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Title: THE 2D DISTRIBUTION OF IRON-RICH EJECTA IN THE REMNANT OF SN 1885 IN M31

Abstract

We present Hubble Space Telescope (HST) ultraviolet Fe i and Fe ii images of the remnant of Supernova 1885 (S And) which is observed in absorption against the bulge of the Andromeda galaxy, M31. We compare these Fe i and Fe ii absorption line images to previous HST absorption images of S And, of which the highest quality and theoretically cleanest is Ca ii H and K. Because the remnant is still in free expansion, these images provide a 2D look at the distribution of iron synthesized in this probable Type Ia explosion, thus providing insights and constraints for theoretical SN Ia models. The Fe i images show extended absorption offset to the east from the remnant’s center as defined by Ca ii images and is likely an ionization effect due to self-shielding. More significant is the remnant’s apparent Fe ii distribution which consists of four streams or plumes of Fe-rich material seen in absorption that extend from remnant center out to about 10,000 km s{sup −1}. This is in contrast to the remnant’s Ca ii absorption, which is concentrated in a clumpy, broken shell spanning velocities of 1000–5000 km s{sup −1} but which extends out to 12,500 km s{supmore » −1}. The observed distributions of Ca- and Fe-rich ejecta in the SN 1885 remnant are consistent with delayed detonation white dwarf models. The largely spherical symmetry of the Ca-rich layer argues against a highly anisotropic explosion as might result from a violent merger of two white dwarfs.« less

Authors:
 [1];  [2];  [3]
  1. Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Lab, Hanover, NH 03755 (United States)
  2. Department of Physics, Florida State University, Tallahassee, FL 32306 (United States)
  3. JILA and the Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States)
Publication Date:
OSTI Identifier:
22522430
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 804; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; ANISOTROPY; CALCIUM; COMPARATIVE EVALUATIONS; GALAXIES; IMAGES; IRON; LAYERS; POTASSIUM; SPACE; SPHERICAL CONFIGURATION; STREAMS; SUPERNOVA REMNANTS; SUPERNOVAE; TELESCOPES; ULTRAVIOLET RADIATION; WHITE DWARF STARS

Citation Formats

Fesen, Robert A., Höflich, Peter A., and Hamilton, Andrew J. S. THE 2D DISTRIBUTION OF IRON-RICH EJECTA IN THE REMNANT OF SN 1885 IN M31. United States: N. p., 2015. Web. doi:10.1088/0004-637X/804/2/140.
Fesen, Robert A., Höflich, Peter A., & Hamilton, Andrew J. S. THE 2D DISTRIBUTION OF IRON-RICH EJECTA IN THE REMNANT OF SN 1885 IN M31. United States. doi:10.1088/0004-637X/804/2/140.
Fesen, Robert A., Höflich, Peter A., and Hamilton, Andrew J. S. Sun . "THE 2D DISTRIBUTION OF IRON-RICH EJECTA IN THE REMNANT OF SN 1885 IN M31". United States. doi:10.1088/0004-637X/804/2/140.
@article{osti_22522430,
title = {THE 2D DISTRIBUTION OF IRON-RICH EJECTA IN THE REMNANT OF SN 1885 IN M31},
author = {Fesen, Robert A. and Höflich, Peter A. and Hamilton, Andrew J. S.},
abstractNote = {We present Hubble Space Telescope (HST) ultraviolet Fe i and Fe ii images of the remnant of Supernova 1885 (S And) which is observed in absorption against the bulge of the Andromeda galaxy, M31. We compare these Fe i and Fe ii absorption line images to previous HST absorption images of S And, of which the highest quality and theoretically cleanest is Ca ii H and K. Because the remnant is still in free expansion, these images provide a 2D look at the distribution of iron synthesized in this probable Type Ia explosion, thus providing insights and constraints for theoretical SN Ia models. The Fe i images show extended absorption offset to the east from the remnant’s center as defined by Ca ii images and is likely an ionization effect due to self-shielding. More significant is the remnant’s apparent Fe ii distribution which consists of four streams or plumes of Fe-rich material seen in absorption that extend from remnant center out to about 10,000 km s{sup −1}. This is in contrast to the remnant’s Ca ii absorption, which is concentrated in a clumpy, broken shell spanning velocities of 1000–5000 km s{sup −1} but which extends out to 12,500 km s{sup −1}. The observed distributions of Ca- and Fe-rich ejecta in the SN 1885 remnant are consistent with delayed detonation white dwarf models. The largely spherical symmetry of the Ca-rich layer argues against a highly anisotropic explosion as might result from a violent merger of two white dwarfs.},
doi = {10.1088/0004-637X/804/2/140},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 804,
place = {United States},
year = {2015},
month = {5}
}