5 research outputs found
Discovery Of A Molecular Outflow in the Haro 6-10 Star-Forming Region
We present high sensitivity 12CO and 13CO (1-0) molecular line maps covering
the full extent of the parsec scale Haro~6-10 Herbig-Haro (HH) flow. We report
the discovery of a molecular CO outflow along the axis of parsec-scale HH flow.
Previous molecular studies missed the identification of the outflow probably
due to their smaller mapping area and the confusing spectral features present
towards the object. Our detailed molecular line study of the full 1.6 pc extent
of the optical flow shows evidence for both blueshifted and redshifted gas set
in motion by Haro~6-10 activity. The molecular outflow is centered at
Haro~6-10, with redshifted gas being clumpy and directed towards the northeast,
while blueshifted gas is in the southwest direction. The molecular gas
terminates well within the cloud, short of the most distant HH objects of the
optical flow. Contamination from an unrelated cloud along the same line of
sight prevents a thorough study of the blueshifted outflow lobe and the mass
distribution at the lowest velocities in both lobes. The cloud core in which
Haro~6-10 is embedded is filamentary and flattened in the east-west direction.
The total cloud mass is calculated from 13CO(1-0) to be ~200Msun. The lower
limit of the mass associated with the outflow is ~0.25Msun.Comment: ApJ Accepted; 9 pages, 8 figures. For high resolution ps file use:
http://www.astro.umass.edu/~irena/haro.p
A Pre-Protostellar Core in L1551. II. State of Dynamical and Chemical Evolution
Both analytic and numerical radiative transfer models applied to high
spectral resolution CS and N2H+ data give insight into the evolutionary state
of L1551 MC. This recently discovered pre-protostellar core in L1551 appears to
be in the early stages of dynamical evolution. Line-of-sight infall velocities
of >0.1km/s are needed in the outer regions of L1551 MC to adequately fit the
data. This translates to an accretion rate of ~ 1e-6 Msun/yr, uncertain to
within a factor of 5 owing to unknown geometry. The observed dynamics are not
due to spherically symmetric gravitational collapse and are not consistent with
the standard model of low-mass star formation. The widespread, fairly uniform
CS line asymmetries are more consistent with planar infall. There is modest
evidence for chemical depletion in the radial profiles of CS and C18O
suggesting that L1551 MC is also chemically young. The models are not very
sensitive to chemical evolution. L1551 MC lies within a quiescent region of
L1551 and is evidence for continued star formation in this evolved cloud.Comment: 27 pages, 7 figures, ApJ accepte
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Discovery of a Molecular Outflow in the Haro 6-10 Star-forming Region
We present high sensitivity 12CO and 13CO J=1!0 molecular line maps covering the full extent of the parsec scale Haro 6-10 Herbig-Haro (HH) flow. We report the discovery of a molecular CO outflow along the axis of parsec-scale HH flow. Previous molecular studies missed the identification of the outflow probably due to their smaller mapping area and the confusing spectral features present towards the object. Our detailed molecular line study of the full 1.6 pc extent of the optical flow shows evidence for both blueshifted and redshifted gas set in motion by Haro 6-10 activity. The molecular outflow is centered at Haro 6-10, with redshifted gas being clumpy and directed towards the northeast, while blueshifted gas is in the southwest direction. The molecular gas terminates well within the cloud, short of the most distant HH objects of the optical flow. Contamination from an unrelated cloud along the same line of sight prevents a thorough study of the blueshifted outflow lobe and the mass distribution at the lowest velocities in both lobes. The cloud core in which Haro 6-10 is embedded is filamentary and flattened in the east-west direction. The total cloud mass is calculated from 13CO J=1--0 to be ~ 200 M⊙. The lower limit of the mass associated with the outflow is ~0.25 M⊙