Emission Lines in the 1 Micron Spectrum of the Class I source SVS13

Details Emission Lines in the 1 Micron Spectrum of the Class I source SVS13 Emission Lines in the 1 Micron Spectrum of the Class I source SVS13

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6226h&link_type=abstract

American Astronomical Society, AAS Meeting #211, #62.26; Bulletin of the American Astronomical Society, Vol. 39, p.852

Astronomy and Astrophysics

Astronomy

Scientific paper

The Class I source SVS 13 in NGC1333 is the driving source for HH7-11 and a powerful molecular outflow, indicating it is in a state of vigorous disk accretion. High resolution near infrared spectra acquired with NIRSPEC (R=25000) in the wavelength range 0.95-1.12 micron show numerous emission lines arising from both accretion and outflow activity. The absence of photospheric features in this wavelength regime seems not to arise from a veiling continuum that overwhelms the photosphere but rather from emission in lines normally seen in absorption in a late type star. Emission lines fall into several categories: (1) broad, blueshifted double peaked forbidden lines of [S II] and N [I] from the inner jet; (2) broad emission from 3 H Paschen lines likely from a combination of the inner wind and the magnetospheric accretion flow; (3) broad blueshifted absorption at He I 10830 from the inner wind; and (4) metallic emission lines displaying a range of line widths and including 15 multiplets from Ti I, Si I, C I, Ca I, Sr II, Fe I, Fe II. The metallic lines are remarkably similar to those seen in absorption in the photosphere of a K2 WTTS.

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