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Title: ASPHERICITY, INTERACTION, AND DUST IN THE TYPE II-P/II-L SUPERNOVA 2013EJ IN MESSIER 74

Abstract

SN 2013ej is a well-studied core-collapse supernova (SN) that stemmed from a directly identified red supergiant (RSG) progenitor in galaxy M74. The source exhibits signs of substantial geometric asphericity, X-rays from persistent interaction with circumstellar material (CSM), thermal emission from warm dust, and a light curve that appears intermediate between supernovae of Types II-P and II-L. The proximity of this source motivates a close inspection of these physical characteristics and their potential interconnection. We present multiepoch spectropolarimetry of SN 2013ej during the first 107 days and deep optical spectroscopy and ultraviolet through infrared photometry past ∼800 days. SN 2013ej exhibits the strongest and most persistent continuum and line polarization ever observed for a SN of its class during the recombination phase. Modeling indicates that the data are consistent with an oblate ellipsoidal photosphere, viewed nearly edge-on and probably augmented by optical scattering from circumstellar dust. We suggest that interaction with an equatorial distribution of CSM, perhaps the result of binary evolution, is responsible for generating the photospheric asphericity. Relatedly, our late-time optical imaging and spectroscopy show that asymmetric CSM interaction is ongoing, and the morphology of broad H α emission from shock-excited ejecta provides additional evidence that the geometry ofmore » the interaction region is ellipsoidal. Alternatively, a prolate ellipsoidal geometry from an intrinsically bipolar explosion is also a plausible interpretation of the data but would probably require a ballistic jet of radioactive material capable of penetrating the hydrogen envelope early in the recombination phase. Finally, our latest space-based optical imaging confirms that the late interaction-powered light curve dropped below the stellar progenitor level, confirming the RSG star’s association with the explosion.« less

Authors:
; ; ;  [1];  [2];  [3]; ;  [4];  [5]
  1. Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States)
  2. Infrared Processing and Analysis Center, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125 (United States)
  3. Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St., Rehovot (Israel)
  4. Department of Physics, Texas A and M University, College Station, TX 77843 (United States)
  5. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
Publication Date:
OSTI Identifier:
22663982
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 834; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMMETRY; DISTRIBUTION; DUSTS; EMISSION; GALAXIES; INTERACTIONS; PHOTOMETRY; PHOTOSPHERE; POLARIZATION; RADIOACTIVE MATERIALS; RECOMBINATION; SCATTERING; SIMULATION; SPACE; SPECTROSCOPY; TYPE II SUPERNOVAE; ULTRAVIOLET RADIATION; X RADIATION

Citation Formats

Mauerhan, Jon C., Graham, Melissa L., Filippenko, Alexei V., Shivvers, Isaac, Van Dyk, Schuyler D., Johansson, Joel, Hu, Maokai, Wang, Lifan, and Fox, Ori D., E-mail: mauerhan@astro.berkeley.edu. ASPHERICITY, INTERACTION, AND DUST IN THE TYPE II-P/II-L SUPERNOVA 2013EJ IN MESSIER 74. United States: N. p., 2017. Web. doi:10.3847/1538-4357/834/2/118.
Mauerhan, Jon C., Graham, Melissa L., Filippenko, Alexei V., Shivvers, Isaac, Van Dyk, Schuyler D., Johansson, Joel, Hu, Maokai, Wang, Lifan, & Fox, Ori D., E-mail: mauerhan@astro.berkeley.edu. ASPHERICITY, INTERACTION, AND DUST IN THE TYPE II-P/II-L SUPERNOVA 2013EJ IN MESSIER 74. United States. doi:10.3847/1538-4357/834/2/118.
Mauerhan, Jon C., Graham, Melissa L., Filippenko, Alexei V., Shivvers, Isaac, Van Dyk, Schuyler D., Johansson, Joel, Hu, Maokai, Wang, Lifan, and Fox, Ori D., E-mail: mauerhan@astro.berkeley.edu. Tue . "ASPHERICITY, INTERACTION, AND DUST IN THE TYPE II-P/II-L SUPERNOVA 2013EJ IN MESSIER 74". United States. doi:10.3847/1538-4357/834/2/118.
@article{osti_22663982,
title = {ASPHERICITY, INTERACTION, AND DUST IN THE TYPE II-P/II-L SUPERNOVA 2013EJ IN MESSIER 74},
author = {Mauerhan, Jon C. and Graham, Melissa L. and Filippenko, Alexei V. and Shivvers, Isaac and Van Dyk, Schuyler D. and Johansson, Joel and Hu, Maokai and Wang, Lifan and Fox, Ori D., E-mail: mauerhan@astro.berkeley.edu},
abstractNote = {SN 2013ej is a well-studied core-collapse supernova (SN) that stemmed from a directly identified red supergiant (RSG) progenitor in galaxy M74. The source exhibits signs of substantial geometric asphericity, X-rays from persistent interaction with circumstellar material (CSM), thermal emission from warm dust, and a light curve that appears intermediate between supernovae of Types II-P and II-L. The proximity of this source motivates a close inspection of these physical characteristics and their potential interconnection. We present multiepoch spectropolarimetry of SN 2013ej during the first 107 days and deep optical spectroscopy and ultraviolet through infrared photometry past ∼800 days. SN 2013ej exhibits the strongest and most persistent continuum and line polarization ever observed for a SN of its class during the recombination phase. Modeling indicates that the data are consistent with an oblate ellipsoidal photosphere, viewed nearly edge-on and probably augmented by optical scattering from circumstellar dust. We suggest that interaction with an equatorial distribution of CSM, perhaps the result of binary evolution, is responsible for generating the photospheric asphericity. Relatedly, our late-time optical imaging and spectroscopy show that asymmetric CSM interaction is ongoing, and the morphology of broad H α emission from shock-excited ejecta provides additional evidence that the geometry of the interaction region is ellipsoidal. Alternatively, a prolate ellipsoidal geometry from an intrinsically bipolar explosion is also a plausible interpretation of the data but would probably require a ballistic jet of radioactive material capable of penetrating the hydrogen envelope early in the recombination phase. Finally, our latest space-based optical imaging confirms that the late interaction-powered light curve dropped below the stellar progenitor level, confirming the RSG star’s association with the explosion.},
doi = {10.3847/1538-4357/834/2/118},
journal = {Astrophysical Journal},
number = 2,
volume = 834,
place = {United States},
year = {Tue Jan 10 00:00:00 EST 2017},
month = {Tue Jan 10 00:00:00 EST 2017}
}