Imaging of Four Galactic Supernovae Remnants in the Mid-Infrared, and their Interaction with the Interstellar Medium

TL;DR

This study uses mid-infrared imaging to analyze four galactic supernova remnants, revealing their interaction with the interstellar medium and potential star formation triggered by supernova events.

Contribution

It provides detailed MIR observations and modeling of SNRs, highlighting their role in ISM interaction and star formation initiation, with insights into shock excitation and dust grain processing.

Findings

Evidence of ISM interaction with SNRs

Possible star formation triggered by supernovae

MIR emission consistent with shock-excited H2 and PAHs

Abstract

We provide mid-infrared (MIR) imaging, photometry and profiles for the Galactic supernova remnants (SNRs) G001.0-00.1, G355.9-02.5, G355.6-00.0, and W28 based upon data deriving for the Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE). All of the sources show evidence for interaction with the interstellar medium (ISM), leading to curved frontal structures and apparent voids in the ISM. An analysis of the spectral energy distributions (SEDs) of Class I young stellar objects (YSOs) within the north-westerly interaction region of W28, and of the density of stars within the borders of the SNR, suggests that many of them may have been triggered by the SN event. 2-D radiative transfer modelling permits us to constrain the physical parameters of the sources. It is also noted that the location of Class I YSOs about the perimeter of G001.0-00.1, and close to frontal arcs associated with SNR G355.9-02.5, suggests that star formation may have been triggered by these SNRs as well. Finally, it is found that the MIR colours of the frontal structures appear consistent with shock excitation of the v = 0->0 transitions of H2, although it is conceivable that emission by polycyclic aromatic hydrocarbons (PAHs) may also play a role. Where the latter mechanism is relevant, then it is possible that emission derives from the shattering of larger grains in frontal regions, leading to increased volume densities of PAH carrying grains.