The Type II-plateau Supernova 2017eaw in NGC 6946 and Its Red Supergiant Progenitor
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Author
Van Dyk, Schuyler D.Zheng, WeiKang

Maund, Justyn R.
Brink, Thomas G.
Srinivasan, Sundar
Andrews, Jennifer E.
Smith, Nathan
Leonard, Douglas C.
Morozova, Viktoriya
Filippenko, Alexei V.
Conner, Brody
Milisavljevic, Dan
de Jaeger, Thomas
Long, Knox S.
Isaacson, Howard
Crossfield, Ian J. M.
Kosiarek, Molly R.
Howard, Andrew W.

Fox, Ori D.
Kelly, Patrick L.
Piro, Anthony L.
Littlefair, Stuart P.
Dhillon, Vik S.
Wilson, Richard
Butterley, Timothy
Yunus, Sameen
Channa, Sanyum
Jeffers, Benjamin T.
Falcon, Edward
Ross, Timothy W.
Hestenes, Julia C.
Stegman, Samantha M.
Zhang, Keto
Kumar, Sahana
Affiliation
Univ Arizona, Steward ObservIssue Date
2019-04-24Keywords
galaxies: distances and redshiftsgalaxies: individual (NGC 6946)
stars: massive
supergiants
supernovae: general
supernovae: individual (SN 2017eaw)
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IOP PUBLISHING LTDCitation
Schuyler D. Van Dyk et al 2019 ApJ 875 136Journal
ASTROPHYSICAL JOURNALRights
Copyright © 2019. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We present extensive optical photometric and spectroscopic observations, from 4 to 482 days after explosion, of the Type II-plateau (II-P) supernova (SN) 2017eaw in NGC 6946. SN 2017eaw is a normal SN II-P intermediate in properties between, for example, SN 1999em and SN 2012aw and the more luminous SN 2004et, also in NGC 6946. We have determined that the extinction to SN 2017eaw is primarily due to the Galactic foreground and that the SN site metallicity is likely subsolar. We have also independently confirmed a tip-of-the-red-giant-branch (TRGB) distance to NGC 6946 of 7.73 ± 0.78 Mpc. The distances to the SN that we have also estimated via both the standardized candle method and expanding photosphere method corroborate the TRGB distance. We confirm the SN progenitor identity in pre-explosion archival Hubble Space Telescope (HST) and Spitzer Space Telescope images, via imaging of the SN through our HST Target of Opportunity program. Detailed modeling of the progenitor's spectral energy distribution indicates that the star was a dusty, luminous red supergiant consistent with an initial mass of ~15 M ⊙.ISSN
0004-637XVersion
Final published versionSponsors
National Aeronautics and Space Administration (NASA) [NAS5-26555]; NASA through grants from STScI [GO-14645, GO-15166]; JPL/Caltech; Royal Society University Research Fellowship; Taiwan Ministry of Science and Technology [MOST104-2628-M-001-004-MY3]; NSF [AST-1515559, DGE 1339067, AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund; Miller Institute for Basic Research in Science (U.C. Berkeley); NASA/HST grant from STScI [AR-14295]; Scialog award by the Research Corporation for Science Advancement; University of Sheffield Alumni Foundation; Science and Technology Facilities Council [ST/P000541/1]; W. M. Keck Foundationae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/ab1136