 0 Y0 1 (30 GHz). We observed 49 regions of massive star formation with the Max-Planck-Institut für Radioastronomie (MPIf R) 100 m telescope. In addition, the SO J K ¼ 4 3 Y3 2 transition was observed with the IRAM 30 m telescope toward a subsample of seven sources. Emission in the SO J K ¼ 1 0 Y0 1 transition most likely arises from the parsec-scale molecular clumps surrounding ultracompact H ii regions. In general, the SO J K ¼ 1 0 Y0 1 line has a Gaussian shape and appears to be optically thin. We derive SO column densities between 0:58 ; 10 14 and 12 ; 10 14 cm À2 and SO abundances in the range 0:18 ; 10 À9 Y4:4 ; 10 À9 . Our observations show that the SO ground state transition is an effective tool to study massive star-forming clumps, and the data presented in this paper provide a useful supplement for future multitransition SO studies.

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SiO in G34.26: Outflows and shocks in a high mass star forming region

Cited by 37 publications

References 31 publications

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Water deuterium fractionation in the high-mass star-forming region G34.26+0.15 based on Herschel/HIFI data

A Survey of the SO J _K = 1 ₀ –0 ₁ Transition toward Massive Star‐forming Regions

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SiO in G34.26: Outflows and shocks in a high mass star forming region

Cited by 37 publications

References 31 publications

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Millimetre spectral line mapping observations towards four massive star-forming H ii regions

Water deuterium fractionation in the high-mass star-forming region G34.26+0.15 based on Herschel/HIFI data

A Survey of the SO J K = 1 0 –0 1 Transition toward Massive Star‐forming Regions

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A Survey of the SO J _K = 1 ₀ –0 ₁ Transition toward Massive Star‐forming Regions