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The environmental dependence of mid-IR luminous dusty Supernovae

Lin Xiao, Zeyue Peng, Lluis Galbany, Tamas Szalai, Ori D. Fox, Lei Hu, Maokai Hu, Thallis Pessi, Yi Yang, Takashi J. Moriya, Zhanwen Han, Xiaofeng Wang, Shengyu Yan

Abstract

Using the Spitzer and WISE images, we discovered 42 mid-IR luminous dusty supernovae with local integral-field spectroscopy data. The observed mid-IR emission indicates the presence of newly formed dust, or pre-existing dust heated by the radiation from the supernovae or circumstellar medium interactions. We carried out a systematic analysis of the supernova host environments and their dust properties, for understanding the dust-veiled exploding stars, and whether such an intense dust production process is associated with their local environments. We find that dusty supernovae prefer the locations with higher EW(Hα), lower metallicity, and heavier host extinctions compared to typical SN types, and they show the same increasing sequence in the values of EW(Hα) and oxygen abundance from hydrogen-rich, type IIn and hydrogen-poor dusty supernovae. These differences in environmental properties of different dusty SN types indicate the diversity of their progenitors. We also found that one marginal correlation is a negative correlation between the SN dust mass and star formation rate. This means that SNe would be more mid-IR luminous and more dust-rich at the region with lower star formation rate. However, the SN dust mass show no correlation with the metallicity and the host extinction, which were thought to be key factors affecting the mass-loss history of progenitors and the CSM environment of SNe. Therefore, the dust formation process in SNe might be insensitive to metallicity and the dust condition of their host environments.

The environmental dependence of mid-IR luminous dusty Supernovae

Abstract

Using the Spitzer and WISE images, we discovered 42 mid-IR luminous dusty supernovae with local integral-field spectroscopy data. The observed mid-IR emission indicates the presence of newly formed dust, or pre-existing dust heated by the radiation from the supernovae or circumstellar medium interactions. We carried out a systematic analysis of the supernova host environments and their dust properties, for understanding the dust-veiled exploding stars, and whether such an intense dust production process is associated with their local environments. We find that dusty supernovae prefer the locations with higher EW(Hα), lower metallicity, and heavier host extinctions compared to typical SN types, and they show the same increasing sequence in the values of EW(Hα) and oxygen abundance from hydrogen-rich, type IIn and hydrogen-poor dusty supernovae. These differences in environmental properties of different dusty SN types indicate the diversity of their progenitors. We also found that one marginal correlation is a negative correlation between the SN dust mass and star formation rate. This means that SNe would be more mid-IR luminous and more dust-rich at the region with lower star formation rate. However, the SN dust mass show no correlation with the metallicity and the host extinction, which were thought to be key factors affecting the mass-loss history of progenitors and the CSM environment of SNe. Therefore, the dust formation process in SNe might be insensitive to metallicity and the dust condition of their host environments.
Paper Structure (5 sections, 3 equations, 2 figures)

This paper contains 5 sections, 3 equations, 2 figures.

Table of Contents

  1. Introduction
  2. Observations and data analysis
  3. Collection of Supernova Data from the IFS sample
  4. Mid-IR photometry from Spitzer and WISE
  5. SED Fitting and Dust properties

Figures (2)

  • Figure 1: The mid-IR photometry of all detected SNe at the band of 3.4 $\mu$m (left) and 4.6 $\mu$m (right), except that SN 2003gd and SN 2013ej detected by Spitzer are at 3.6 $\mu$m (right) and 4.5 $\mu$m (left). The colors are for different subclasses with hydrogen-rich SNe in red, hydrogen-poor SNe in blue and type IIn SNe in green. In the left panel, the empty symbols with downward arrows denote SNe whose absolute magnitudes were calculated with a 3$\sigma$ upper limits. All data are listed in Table \ref{['tab:sndata-photo']}.
  • Figure 2: SEDs of ASASSN-15kj, SN 2016gkg, SN 2017faa and SN 2017hpc at different epochs. WISE data are plotted in circles, and the overplotted lines are the best fit dust models following Equation（\ref{['eq:flux']}）.