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Title: A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3

Abstract

While theoretical models of dust condensation predict that most refractory elements produced in core-collapse supernovae (SNe) efficiently condense into dust, a large quantity of dust has so far only been observed in SN 1987A. We present an analysis of observations from the Spitzer Space Telescope , Herschel Space Observatory , Stratospheric Observatory for Infrared Astronomy, and AKARI of the infrared shell surrounding the pulsar wind nebula in the supernova remnant G54.1+0.3. We attribute a distinctive spectral feature at 21 μ m to a magnesium silicate grain species that has been invoked in modeling the ejecta-condensed dust in Cas A, which exhibits the same spectral signature. If this species is responsible for producing the observed spectral feature and accounts for a significant fraction of the observed infrared continuum, we find that it would be the dominant constituent of the dust in G54.1+0.3, with possible secondary contributions from other compositions, such as carbon, silicate, or alumina grains. The total mass of SN-formed dust required by this model is at least 0.3 M {sub ⊙}. We discuss how these results may be affected by varying dust grain properties and self-consistent grain heating models. The spatial distribution of the dust mass and temperature inmore » G54.1+0.3 confirms the scenario in which the SN-formed dust has not yet been processed by the SN reverse shock and is being heated by stars belonging to a cluster in which the SN progenitor exploded. The dust mass and composition suggest a progenitor mass of 16–27 M {sub ⊙} and imply a high dust condensation efficiency, similar to that found for Cas A and SN 1987A. The study provides another example of significant dust formation in a Type IIP SN explosion and sheds light on the properties of pristine SN-condensed dust.« less

Authors:
 [1]; ;  [2]; ;  [3]; ;  [4];  [5]
  1. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
  2. Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)
  3. North Carolina State University, Raleigh, NC 27695 (United States)
  4. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
  5. New York University, Abu Dhabi (United Arab Emirates)
Publication Date:
OSTI Identifier:
22663806
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 836; Journal Issue: 1; 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; ALUMINIUM OXIDES; ASTRONOMY; CARBON; DUSTS; EFFICIENCY; EXPLOSIONS; HEATING; MAGNESIUM SILICATES; MASS; NEBULAE; PULSARS; REFRACTORIES; SIMULATION; SPATIAL DISTRIBUTION; SUPERNOVA REMNANTS; SUPERNOVAE; TELESCOPES; VISIBLE RADIATION

Citation Formats

Temim, Tea, Dwek, Eli, Arendt, Richard G., Borkowski, Kazimierz J., Reynolds, Stephen P., Slane, Patrick, Raymond, John C., and Gelfand, Joseph D. A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3. United States: N. p., 2017. Web. doi:10.3847/1538-4357/836/1/129.
Temim, Tea, Dwek, Eli, Arendt, Richard G., Borkowski, Kazimierz J., Reynolds, Stephen P., Slane, Patrick, Raymond, John C., & Gelfand, Joseph D. A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3. United States. doi:10.3847/1538-4357/836/1/129.
Temim, Tea, Dwek, Eli, Arendt, Richard G., Borkowski, Kazimierz J., Reynolds, Stephen P., Slane, Patrick, Raymond, John C., and Gelfand, Joseph D. Fri . "A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3". United States. doi:10.3847/1538-4357/836/1/129.
@article{osti_22663806,
title = {A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3},
author = {Temim, Tea and Dwek, Eli and Arendt, Richard G. and Borkowski, Kazimierz J. and Reynolds, Stephen P. and Slane, Patrick and Raymond, John C. and Gelfand, Joseph D.},
abstractNote = {While theoretical models of dust condensation predict that most refractory elements produced in core-collapse supernovae (SNe) efficiently condense into dust, a large quantity of dust has so far only been observed in SN 1987A. We present an analysis of observations from the Spitzer Space Telescope , Herschel Space Observatory , Stratospheric Observatory for Infrared Astronomy, and AKARI of the infrared shell surrounding the pulsar wind nebula in the supernova remnant G54.1+0.3. We attribute a distinctive spectral feature at 21 μ m to a magnesium silicate grain species that has been invoked in modeling the ejecta-condensed dust in Cas A, which exhibits the same spectral signature. If this species is responsible for producing the observed spectral feature and accounts for a significant fraction of the observed infrared continuum, we find that it would be the dominant constituent of the dust in G54.1+0.3, with possible secondary contributions from other compositions, such as carbon, silicate, or alumina grains. The total mass of SN-formed dust required by this model is at least 0.3 M {sub ⊙}. We discuss how these results may be affected by varying dust grain properties and self-consistent grain heating models. The spatial distribution of the dust mass and temperature in G54.1+0.3 confirms the scenario in which the SN-formed dust has not yet been processed by the SN reverse shock and is being heated by stars belonging to a cluster in which the SN progenitor exploded. The dust mass and composition suggest a progenitor mass of 16–27 M {sub ⊙} and imply a high dust condensation efficiency, similar to that found for Cas A and SN 1987A. The study provides another example of significant dust formation in a Type IIP SN explosion and sheds light on the properties of pristine SN-condensed dust.},
doi = {10.3847/1538-4357/836/1/129},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 836,
place = {United States},
year = {2017},
month = {2}
}