Red and Reddened: Ultraviolet through Near-infrared Observations of Type Ia Supernova 2017erp
AuthorBrown, Peter J.
Jha, Saurabh W.
Dettman, Kyle G.
Burns, Chris R.
Howell, D. Andrew
Hsiao, E. Y.
Marion, G. H.
Milne, Peter A.
Ruiter, Ashley J.
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationPeter J. Brown et al 2019 ApJ 877 152
RightsCopyright © 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis 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 email@example.com.
AbstractWe present space-based ultraviolet/optical photometry and spectroscopy with the Swift Ultra-Violet/Optical Telescope and Hubble Space Telescope (HST), respectively, along with ground-based optical photometry and spectroscopy and near-infrared spectroscopy of supernova SN 2017erp. The optical light curves and spectra are consistent with a normal SN Ia. Compared to previous photometric samples in the near-ultraviolet (NUV), SN 2017erp has UV colors that are redder than NUV-blue SNe Ia corrected to similar optical colors. The chromatic difference between SNe 2011fe and 2017erp is dominated by the intrinsic differences in the UV rather than the expected dust reddening. This chromatic difference is similar to the SALT2 color law, derived from rest-frame ultraviolet photometry of higher redshift SNe Ia. Differentiating between intrinsic UV diversity and dust reddening can have important consequences for determining cosmological distances with rest-frame ultraviolet photometry. This ultraviolet spectroscopic series is the first from HST of a normal, albeit reddened, NUV-red SN Ia and is important for analyzing SNe Ia with intrinsically redder NUV colors. We show model comparisons suggesting that metallicity could be the physical difference between NUV-blue and NUV-red SNe Ia, with emission peaks from reverse fluorescence near 3000 Å implying a factor of ~10 higher metallicity in the upper layers of SN 2017erp compared to SN 2011fe. Metallicity estimates are very model dependent, however, and there are multiple effects in the UV. Further models and UV spectra of SNe Ia are needed to explore the diversity of SNe Ia, which show seemingly independent differences in the near-UV peaks and mid-UV flux levels.
VersionFinal published version
SponsorsNASA from the Space Telescope Science Institute ; NASA [NAS 5-26555, NNG17PX03C]; NASA's Astrophysics Data Analysis Program [NNX13AF35G]; NSF [AST 1313484, AST-1821967, 1821987, 1813708, 1813466]; Gemini Observatory [GS-2017A-Q-33]; US Department of Energy [DE-SC0011636]; Australian Research Council [CE110001020, FT170100243]; Chinese Academy of Sciences President's International Fellowship Initiative grant [2016PM014]; National Science Foundation [AST-1613472]