Observations of Orion Source I Disk and Outflow Interface

Abstract

We imaged the continuum and molecular line emission from Orion Source I (SrcI) with up to 30 mas (12 AU) resolution at 43, 99, 223, and 340 GHz in an attempt to probe the structure and chemistry of the circumstellar disk and bipolar outflow associated with this high mass protostar. The continuum spectral index ranges from $\sim$2 along the midplane of the disk to $\sim$3 along the edges, consistent with dust that is optically thick in the midplane but becomes optically thin at the periphery. Salt (NaCl) emission is visible where the dust is optically thin; it provides a unique tracer of the velocity field within the disk. All other molecules that we have mapped - H${}_2$O, AlO, SiO, SiS, SO, and SO${}_2$ - appear to originate primarily in the bipolar outflow. The base of the outflow is corotating with the disk. SiS shows a filamentary structure that is most prominent along the edges of the outflow. The molecular distributions suggest that Si and Al released from dust grains in the disk react with oxygen derived from H${}_2$O to form SiO and AlO, and with SO and SO${}_2$ to form SiS.

Accepted in the Astrophysical Journal. 18 pages, 17 figures

References in corpus (11)

• The distance to the Orion Nebula
• Disk-Driven Rotating Bipolar Outflow in Orion Source I
• Monitoring the Large Proper Motions of Radio Sources in the Orion BN/KL Region
• The ALMA View of the OMC1 Explosion in Orion
• Imaging the Ionized Disk of the High-Mass Protostar Orion-I
• ALMA Observations of Orion Source I at 350 and 660 GHz
• Orion Source I's disk is salty
• OH maser disc and outflow in the Orion-BN/KL region
• ALMA Images of the Orion Hot Core at 349 GHz
• VLBA imaging of the 3mm SiO maser emission in the disk-wind from the massive protostellar system Orion Source I
• Extremely high excitation SiO lines in disk-outflow system in Orion Source I

Cited by in corpus (1)

• Salt, Hot Water, and Silicon Compounds Tracing Massive Twin Disks