Infrared Ejecta and Cold Dust in the Young Supernova Remnant N132D

Abstract

We present Spitzer, Wide-field Infrared Survey Explorer (WISE), and Herschel observations of the young supernova remnant (SNR) N132D in the Large Magellanic Cloud, including 3–40 μm Spitzer Infrared Spectrograph (IRS) mapping, 12 μm WISE and 70, 100, 160, 250, 350, and 500 μm Herschel images. The high-velocity lines of [Ne ii] at 12.8 μm, [Ne iii] at 15.5 μm, and [O iv] 26 μm reveal infrared ejecta concentrated in a central ring and coincide with the optical and X-ray ejecta. Herschel images reveal far-IR emission coinciding with the central ejecta, which suggests that the IR emission is freshly formed, cold dust in the SN ejecta. The infrared spectra are remarkably similar to those of another young SNR of 1E0102 with Ne and O lines. Shock modeling of the Ne ejecta emission suggests a gas temperature of 300–600 K and densities in the range 1000–2 × 104 cm−3 in the postshock photoionized region. The IR continuum from the ejecta shows an 18 μm peak dust feature. We performed spectral fitting to the IRS dust continuum and Herschel photometry. The dust mass associated with the central ejecta is 1.25 ± 0.65 M ⊙, while the 18 μm dust feature requires forsterite grains. The dust mass of the central ejecta region in N132D is higher than those of other young SNRs, which is likely associated with its higher progenitor mass. We discuss the dust productivity in the ejecta of N132D and infer its plausible implications for dust in the early universe.

Fine-structure Transitions of Ne+, Ar+, Ne2+, and Ar2+ Induced by Collisions with Atomic Hydrogen

“…The recent spectral data obtained by the medium-resolution spectrometer (MRS) on the mid-infrared instrument (MIRI) of James Webb Space Telescope (JWST) has unveiled a substantial volume of fine-structure line emissions (Pereira-Santaella et al 2022;Jones et al 2023;Rho et al 2023) continuing progress in mid-infrared observations since, for example, the Infrared Space Observatory (Moorwood et al 1996) and other missions. These emissions arise from a variety of ions, including [Ar II], [Ar III], [Ne II], and [Ne III].…”