The environments of young stars - Mid-infrared and molecular line imaging

Keto, Eric; Proctor, Deanne D.; Ball, Roger; Arens, J. F.; Jernigan, G.

doi:10.1086/186684

Cited by 22 publications

(51 citation statements)

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“…This can best be seen in Figure 13, which shows the Gemini 10.5 lm image overlaid with the 12.5 lm image of Keto et al (1992). Figure 14 shows the NH 3 image of Keto et al (1992) overlaid on the 18.1 lm image from (2000) is also marked with a cross. Like G11.94À0.62, the cometary UC H ii region, C, in this field does not appear to have a cometary shape in the mid-infrared.…”

Section: G3426+015mentioning

confidence: 90%

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A Search for Mid‐Infrared Emission from Hot Molecular Core Candidates

Buizer

Radomski

Telesco

et al. 2003

ApJ

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We present here mid-infrared images of seven sites of water maser emission thought to be associated with the hot molecular core (HMC) phase of massive star formation. We have detected mid-infrared emission from the locations of two of these HMC candidates, G11.94À0.62 and G45.07þ0.13. From our observations we derived lower limit estimates of the luminosities for the exciting sources in these two HMC candidates. We find that the estimates are consistent with the hypothesis that the HMCs are internally heated by massive B-and O-type stars. We observed two sites with HMCs previously claimed to be detected in the mid-infrared, G19.61À0.23 and G34.26+0.15; however, we did not detect mid-infrared emission from either HMC location. We place new upper limits on the mid-infrared flux densities for these HMCs that are much lower than their previously reported flux densities. We were also able to obtain extremely accurate astrometry for our mid-infrared observations of G9.62+0.19 and conclude that the mid-infrared emission previously thought to be coming from the HMC in this field is in fact coming from a different source altogether.

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Section: G3426+015mentioning

confidence: 90%

“…10). In front of the cometary arc of C, there is a confirmed HMC that is seen in several molecular species (e.g., Keto et al 1992;Churchwell et al 1992).…”

Section: G3426+015mentioning

confidence: 96%

A Search for Mid‐Infrared Emission from Hot Molecular Core Candidates

Buizer

Radomski

Telesco

et al. 2003

ApJ

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“…More recent observations indicate two additional weak sources near C and E (De Buizer 2001;De Buizer et al 2003). Keto et al (1992) observed a 70 mJy source at 12.5 m at the hot molecular core, below the detection limit of Campbell et al (2000). De Buizer et al (2003) set an upper limit of 21 mJy at 18 m for this source.…”

Section: Introductionmentioning

confidence: 79%

“…VLA observations of NH 3 by Heaton, Little, & Bishop (1989) and Garay & Rodríguez (1990), together with previous observations, indicate a hierarchy of structures: a cool envelope with T rot $ 18 K that surrounds the UC H ii regions, an apparent disk of warmer, denser gas 2 00 east of component C, appearing as an elongated structure inclined $55 west of north, and a hot molecular core in its center, due east of component C, with n H 2 ' 4 7 ð ÞÂ10 7 cm À3 and T rot $ 200 K. They described this hot molecular core, shown in Figure 1, as ''ultracompact.'' The NH 3 emission was also mapped by Keto et al (1992), who show a map of the disk and ultracompact molecular core overlaid on the radio continuum emission. Heaton et al (1989) and Gómez et al (2000) (who have reprocessed the data of Garay & Rodríguez 1990) show maps of NH 3 emission wrapping around component C. Carral, Welch, & Wright (1987) and Carral & Welch (1992) mapped other molecular tracers of high density with the BIMA-Hat Creek millimeter array and show similar maps of HCO + wrapping around component C. There is a consensus among these authors that the densest parts of the hot molecular core lie to the east and behind the UC H ii regions and that the cometary shape is due to a champagne outflow to the west; other authors have interpreted the cometary appearance differently, however.…”

Section: Introductionmentioning

confidence: 99%

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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“…1. SC 10 11.7 µm image of W3(OH) with contours of the 11.7 µm (grey) emission and of the 3.6 cm radio continuum (black, from [19] and rotation temperatures in the range of 160-200 K. The detection of the HC at mid-infrared (MIR) wavelengths was claimed by [8]. Fig.…”

Section: Observations and Data Reductionmentioning

confidence: 93%

Infrared Observation of Hot Cores

Stecklum

Brandl

Feldt

et al.

The Origin of Stars and Planets: The VLT View

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Abstract. We report on mid-infrared imaging of hot cores performed with SpectroCam-10 and TIMMI2. The observations aimed at the detection of thermal emission presumably associated with the hot cores. Mid-infrared flux measurements are required to improve the luminosity and optical depth estimates for these sources. Results are presented for W3(H2O), G9.62+0.19, G10.47+0.03, and the possible hot core candidate G232.620+0.996. They illustrate that the morphology of these sources cannot be described by simple geometries. Therefore, line-of-sight effects and considerable extinction even at mid-infrared wavelengths must not be neglected.

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The environments of young stars - Mid-infrared and molecular line imaging

Cited by 22 publications

References 0 publications

A Search for Mid‐Infrared Emission from Hot Molecular Core Candidates

A Search for Mid‐Infrared Emission from Hot Molecular Core Candidates

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

Infrared Observation of Hot Cores

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