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Title: ALMA Images of the Orion Hot Core at 349 GHz

Abstract

We present ALMA images of the dust and molecular line emission in the Orion Hot Core at 349 GHz. At 0.″2 angular resolution the images reveal multiple clumps in an arc ∼1″ east of Orion Source I, the protostar at the center of the Kleinmann–Low Nebula, and another chain of peaks from IRc7 toward the southwest. The molecular line images show narrow filamentary structures at velocities >10 km s{sup −1} away from the heavily resolved ambient cloud velocity ∼5 km s{sup −1}. Many of these filaments trace the SiO outflow from Source I, and lie along the edges of the dust emission. Molecular line emission at excitation temperatures 300–2000 K, and velocities >10 km s{sup −1} from the ambient cloud, suggest that the Hot Core may be heated in shocks by the outflow from Source I or from the Becklin–Neugebauer (BN)/SrcI explosion. The spectral line observations also reveal a remarkable molecular ring, ∼2″ south of SrcI, with a diameter ∼600 au. The ring is seen in high-excitation transitions of HC{sub 3}N, HCN v 2 = 1, and SO{sub 2}. An impact of ejecta from the BN/SrcI explosion with a dense dust clump could result in the observed ring of shockedmore » material.« less

Authors:
;  [1]
  1. Radio Astronomy Laboratory, University of California, Berkeley, CA 94720 (United States)
Publication Date:
OSTI Identifier:
22663425
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 843; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BORON NITRIDES; CLOUDS; COSMIC DUST; EMISSION; EXCITATION; EXPLOSIONS; GHZ RANGE; HYDROCYANIC ACID; INTERSTELLAR SPACE; NEBULAE; NITRILES; PROTOSTARS; RESOLUTION; SILICON OXIDES; STARS; SULFUR DIOXIDE

Citation Formats

Wright, M. C. H., and Plambeck, R. L., E-mail: wright@astro.berkeley.edu. ALMA Images of the Orion Hot Core at 349 GHz. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA72E6.
Wright, M. C. H., & Plambeck, R. L., E-mail: wright@astro.berkeley.edu. ALMA Images of the Orion Hot Core at 349 GHz. United States. doi:10.3847/1538-4357/AA72E6.
Wright, M. C. H., and Plambeck, R. L., E-mail: wright@astro.berkeley.edu. Mon . "ALMA Images of the Orion Hot Core at 349 GHz". United States. doi:10.3847/1538-4357/AA72E6.
@article{osti_22663425,
title = {ALMA Images of the Orion Hot Core at 349 GHz},
author = {Wright, M. C. H. and Plambeck, R. L., E-mail: wright@astro.berkeley.edu},
abstractNote = {We present ALMA images of the dust and molecular line emission in the Orion Hot Core at 349 GHz. At 0.″2 angular resolution the images reveal multiple clumps in an arc ∼1″ east of Orion Source I, the protostar at the center of the Kleinmann–Low Nebula, and another chain of peaks from IRc7 toward the southwest. The molecular line images show narrow filamentary structures at velocities >10 km s{sup −1} away from the heavily resolved ambient cloud velocity ∼5 km s{sup −1}. Many of these filaments trace the SiO outflow from Source I, and lie along the edges of the dust emission. Molecular line emission at excitation temperatures 300–2000 K, and velocities >10 km s{sup −1} from the ambient cloud, suggest that the Hot Core may be heated in shocks by the outflow from Source I or from the Becklin–Neugebauer (BN)/SrcI explosion. The spectral line observations also reveal a remarkable molecular ring, ∼2″ south of SrcI, with a diameter ∼600 au. The ring is seen in high-excitation transitions of HC{sub 3}N, HCN v 2 = 1, and SO{sub 2}. An impact of ejecta from the BN/SrcI explosion with a dense dust clump could result in the observed ring of shocked material.},
doi = {10.3847/1538-4357/AA72E6},
journal = {Astrophysical Journal},
number = 2,
volume = 843,
place = {United States},
year = {Mon Jul 10 00:00:00 EDT 2017},
month = {Mon Jul 10 00:00:00 EDT 2017}
}