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Title:
Hubble Space Telescope WFPC2 Imaging of Cassiopeia A
Authors:
Fesen, Robert A.; Morse, Jon A.; Chevalier, Roger A.; Borkowski, Kazimierz J.; Gerardy, Christopher L.; Lawrence, Stephen S.; van den Bergh, Sidney
Affiliation:
AA(; Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College, Hanover, NH 03755.), AB(; Center for Astrophysics and Space Astronomy, University of Colorado, Campus Box 389, Boulder, CO 80309.), AC(; Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903.), AD(; Department of Physics, North Carolina State University, Raleigh, NC 27695.), AE(; Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College, Hanover, NH 03755.), AF(; Department of Physics and Astronomy, Hofstra University, Hempstead, NY 11549.), AG(; Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada.)
Publication:
The Astronomical Journal, Volume 122, Issue 5, pp. 2644-2661. (AJ Homepage)
Publication Date:
11/2001
Origin:
UCP
AJ Keywords:
ISM: Abundances, ISM: Individual: Name: Cassiopeia A, ISM: Kinematics and Dynamics, ISM: Supernova Remnants
DOI:
10.1086/323539
Bibliographic Code:
2001AJ....122.2644F

Abstract

The young galactic supernova remnant Cassiopeia A was imaged with Wide Field Planetary Camera 2 (WFPC2) aboard the Hubble Space Telescope through filters selected to capture the complete velocity range of the remnant's main shell in several emission lines. The primary lines detected, along with the specific WFPC2 filters used, were [O III] λλ4959, 5007 (F450W), [N II] λ6583 (F658N), [S II] λλ6716, 6731+[O II] λλ7319, 7330+[O I] λλ6300, 6364 (F675W), and [S III] λλ9069, 9532 (F850LP). About three-quarters of the remnant's 4' diameter main shell was imaged with all four filters in three WFPC2 pointings, with most remaining shell regions imaged in just the F675W filter via three additional pointings. Considerable detail is observed in the reverse-shocked ejecta with typical knot scale lengths of 0.2"-0.4" (1-2×1016 cm). Both bright and faint emission features appear highly clumped with little in the way of a smooth, diffuse emission component detected. Strong differences in [S III] and [O III] line intensities, indicating chemical abundance differences, are also seen, particularly in knots located along the bright northern limb and near the base of the northeastern jet. A line of curved overlapping filaments in the remnant's northwestern rim appears to mark the location of the remnant's reverse shock front in this region. The morphology of some finger-like ejecta structures elsewhere suggest cases in which the reverse shock front is encountering the remnant's clumped ejecta. Large velocity shears (~=1000 km s-1), possibly associated with the formation of these Rayleigh-Taylor-like features, are found in the line profiles of several emission lines (e.g., [S III] λλ9069, 9532 and [Cl II] λ8679) in ground-based, optical spectra of knots near the remnant's center. The [N II] images of the remnant's circumstellar knots (QSFs) reveal them to be 0.1"-0.6" thick knots and filaments, often with diffuse edges facing away from the center of expansion. Three-color composite images of the whole remnant and certain sections, along with individual filter enlargements of selected regions of the bright optical shell, are presented and discussed. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS 5-26555.
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