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Title:
Optical Imaging and Spectroscopy of the Galactic Supernova Remnant 3C 58 (G130.7+3.1)
Authors:
Fesen, Robert; Rudie, Gwen; Hurford, Alan; Soto, Aljeandro
Affiliation:
AA(6127 Wilder Laboratory, Physics and Astronomy Department Dartmouth College, Hanover, NH 03755), AB(6127 Wilder Laboratory, Physics and Astronomy Department Dartmouth College, Hanover, NH 03755), AC(6127 Wilder Laboratory, Physics and Astronomy Department Dartmouth College, Hanover, NH 03755), AD(6127 Wilder Laboratory, Physics and Astronomy Department Dartmouth College, Hanover, NH 03755)
Publication:
The Astrophysical Journal Supplement Series, Volume 174, Issue 2, pp. 379-395. (ApJS Homepage)
Publication Date:
02/2008
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: 3C 58, ISM: Kinematics and Dynamics, ISM: Supernova Remnants
DOI:
10.1086/522781
Bibliographic Code:
2008ApJS..174..379F

Abstract

We present a comprehensive imaging and spectroscopic survey of optical emission knots associated with the young Galactic supernova remnant 3C 58. Hα images show hundreds of clumpy filaments and knots arranged in a complex structure covering a nearly circular area roughly 400" in diameter. A quite different emission structure is seen in [O III], where the brightest features are less clumpy and largely confined to the remnant's northwest quadrant. Measured radial velocities of over 450 knots reveal two distinct kinematic populations; one with average and peak expansion velocities of 770 and 1100 km s-1, respectively, forming a thick shell, and the other showing |v|<=250 km s-1. High-velocity knots (|v|>=500 km s-1) exhibit a strong bipolar expansion pattern with redshifted and blueshifted knots located in northeastern and southwestern regions, respectively. These knots also show strong [N II]/Hα line emission ratios, suggesting enhanced N/H. In contrast, the slower expanding knot population shows much lower [N II]/Hα line ratios and likely represents circumstellar mass loss material from the 3C 58 progenitor. Proper-motion estimates using images spanning a 28 yr time interval suggest positional shifts of between 0.5" and 2.0", implying proper motions of 0.02"-0.07" yr-1. These values agree with previous estimates but are much less than the ~0.2" yr-1 expected if 3C 58 were associated with historic guest star of 1181 CE.

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