Red and Reddened: Ultraviolet through Near-Infrared Observations of Type Ia Supernova 2017erp

TL;DR

This study presents ultraviolet to near-infrared observations of SN2017erp, a Type Ia supernova, revealing intrinsic UV color differences likely due to metallicity variations, which impact cosmological distance measurements.

Contribution

It provides detailed multi-wavelength data of SN2017erp and analyzes intrinsic UV color differences, highlighting metallicity as a key factor influencing NUV variations in Type Ia supernovae.

Findings

SN2017erp is a normal Type Ia supernova with NUV-red colors.

Intrinsic UV differences are significant and not solely due to dust reddening.

Metallicity may be the physical cause of NUV color variations.

Abstract

We present space-based ultraviolet/optical photometry and spectroscopy with the Swift Ultra-Violet/Optical Telescope and Hubble Space Telescope, respectively, along with ground-based optical photometry and spectroscopy and near-infrared spectroscopy of supernova SN2017erp. The optical light curves and spectra are consistent with a normal Type Ia supernova (SN Ia). Compared to previous photometric samples in the near-ultraviolet (NUV), SN2017erp has colors similar to the NUV-red category after correcting for Milky Way and host dust reddening. We find the difference between SN2017erp and the NUV-blue SN2011fe is not consistent with dust reddening alone but is similar to the SALT color law, derived from rest-frame UV photometry of higher redshift SNe Ia. This chromatic difference is dominated by the intrinsic differences in the UV and only a small contribution from the expected dust reddening. Differentiating the two can have important consequences for determining cosmological distances with rest-frame UV photometry. This spectroscopic series is important for analyzing SNe Ia with intrinsically redder NUV colors. We also 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 Angstroms implying a factor of ten higher metallicity in the upper layers of SN2017erp 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.