AO Assisted Near-IR Spectroscopy of SVS 13 and its Jet

Details AO Assisted Near-IR Spectroscopy of SVS 13 and its Jet AO Assisted Near-IR Spectroscopy of SVS 13 and its Jet

2005-11-15

arxiv.org/abs/astro-ph/0511427v1

Astrophys.J.639:969-974,2006

Astronomy and Astrophysics

Astrophysics

Astrophys. J accepted, 14 pages, 5 figures. See also http://www.jach.hawaii.edu/~cdavis

Scientific paper

10.1086/499557

We present long-slit H- and K-band spectroscopy of the low-mass outflow source SVS 13, obtained with the adaptive-optics assisted imager-spectrometer NACO on the VLT. With a spatial resolution of < 0.25 arcsec and a pixel scale of 0.027 arcsec we precisely establish the relative offsets of H2, [FeII], CO, HI and NaI components from the source continuum. The H2 and [FeII] peaks are clearly associated with the jet, while the CO, HI and NaI peaks are spatially unresolved and coincident with the source, as is expected for emission associated with accretion processes. The H2 profile along the slit is resolved into multiple components, which increase in size though decrease in intensity with distance from the source. This trend might be consistent with thermal expansion of packets of gas ejected during periods of increased accretion activity. Indeed, for the brightest component nearest the source, proper motion measurements indicate a tangential velocity of 0.028 arcsec/year. It therefore seems unlikely that this emission peak is associated with a stationary zone of warm gas at the base of the jet. However, the same can not be said for the [FeII] peak, for which we see no evidence for motion downwind, even though radial velocity measurements indicate that the emission is associated with higher jet velocities. We postulate that the [FeII] could be associated with a collimation shock at the base of the jet.

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