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 »
- Authors:
-
- Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Lab, Hanover, NH 03755 (United States)
- Department of Physics, Florida State University, Tallahassee, FL 32306 (United States)
- 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. https://doi.org/10.1088/0004-637X/804/2/140
Fesen, Robert A., Höflich, Peter A., and Hamilton, Andrew J. S. 2015.
"THE 2D DISTRIBUTION OF IRON-RICH EJECTA IN THE REMNANT OF SN 1885 IN M31". United States. https://doi.org/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},
url = {https://www.osti.gov/biblio/22522430},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 804,
place = {United States},
year = {Sun May 10 00:00:00 EDT 2015},
month = {Sun May 10 00:00:00 EDT 2015}
}