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Title:
The Optical Spectrum of the SN 1006 Supernova Remnant Revisited
Authors:
Ghavamian, Parviz; Winkler, P. Frank; Raymond, John C.; Long, Knox S.
Affiliation:
AA(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019 .), AB(Department of Physics, Middlebury College, Middlebury, VT 05753; .; Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory. CTIO is operated by AURA, Inc., under contract to the National Science Foundation.), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; .), AD(Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory. CTIO is operated by AURA, Inc., under contract to the National Science Foundation.; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; .)
Publication:
The Astrophysical Journal, Volume 572, Issue 2, pp. 888-896. (ApJ Homepage)
Publication Date:
06/2002
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: SN 1006, ISM: Kinematics and Dynamics, Shock Waves, ISM: Supernova Remnants
DOI:
10.1086/340437
Bibliographic Code:
2002ApJ...572..888G

Abstract

We present the deepest optical spectrum acquired to date of Balmer-dominated shocks in the northwest rim of SN 1006. We detect the broad and narrow components of Hα, Hβ, and Hγ and report the first detection of the He I λ6678 emission line in this supernova remnant. We may have detected, at the 1.5 σ level, faint He II λ4686 emission. We measure a full width at half-maximum of 2290+/-80 km s-1 in the broad-component Hα line, with broad-to-narrow flux ratios of 0.84+0.03-0.01 and 0.93+0.18-0.16 in Hα and Hβ, respectively. To match these observations, our nonradiative shock models require a low degree of electron-proton equilibration at the shock front, Te/Tp<=0.07, and a shock speed of 2890+/-100 km s-1 . These results agree well with an earlier analysis of ultraviolet lines from SN 1006. The He I/Hα and He I/He II flux ratios also indicate low equilibration. Furthermore, our models match the observations for mostly ionized (~90%) preshock H and mostly neutral (>~70%) preshock He, respectively. We conclude that the high H ionization fraction cannot be explained by either photoionization from the reverse shock or relic ionization from EUV photons released in the A.D. 1006 supernova. The most plausible explanation appears to be photoionization from the Galactic Lyman continuum.
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