Dense Cores in the Orion Molecular Cloud

Wilson, Thomas L.; Mauersberger, R.; Gensheimer, P. D.; Muders, D.; Bieging, John H.

doi:10.1086/307878

Cited by 44 publications

(94 citation statements)

References 27 publications

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“…The telescope beam size was 35 at the line frequency. The SIS mixer is a double sideband system, so the line intensities were calibrated using the peak C 18 O temperature measured for Orion KL (see e.g., Wilson et al 1999 for a fuller discussion of this procedure). The SIS receiver noise temperature was ∼380 K, the spectrometers were Acoustic Optical Spectrometers and filter banks.…”

Section: Observationsmentioning

confidence: 99%

Kinetic temperatures in the Orion Bar

Batrla¹,

Wilson

2003

A&A

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Abstract. We report the detection of the (J, K) = (1, 1), (2, 2) and (4, 4) inversion lines of ammonia towards the Photo Dissociation Region (PDR) of the Orion Bar. The NH 3 emission is found in the same location as emission from HCN. Temperatures determined from line intensity ratios indicate a warm gas with T k of ∼150 K. This value is inconsistent with temperatures predicted from models of the gas phase chemistry of dense PDRs. We propose that the emission arises from ammonia released into the gas phase from the evaporation of dense clumps. From measurements of the J = 2−1 line of C 18 O, we obtain beam-averaged column densities for those positions where the (1, 1), (2, 2) and (4, 4) inversion lines were measured. The ammonia to C 18 O abundance ratio is 1.4 ± 0.5 × 10 −2 .

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Section: Observationsmentioning

confidence: 99%

Kinetic temperatures in the Orion Bar

Batrla¹,

Wilson

2003

A&A

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“…(Wilson et al 1999). Therefore, the systemic velocity of the V380 Ori NE dense core is determined to be V 0 =7.1 km s −1 .…”

Section: Comentioning

confidence: 97%

“…Considering that it does not have an internal heating source, the dust temperature could be relatively low. However, Ohashi et al (2014) derived a kinetic temperature of 17 K from the NH 3 data of Wilson et al (1999). Therefore, the assumed dust temperature of 20 K is reasonable.…”

Section: Appendix Individual Dense Coresmentioning

confidence: 98%

“…If the starless stage of dense cores can last long enough to produce large dust grains, there are interesting implications on the evolution of the cores. Such cores are likely to be in a quasistatic or marginally subcritical state, because substantially et al 1999), and (c) NH 3 (1, 1)/(2, 2) (Wilson et al 1999). Strom 11 and HH 1-2 MMS 2 are missing from these plots because there is no counterpart in the CS core catalog of Tatematsu et al (1993).…”

Section: Timescales and Dust Growth In Dense Coresmentioning

confidence: 99%

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Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer^∗

Wilson

Cooray

Nayyeri

et al. 2017

ApJ

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The V380 Ori NE bipolar outflow was imaged in the SiO and CO =  J 1 0 lines, and dense cores in L1641 were observed in the 2.0-0.89 mm continuum. The highly collimated SiO jet shows point-symmetric oscillation patterns in both position and velocity, which suggests that the jet axis is precessing and the driving source may belong to a non-coplanar binary system. By considering the position and velocity variabilities together, accurate jet parameters were derived. The protostellar system is viewed nearly edge-on, and the jet has a flow speed of ∼35 km s −1 and a precession period of ∼1600 years. The CO outflow length gives a dynamical timescale of ∼6300 years, and the protostar must be extremely young. The inferred binary separation of 6-70 au implies that this protobinary system may have been formed through the disk instability process. The continuum spectra of L1641 dense cores indicate that the emission comes from dust, and the fits with modified blackbody functions give emissivity power indices of β=0.3-2.2. The emissivity index shows a positive correlation with the molecular line width, but no strong correlation with bolometric luminosity or temperature. V380 Ori NE has a particularly low value of β=0.3, which tentatively suggests the presence of millimeter-sized dust grains. Because the dust growth takes millions of years, much longer than the protostellar age, this core may have produced large grains in the starless core stage. HH 34 MMS and HH 147 MMS also have low emissivity indices.

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“…High-mass prestellar cores are expected to have higher temperatures, of up to 50 K (e.g. Wilson et al 1999). Prestellar cores are expected to have a radial temperature gradient, with the centres colder than the edges (e.g.…”

Section: Temperaturementioning

confidence: 99%

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Pattle¹

2017

Springer Theses

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Dense Cores in the Orion Molecular Cloud

Cited by 44 publications

References 27 publications

Kinetic temperatures in the Orion Bar

Kinetic temperatures in the Orion Bar

Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer^∗

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

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Dense Cores in the Orion Molecular Cloud

Cited by 44 publications

References 27 publications

Kinetic temperatures in the Orion Bar

Kinetic temperatures in the Orion Bar

Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer∗

Submillimetre Studies of Prestellar and Starless Cores in the Ophiuchus, Taurus and Cepheus Molecular Clouds

Contact Info

Product

Resources

About

Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer^∗