SNR G292.0+1.8: A Remnant of a Low-mass-progenitor Stripped-envelope Supernova

Abstract

We present a study of the Galactic supernova remnant (SNR) G292.0+1.8, a classic example of a core-collapse SNR that contains oxygen-rich ejecta, circumstellar material, a rapidly moving pulsar, and a pulsar wind nebula (PWN). We use hydrodynamic simulations of the remnant’s evolution to show that the SNR reverse shock is interacting with the PWN and has most likely shocked the majority of the supernova ejecta. In our models, such a scenario requires a total ejecta mass of ≲3 M ⊙ and implies that there is no significant quantity of cold ejecta in the interior of the reverse shock. In light of these results, we compare the estimated elemental masses and abundance ratios in the reverse-shocked ejecta to nucleosynthesis models, and further conclude that they are consistent with a progenitor star with an initial mass of 12–16 M ⊙. We conclude that the progenitor of G292.0+1.8 was likely a relatively low-mass star that experienced significant mass loss through a binary interaction and would have produced a stripped-envelope supernova explosion. We also argue that the region known as the “spur” in G292.0+1.8 arises as a result of the pulsar’s motion through the supernova ejecta, and that its dynamical properties may suggest a line-of-sight component to the pulsar’s velocity, leading to a total space velocity of ∼600 km s−1 and implying a significant natal kick. Finally, we discuss binary mass-loss scenarios relevant to G292.0+1.8 and their implications for the binary companion properties and future searches.

Hubble Space Telescope Proper Motion Measurements of Supernova Remnant N132D: Center of Expansion and Age

“…Recent simulations show that inhomogenous surrounding environments are reflected in the forward and reverse shock for only ≈2000 yr (Orlando et al 2022). There is also evidence that G292ʼs morphology is influenced by the motion of its surviving pulsar (Temim et al 2022).…”

“…They offer unique opportunities to probe the elemental distribution of metal-rich ejecta and investigate the progenitor star's mass-loss history at fine scales (see Lopez & Fesen 2018 for a review). Young, nearby oxygen-rich (O-rich) SNRs, created from the collapse of massive stars (zero-age main sequence, ZAMS, mass > 8 M e ; Smartt 2009), are especially informative to study core-collapse dynamics because they are often associated with progenitor stars that were largely stripped of their hydrogen envelopes (e.g., Blair et al 2000;Chevalier 2005;Temim et al 2022). The kinematic and chemical properties of their metal-rich ejecta retain information about the parent supernova explosion that would otherwise be lost in an H-rich explosion (Milisavljevic et al 2010).…”

The Distance to the S147 Supernova Remnant

“…They are physically interesting and important probes of both the explosion and nature of progenitor stars (see, e.g., the reviews of Vink 2012 andDubner &Giacani 2015). For example, estimates of ejecta masses, velocities, and energies constrain the progenitor and explosions (e.g., Temim et al 2022;Braun et al 2023). They are laboratories for shock physics (e.g., Raymond et al 2020aRaymond et al , 2020b.…”

A Nitrogen-rich Supernova Remnant in M31: Interaction with the Circumstellar Medium at Late Times

“…Supernova remnants (SNRs) that show optical emission from supernova (SN) ejecta and circumstellar medium (CSM) are rare, but they provide unique information about the SN progenitor and about the explosion. There are a handful of oxygen-rich SNRs in the Galaxy and the Magellanic Clouds such as Cas A, G292.0+1.8, N132D, and 1E102-72.3 (Blair et al 2000;Hwang & Laming 2012;Temim et al 2022), but only three oxygen-rich SNRs are known in other galaxies (NGC 4449 and M83;Blair et al 1984;Lee & Lee 2014;Winkler et al 2017), and it is somewhat surprising that so few SNRs like Cas A have been found in surveys of other galaxies. Nitrogen-rich SNRs are even more rare.…”