Narrowband Mid‐Infrared Images and Models of the H<scp>ii</scp>Complex G34.3+0.2

Campbell, M. F.; Garland, C. A.; Deutsch, L. K.; Hora, J. L.; Fazio, G. G.; Dayal, Aditya; Hoffmann, W. F.

doi:10.1086/308970

Cited by 18 publications

(53 citation statements)

References 44 publications

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“…Very deep silicate absorption is present at these sources, as had also been observed by Faison et al (1998). This feature could not be due to self-absorption in the models of Campbell et al (2000), and they attributed it to an external absorbing cloud with a ' 3:5 at 20.6 m. Hatchell et al (2001) have recently concluded that the lack of MIR emission at the UC H ii component B is due to extremely strong extinction of the source. They found it Gaume et al (1994), with radio components marked ''A,'' ''B,'' ''C,'' and ''D.''…”

Section: Introductionmentioning

confidence: 53%

“…In the analysis of our FIR observations and models, we address the relationship of the different core components and compare the mass inferred from the dust emission to the mass in the various molecular components. Campbell et al (2000) obtained narrowband MIR images of G34.3+0.2 on the Infrared Telescope Facility (IRTF) with $1 00 resolution. As has been observed by others in wider MIR bandpasses, sources of arcsecond size are associated with components C and A, but not B, and the MIR image of C does not show the cometary morphology.…”

Section: Introductionmentioning

confidence: 99%

“…There is no evidence of a photodissociation region (PDR) at the head of the cometary UC H ii region. Campbell et al (2000) made radiative transfer models of the emission due to C and A in which a small amount of dust is located in or just outside the UC H ii regions. Very deep silicate absorption is present at these sources, as had also been observed by Faison et al (1998).…”

Section: Introductionmentioning

confidence: 99%

“…The lowest contour is 3% of the peak, followed by multiples of 10% of the peak. Campbell et al (2000) observed MIR sources at A, C, D, and additional locations marked ''E'' and ''F.'' The filled circle labeled ''NH 3 Core'' is the hot molecular core described in the text.…”

Section: Introductionmentioning

confidence: 99%

“…1). E is only $2 00 south of C; Campbell et al (2000) modeled it as an embedded high-mass protostar. More recent observations indicate two additional weak sources near C and E (De Buizer 2001;De Buizer et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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High‐Resolution Far‐Infrared Observations and Models of the Star Formation Core of G34.3+0.2C

Campbell

Harvey

Lester

et al. 2004

ApJ

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High spatial resolution far-infrared (FIR) maps made on the Kuiper Airborne Observatory are presented of the extremely bright source associated with the ''cometary'' ultracompact H ii region G34.3+0.2C. The maps show sharply peaked emission at G34.3+0.2C, surrounded by extended emission of uniform temperature. Maximum entropy method deconvolutions indicate FIR core source sizes of 12 00 and 20 00 at 47 and 95 m, respectively. Radiative transfer models of centrally heated dust cloud cores are presented that match estimates of the FIR core emission at G34.3+0.2C. The FIR data and models imply that this emission is due to a compact, centrally peaked, massive core separate from the hot molecular core 2 00 east of G34.3+0.2C. In comparison to the hot molecular core, the FIR core represents a separate, more evolved core that contains a group of high-mass stars and protostars.

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Section: Introductionmentioning

confidence: 53%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

High‐Resolution Far‐Infrared Observations and Models of the Star Formation Core of G34.3+0.2C

Campbell

Harvey

Lester

et al. 2004

ApJ

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

Hatchell

Fuller²,

Millar³

2001

A&A

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Abstract.We have looked for SiO emission as evidence of shocks in the high mass star formation region G34.26+0.15. JCMT, VLA and FCRAO observations show that SiO emission is widespread across the region. The SiO emission highlights a massive, collimated outflow and other regions where stellar winds are interacting with molecular clumps. As in other star forming regions, there is also SiO at ambient velocities which is related to the outflow activity. No strong SiO abundance enhancement was measured in either the outflow or the low velocity gas, though abundances up to 10 −8 are possible if the SiO is locally enhanced in clumps and optically thick. SiO emission is not detected from the hot core itself, indicating either that SiO is not strongly enhanced in the hot core or that column densities in the region where grain mantle evaporation has taken place are low. In line of sight spiral arm clouds, we measure a SiO abundance of 0.4-2 × 10 −10 , consistent with previous estimates for quiescent clouds.

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The circumstellar environments of high-mass protostellar objects

Williams

Fuller

Sridharan

2005

A&A

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Abstract. We analyse the dust continuum emission seen towards a sample of candidate high-mass protostellar objects, modelling the cores we recently observed at 850 µm with a one-dimensional radiative transfer code. Fitting radial slices in a range of directions across sources, we identify a number of objects that have non-spherical density profiles and show that for such sources fitting the azimuthal averaged emission produces erroneous estimates of the source properties. We find the majority of cores can be successfully modelled using envelopes of power-law density structure (where ρ ∝ r −α ), finding a mean power-law index of α = 1.3 ± 0.4. These envelopes extend considerably further, are more dense, and have a more shallow density profile than those bearing low-mass protostars. The majority of best-fit models have a SED resembling the cold-component dust bodies previously proposed for the sample, implying the short wavelength emission seen towards the HMPOs either originates from a separate hot dust component(s), or involves mechanisms such as accretion disks, stochastic heating and/or optically thin cavities not included in the radiative transfer model. We find evidence of smaller dust-free cavities towards some pre-UCHII sources. The modelling indicates a correlation between α and optical depth, suggesting that the densest cores also tend to have the most strongly peaked power-law density profiles.

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Narrowband Mid‐Infrared Images and Models of the HiiComplex G34.3+0.2

Cited by 18 publications

References 44 publications

High‐Resolution Far‐Infrared Observations and Models of the Star Formation Core of G34.3+0.2C

High‐Resolution Far‐Infrared Observations and Models of the Star Formation Core of G34.3+0.2C

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

The circumstellar environments of high-mass protostellar objects

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