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Title: The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star

Abstract

A blue source in pre-explosion Hubble Space Telescope ( HST )/Wide-Field Planetary Camera 2 (WFPC2) images falls within the 5 σ astrometric error circle (∼0.″24) derived from post-explosion ground-based imaging of SN 2010jl. At the time the ground-based astrometry was published, however, the SN had not faded sufficiently for post-explosion HST follow-up observations to determine a more precise astrometric solution and/or confirm if the pre-explosion source had disappeared, both of which are necessary to ultimately disentangle the possible progenitor scenarios. Here we present HST /WFC3 imaging of the SN 2010jl field obtained in 2014, 2015, and 2016 when the SN had faded sufficiently to allow for new constraints on the progenitor. The SN, which is still detected in the new images, is offset by 0.″061 ± 0.″008 (15 ± 2 pc) from the underlying and extended source of emission that contributes at least partially, if not entirely, to the blue source previously suggested as the candidate progenitor in the WFPC2 data. This point alone rules out the possibility that the blue source in the pre-explosion images is the exploding star, but may instead suggest an association with a young (<5–6 Myr) cluster and still argues for a massive (>30 Mmore » {sub ⊙}) progenitor. We obtain new upper limits on the flux from a single star at the SN position in the pre-explosion WFPC2 and Spitzer /IRAC images that may ultimately be used to constrain the progenitor properties.« less

Authors:
 [1];  [2];  [3]; ;  [4]; ; ;  [5];  [6];  [7];  [8]
  1. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
  2. IPAC/Caltech, Mailcode 100-22, Pasadena, CA 91125 (United States)
  3. Astrophysics Science Division, NASA Goddard Space Flight Center, Mail Code 665, Greenbelt, MD 20771 (United States)
  4. Steward Observatory, 933 N. Cherry Avenue, Tucson, AZ 85721 (United States)
  5. Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States)
  6. CRESST/UMBC/GSFC Code 665, NASA/GSFC, Greenbelt MD, 20771 (United States)
  7. Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States)
  8. Jet Propulsion Laboratory, 4800 Oak Grove Drive, MS 169-506, Pasadena, CA 91109 (United States)
Publication Date:
OSTI Identifier:
22663766
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 836; 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; DUSTS; EMISSION; EXPLOSIONS; LIMITING VALUES; LUMINOSITY; SPACE; SUPERNOVAE; TELESCOPES; TYPE II SUPERNOVAE

Citation Formats

Fox, Ori D., Dyk, Schuyler D. Van, Dwek, Eli, Smith, Nathan, Andrews, Jennifer, Filippenko, Alexei V., Kelly, Patrick L., Shivvers, Isaac, Arendt, Richard G., Foley, Ryan J., and Miller, Adam A., E-mail: ofox@stsci.edu. The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star. United States: N. p., 2017. Web. doi:10.3847/1538-4357/836/2/222.
Fox, Ori D., Dyk, Schuyler D. Van, Dwek, Eli, Smith, Nathan, Andrews, Jennifer, Filippenko, Alexei V., Kelly, Patrick L., Shivvers, Isaac, Arendt, Richard G., Foley, Ryan J., & Miller, Adam A., E-mail: ofox@stsci.edu. The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star. United States. doi:10.3847/1538-4357/836/2/222.
Fox, Ori D., Dyk, Schuyler D. Van, Dwek, Eli, Smith, Nathan, Andrews, Jennifer, Filippenko, Alexei V., Kelly, Patrick L., Shivvers, Isaac, Arendt, Richard G., Foley, Ryan J., and Miller, Adam A., E-mail: ofox@stsci.edu. Mon . "The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star". United States. doi:10.3847/1538-4357/836/2/222.
@article{osti_22663766,
title = {The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star},
author = {Fox, Ori D. and Dyk, Schuyler D. Van and Dwek, Eli and Smith, Nathan and Andrews, Jennifer and Filippenko, Alexei V. and Kelly, Patrick L. and Shivvers, Isaac and Arendt, Richard G. and Foley, Ryan J. and Miller, Adam A., E-mail: ofox@stsci.edu},
abstractNote = {A blue source in pre-explosion Hubble Space Telescope ( HST )/Wide-Field Planetary Camera 2 (WFPC2) images falls within the 5 σ astrometric error circle (∼0.″24) derived from post-explosion ground-based imaging of SN 2010jl. At the time the ground-based astrometry was published, however, the SN had not faded sufficiently for post-explosion HST follow-up observations to determine a more precise astrometric solution and/or confirm if the pre-explosion source had disappeared, both of which are necessary to ultimately disentangle the possible progenitor scenarios. Here we present HST /WFC3 imaging of the SN 2010jl field obtained in 2014, 2015, and 2016 when the SN had faded sufficiently to allow for new constraints on the progenitor. The SN, which is still detected in the new images, is offset by 0.″061 ± 0.″008 (15 ± 2 pc) from the underlying and extended source of emission that contributes at least partially, if not entirely, to the blue source previously suggested as the candidate progenitor in the WFPC2 data. This point alone rules out the possibility that the blue source in the pre-explosion images is the exploding star, but may instead suggest an association with a young (<5–6 Myr) cluster and still argues for a massive (>30 M {sub ⊙}) progenitor. We obtain new upper limits on the flux from a single star at the SN position in the pre-explosion WFPC2 and Spitzer /IRAC images that may ultimately be used to constrain the progenitor properties.},
doi = {10.3847/1538-4357/836/2/222},
journal = {Astrophysical Journal},
number = 2,
volume = 836,
place = {United States},
year = {Mon Feb 20 00:00:00 EST 2017},
month = {Mon Feb 20 00:00:00 EST 2017}
}