Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apjs..174..379f&link_type=abstract
The Astrophysical Journal Supplement Series, Volume 174, Issue 2, pp. 379-395.
Astronomy and Astrophysics
Astronomy
15
Ism: Individual: Alphanumeric: 3C 58, Ism: Kinematics And Dynamics, Ism: Supernova Remnants
Scientific paper
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.
Fesen Robert
Hurford Alan
Rudie Gwen
Soto Aljeandro
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