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Title: Spectral models for early time SN 2011fe observations

Abstract

We use observed UV through near-IR spectra to examine whether SN 2011fe can be understood in the framework of Branch-normal Type Ia supernovae (SNe Ia) and to examine its individual peculiarities. As a benchmark, we use a delayed-detonationmodel with a progenitormetallicity of Z /20. We study the sensitivity of features to variations in progenitor metallicity, the outer density profile, and the distribution of radioactive nickel. The effect of metallicity variations in the progenitor have a relatively small effect on the synthetic spectra. We also find that the abundance stratification of SN 2011fe resembles closely that of a delayed-detonation model with a transition density that has been fit to other Branch-normal SNe Ia. At early times, the model photosphere is formed in material with velocities that are too high, indicating that the photosphere recedes too slowly or that SN 2011fe has a lower specific energy in the outer ≈0.1 M than does the model. We discuss several explanations for the discrepancies. Lastly, we examine variations in both the spectral energy distribution and in the colours due to variations in the progenitor metallicity, which suggests that colours are only weak indicators for the progenitor metallicity, in the particular explosion model thatmore » we have studied. Here we do find that the flux in the U band is significantly higher at maximum light in the solar metallicity model than in the lower metallicity model and the lower metallicity model much better matches the observed spectrum.« less

Authors:
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [5];  [11];  [11];  [10]
  1. Univ. of Oklahoma, Norman, OK (United States). Homer L. Dodge Dept. of Physics and Astronomy; Hamburger Sternwarte, Hamburg (Germany)
  2. Florida State Univ., Tallahassee, FL (United States). Dept. of Physics
  3. Univ. of Oklahoma, Norman, OK (United States). Homer L. Dodge Dept. of Physics and Astronomy
  4. Univ. of Southampton (United Kingdom). School of Physics and Astronomy
  5. Las Campanas Observatory, La Serena (Chile)
  6. California Inst. of Technology (CalTech), Pasadena, CA (United States). Cahill Center for Astrophysics
  7. Weizmann Inst. of Science, Rehovot (Israel). Benoziyo Center for Astrophysics
  8. Las Cumbres Observatory Global Telescope Network, Goleta, CA (United States); Univ. of California, Santa Barbara, CA (United States). Dept. of Physics
  9. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). Computational Cosmology Center
  10. Univ. of Granada (Spain)
  11. Texas A & M Univ., College Station, TX (United States). Dept. of Physics and Astronomy, George P. and Cynthia Woods Mitchell Inst. for Fundamental Physics and Astronomy
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); German Research Foundation (DFG); Spanish Ministry of Science and Innovation
OSTI Identifier:
1407294
Grant/Contract Number:  
AC02-05CH11231; NAS5-26555; AST-0703902
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 454; Journal Issue: 3; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; radiative transfer; supernovae general; supernovae individual; SN 2011fe

Citation Formats

Baron, E., Hoeflich, P., Friesen, Brian, Sullivan, M., Hsiao, E., Ellis, R. S., Gal-Yam, A., Howell, D. A., Nugent, P. E., Dominguez, I., Krisciunas, K., Phillips, M. M., Suntzeff, N., Wang, L., and Thomas, R. C. Spectral models for early time SN 2011fe observations. United States: N. p., 2015. Web. doi:10.1093/mnras/stv1951.
Baron, E., Hoeflich, P., Friesen, Brian, Sullivan, M., Hsiao, E., Ellis, R. S., Gal-Yam, A., Howell, D. A., Nugent, P. E., Dominguez, I., Krisciunas, K., Phillips, M. M., Suntzeff, N., Wang, L., & Thomas, R. C. Spectral models for early time SN 2011fe observations. United States. doi:10.1093/mnras/stv1951.
Baron, E., Hoeflich, P., Friesen, Brian, Sullivan, M., Hsiao, E., Ellis, R. S., Gal-Yam, A., Howell, D. A., Nugent, P. E., Dominguez, I., Krisciunas, K., Phillips, M. M., Suntzeff, N., Wang, L., and Thomas, R. C. Tue . "Spectral models for early time SN 2011fe observations". United States. doi:10.1093/mnras/stv1951. https://www.osti.gov/servlets/purl/1407294.
@article{osti_1407294,
title = {Spectral models for early time SN 2011fe observations},
author = {Baron, E. and Hoeflich, P. and Friesen, Brian and Sullivan, M. and Hsiao, E. and Ellis, R. S. and Gal-Yam, A. and Howell, D. A. and Nugent, P. E. and Dominguez, I. and Krisciunas, K. and Phillips, M. M. and Suntzeff, N. and Wang, L. and Thomas, R. C.},
abstractNote = {We use observed UV through near-IR spectra to examine whether SN 2011fe can be understood in the framework of Branch-normal Type Ia supernovae (SNe Ia) and to examine its individual peculiarities. As a benchmark, we use a delayed-detonationmodel with a progenitormetallicity of Z⊙/20. We study the sensitivity of features to variations in progenitor metallicity, the outer density profile, and the distribution of radioactive nickel. The effect of metallicity variations in the progenitor have a relatively small effect on the synthetic spectra. We also find that the abundance stratification of SN 2011fe resembles closely that of a delayed-detonation model with a transition density that has been fit to other Branch-normal SNe Ia. At early times, the model photosphere is formed in material with velocities that are too high, indicating that the photosphere recedes too slowly or that SN 2011fe has a lower specific energy in the outer ≈0.1 M⊙ than does the model. We discuss several explanations for the discrepancies. Lastly, we examine variations in both the spectral energy distribution and in the colours due to variations in the progenitor metallicity, which suggests that colours are only weak indicators for the progenitor metallicity, in the particular explosion model that we have studied. Here we do find that the flux in the U band is significantly higher at maximum light in the solar metallicity model than in the lower metallicity model and the lower metallicity model much better matches the observed spectrum.},
doi = {10.1093/mnras/stv1951},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 454,
place = {United States},
year = {2015},
month = {10}
}

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    Works referencing / citing this record:

    Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv
    journal, March 2018