A Spitzer Survey for Dust-Obscured Supernovae

TL;DR

This study uses a space-based infrared survey with Spitzer to detect dust-obscured supernovae in luminous infrared galaxies, addressing limitations of ground-based observations and aligning observed rates with theoretical models.

Contribution

First infrared space-based survey of dust-obscured supernovae in LIRGs, demonstrating improved sensitivity and detection rates despite PSF challenges.

Findings

Detected 9 supernovae, 5 previously undiscovered by optical surveys.

Forward-modeling improved sensitivity by approximately 1.5 magnitudes.

Observed supernova rates are consistent with theoretical models after sensitivity adjustments.

Abstract

Supernova (SN) rates serve as an important probe of star-formation models and initial mass functions. Near-infrared seeing-limited ground-based surveys typically discover a factor of 3-10 fewer SNe than predicted from far-infrared (FIR) luminosities owing to sensitivity limitations arising from both a variable point-spread function (PSF) and high dust extinction in the nuclear regions of star-forming galaxies. This inconsistency has potential implications for our understanding of star-formation rates and massive-star evolution, particularly at higher redshifts, where star-forming galaxies are more common. To resolve this inconsistency, a successful SN survey in the local universe must be conducted at longer wavelengths and with a space-based telescope, which has a stable PSF to reduce the necessity for any subtraction algorithms and thus residuals. Here we report on a two-year Spitzer/IRAC 3.6 um survey for dust-extinguished SNe in the nuclear regions of forty luminous infrared galaxies (LIRGs) within 200 Mpc. The asymmetric Spitzer PSF results in worse than expected subtraction residuals when implementing standard template subtraction. Forward-modeling techniques improve our sensitivity by ~1.5 magnitudes. We report the detection of 9 SNe, five of which were not discovered by optical surveys. After adjusting our predicted rates to account for the sensitivity of our survey, we find that the number of detections is consistent with the models. While this search is nonetheless hampered by a difficult-to-model PSF and the relatively poor resolution of Spitzer, it will benefit from future missions, such as Roman Space Telescope and JWST, with higher resolution and more symmetric PSFs.