Millimeter Imaging of the HH 270 Protostellar Core and Outflow

Details Millimeter Imaging of the HH 270 Protostellar Core and Outflow Millimeter Imaging of the HH 270 Protostellar Core and Outflow

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...648..504c&link_type=abstract

The Astrophysical Journal, Volume 648, Issue 1, pp. 504-509.

Astronomy and Astrophysics

Astronomy

4

Ism: Individual: Alphanumeric: Hh 270, Ism: Jets And Outflows, Stars: Formation

Scientific paper

The HH 270 region was observed in the C18O and the 13 CO J=1-->0 lines with angular resolutions ranging from 3" to 10". The dense molecular core containing the centimeter continuum source VLA 1 has a mass of ~1.6 Msolar. As the 13CO image shows that the dense core is elongated in the direction perpendicular to the outflow axis, the core may be flattened and viewed nearly edge-on. The 13CO spectrum shows a blue-skewed line profile when the imaging is done at a high resolution, suggesting that the infall motion becomes kinematically important on a small scale, within ~2000 AU from the center. The molecular outflow does not show a large line width, and the outflow axis may be close to the plane of the sky. Archival near-IR images reveal that there is a nebulosity associated with VLA 1, and that VLA 1 and HH 270 IRS are separate objects. Comparison of the near-IR and optical images with an accurate positional alignment shows that VLA 1 is the driving source of the HH 270 flow. If HH 270 IRS is not a background star, the HH 270 core may contain a binary system with inhomogeneous spectral classes: VLA 1 may be a Class 0 protostar, and HH 270 IRS may be a young stellar object with a hotter spectral energy distribution.

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