CaltechAUTHORS
  A Caltech Library Service

Supernova 2017eaw: Molecule and Dust Formation from Infrared Observations

Tinyanont, Samaporn and Kasliwal, Mansi M. and Krafton, Kelsie and Lau, Ryan and Rho, Jeonghee and Leonard, Douglas C. and De, Kishalay and Jencson, Jacob and Mawet, Dimitri and Millar-Blanchaer, Maxwell and Nilsson, Ricky and Yan, Lin and Gehrz, Robert D. and Helou, George and Van Dyk, Schuyler D. and Serabyn, Eugene and Fox, Ori D. and Clayton, Geoffrey (2019) Supernova 2017eaw: Molecule and Dust Formation from Infrared Observations. Astrophysical Journal, 873 (2). Art. No. 127. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20190313-132337168

[img] PDF - Published Version
See Usage Policy.

3689Kb
[img] PDF - Submitted Version
See Usage Policy.

1652Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20190313-132337168

Abstract

We present infrared (IR) photometry and spectroscopy of the Type II-P SN 2017eaw and its progenitor in the nearby galaxy NGC 6946. Progenitor observations in the Ks band in four epochs from 1 yr to 1 day before the explosion reveal no significant variability in the progenitor star greater than 6% that lasts longer than 200 days. SN 2017eaw is a typical SN II-P with near-IR and mid-IR photometric evolution similar to those of SNe 2002hh and 2004et, other normal SNe II-P in the same galaxy. Spectroscopic monitoring during the plateau phase reveals a possible high-velocity He I 1.083 μm absorption line, indicative of a shock interaction with the circumstellar medium. Spectra between 389 and 480 days postexplosion reveal a strong CO first overtone emission at 389 days, with a line profile matching that of SN 1987A from the same epoch, indicating ~10^(−3) M⊙ of CO at 1800 K. From the 389 days epoch until the most recent observation at 566 days, the first overtone feature fades while the 4.5 μm excess, likely from the CO fundamental band, remains. This behavior indicates that the CO has not been destroyed, but that the gas has cooled enough that the levels responsible for first overtone emissions are no longer populated. Finally, the evolution of Spitzer 3.6 μm photometry shows evidence for dust formation in SN 2017eaw, with a dust mass of 10^(−6) or 10^(−4) M⊙ assuming carbonaceous or silicate grains, respectively.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ab0897DOIArticle
https://arxiv.org/abs/1901.01940arXivDiscussion Paper
ORCID:
AuthorORCID
Tinyanont, Samaporn0000-0002-1481-4676
Kasliwal, Mansi M.0000-0002-5619-4938
Rho, Jeonghee0000-0003-3643-839X
De, Kishalay0000-0002-8989-0542
Jencson, Jacob0000-0001-5754-4007
Mawet, Dimitri0000-0002-8895-4735
Nilsson, Ricky0000-0002-5408-4954
Yan, Lin0000-0003-1710-9339
Gehrz, Robert D.0000-0003-1319-4089
Helou, George0000-0003-3367-3415
Van Dyk, Schuyler D.0000-0001-9038-9950
Fox, Ori D.0000-0003-2238-1572
Clayton, Geoffrey0000-0002-0141-7436
Additional Information:© 2019 The American Astronomical Society. Received 2019 January 28; revised 2019 February 16; accepted 2019 February 18; published 2019 March 13. We thank Jim Fuller and Luc Dessart for helpful discussions and input on the paper draft. We also thank the anonymous referee for reviewing the article. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some of the data presented herein were obtained at Palomar Observatory, which is operated by a collaboration between California Institute of Technology, Jet Propulsion Laboratory, Yale University, and National Astronomical Observatories of China. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. R.D.G. was supported by NASA and the United States Air Force. Facilities: Hale (WIRC, TripleSpec) - , Spitzer - Spitzer Space Telescope satellite, Keck (MOSFIRE, NIRES) - . Software: astropy (Astropy Collaboration et al. 2013; Price-Whelan et al. 2018), spextool (Cushing et al. 2004), xtellcor (Vacca et al. 2003), MOSFIRE data reduction pipeline (McLean et al. 2012), MOCASSIN (v.2.02.72 Ercolano et al. 2003, 2005, 2008), Matplotlib (Hunter 2007).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:circumstellar matter – supernovae: individual (SN2017eaw)
Record Number:CaltechAUTHORS:20190313-132337168
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190313-132337168
Official Citation:Samaporn Tinyanont et al 2019 ApJ 873 127
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:93785
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:13 Mar 2019 21:06
Last Modified:13 Mar 2019 21:06

Repository Staff Only: item control page