ALMA Images of the Orion Hot Core at 349GHz

作者：Wright M C H^*; Plambeck R L

来源：Astrophysical Journal, 2017, 843(2): 83.

DOI：10.3847/1538-4357/aa72e6

• ISM: individual objects (Orion-KL)
• radio continuum: stars
• radio lines: stars
• stars: formation
• stars: individual (Hot Core)

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 similar to 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(-1) away from the heavily resolved ambient cloud velocity similar to 5 km s(-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(-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, similar to 2 ''. south of SrcI, with a diameter similar to 600 au. The ring is seen in high-excitation transitions of HC3N, HCN v2. =. 1, and SO2. An impact of ejecta from the BN/SrcI explosion with a dense dust clump could result in the observed ring of shocked material.

• 出版日期2017-7-10