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IRAS 16293-2422 Evidence for Infall onto a Counter-Rotating Protostellar Accretion Disk
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IRAS 16293-2422: Evidence for Infall onto a Counter-Rotating
Protostellar Accretion Disk
Anthony J. Remijan1,2 and J. M. Hollis1
ABSTRACT
We report high spatial resolution VLA observations of the low-mass star-
forming region IRAS 16293-2422 using four molecular probes: ethyl cyanide
(CH3CH2CN), methyl formate (CH3OCHO), formic acid (HCOOH), and the
ground vibrational state of silicon monoxide (SiO). Ethyl cyanide emission has
a spatial scale of ～20′′ and encompasses binary cores A and B as determined
by continuum emission peaks. Surrounded by formic acid emission, methyl for-
mate emission has a spatial scale of ～6′′and is confined to core B. SiO emission
shows two velocity components with spatial scales less than 2′′ that map ～2′′
northeast of the A and B symmetry axis. The redshifted SiO is ～2′′ northwest
of blueshifted SiO along a position angle of ～135o which is approximately par-
allel to the A and B symmetry axis. We interpret the spatial position offset in
red and blueshifted SiO emission as due to rotation of a protostellar accretion
disk and we derive ～1.4 M⊙ interior to the SiO emission. In the same vicinity,
Mundy et al. (1986) also concluded rotation of a nearly edge-on disk from OVRO
observations of much stronger and ubiquitous 13CO emission but the direction of
rotation is opposite to the SiO emission findings. Taken together, SiO and 13CO
data suggest evidence for a counter-rotating disk. Moreover, archival BIMA array
12CO data show an inverse P Cygni profile with the strongest absorption in close
proximity to the SiO emission, indicating unambiguous material infall toward
the counter-rotating protostellar disk at a new source location within the IRAS
16293-2422 complex. The details of these observations and our interpretations
are discussed.
Subject headings: ISM: abundances - ISM: clouds - ISM: individual (IRAS 16293-
2422) - ISM: molecules - radio lines: ISM
1NASA Goddard Space F
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