Subarcsecond submillimeter continuum observations of orion KL

H. Beuther, Q. Zhang, L. J. Greenhill, M. J. Reid, D. Wilner, E. Keto, Daniel P Marrone, P. T P Ho, J. M. Moran, R. Rao, H. Shinnaga, S. Y. Liu

Research output: Contribution to journalArticle

56 Citations (Scopus)

Abstract

We present the first 865 μm continuum image with subarcsecond resolution obtained with the Submillimeter Array. These data resolve the Orion KL region into the hot core, the nearby radio source I, the submillimeter counterpart to the infrared source n (radio source L), and new submillimeter continuum sources. The radio to submillimeter emission from source I can be modeled as either the result of proton-electron free-free emission that is optically thick to ∼100 GHz plus dust emission that accounts for the majority of the submillimeter flux, or H free-free emission that gives rise to a power-law spectrum with a power-law index of ∼1.6. The latter model would indicate similar physical conditions as found in the inner circumstellar environment of Mira variable stars. Future subarcsecond resolution observations at shorter submillimeter wavelengths should easily discriminate between these two possibilities. The submillimeter continuum emission toward source n can be interpreted in the framework of emission from an accretion disk.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume616
Issue number1 II
StatePublished - Nov 20 2004
Externally publishedYes

Fingerprint

continuums
radio
power law
Mira variables
variable stars
accretion disks
free electrons
accretion
dust
wavelength
electron
protons
wavelengths

Keywords

  • Dust
  • Extinction
  • ISM: individual (Orion Kleinmann-Low)
  • Stars: early-type stars: Formation
  • Submillimeter
  • Techniques: interferometric

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Beuther, H., Zhang, Q., Greenhill, L. J., Reid, M. J., Wilner, D., Keto, E., ... Liu, S. Y. (2004). Subarcsecond submillimeter continuum observations of orion KL. Astrophysical Journal, 616(1 II).

Subarcsecond submillimeter continuum observations of orion KL. / Beuther, H.; Zhang, Q.; Greenhill, L. J.; Reid, M. J.; Wilner, D.; Keto, E.; Marrone, Daniel P; Ho, P. T P; Moran, J. M.; Rao, R.; Shinnaga, H.; Liu, S. Y.

In: Astrophysical Journal, Vol. 616, No. 1 II, 20.11.2004.

Research output: Contribution to journalArticle

Beuther, H, Zhang, Q, Greenhill, LJ, Reid, MJ, Wilner, D, Keto, E, Marrone, DP, Ho, PTP, Moran, JM, Rao, R, Shinnaga, H & Liu, SY 2004, 'Subarcsecond submillimeter continuum observations of orion KL', Astrophysical Journal, vol. 616, no. 1 II.
Beuther H, Zhang Q, Greenhill LJ, Reid MJ, Wilner D, Keto E et al. Subarcsecond submillimeter continuum observations of orion KL. Astrophysical Journal. 2004 Nov 20;616(1 II).
Beuther, H. ; Zhang, Q. ; Greenhill, L. J. ; Reid, M. J. ; Wilner, D. ; Keto, E. ; Marrone, Daniel P ; Ho, P. T P ; Moran, J. M. ; Rao, R. ; Shinnaga, H. ; Liu, S. Y. / Subarcsecond submillimeter continuum observations of orion KL. In: Astrophysical Journal. 2004 ; Vol. 616, No. 1 II.
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AU - Marrone, Daniel P

AU - Ho, P. T P

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AB - We present the first 865 μm continuum image with subarcsecond resolution obtained with the Submillimeter Array. These data resolve the Orion KL region into the hot core, the nearby radio source I, the submillimeter counterpart to the infrared source n (radio source L), and new submillimeter continuum sources. The radio to submillimeter emission from source I can be modeled as either the result of proton-electron free-free emission that is optically thick to ∼100 GHz plus dust emission that accounts for the majority of the submillimeter flux, or H free-free emission that gives rise to a power-law spectrum with a power-law index of ∼1.6. The latter model would indicate similar physical conditions as found in the inner circumstellar environment of Mira variable stars. Future subarcsecond resolution observations at shorter submillimeter wavelengths should easily discriminate between these two possibilities. The submillimeter continuum emission toward source n can be interpreted in the framework of emission from an accretion disk.

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