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1. Angular emission patterns of remnant black holes

   https://doi.org/10.1103/PhysRevD.105.024016  

   Li, Xiang; Sun, Ling; Lo, Rico Ka Lok; Payne, Ethan; Chen, Yanbei (January 2022, Physical Review D)
2. The Distance to the S147 Supernova Remnant

   https://doi.org/10.3847/1538-4357/ad4493  

   Kochanek, C_S; Raymond, John_C; Caldwell, Nelson (June 2024, The Astrophysical Journal)

   Abstract In the absence of a parallax distance to a pulsar or a surviving binary in a supernova remnant (SNR), distances to Galactic SNRs are generally very uncertain. However, by combining Gaia data with wide-field, multifiber echelle spectroscopy, it is now possible to obtain accurate distances to many SNRs with limited extinction by searching for the appearance of high-velocity Caiior Naiabsorption lines in hot stars as a function of distance. We demonstrate this for the SNR S147 using the spectra of 259 luminous blue stars. We obtain a median distance of 1.37 kpc (1.30–1.47 kpc at 90% confidence), which is consistent with the median parallax distance to the pulsar of 1.46 kpc (1.12–2.10 kpc at 90% confidence) but with significantly smaller uncertainties. Our distance is also consistent with the distance to the candidate unbound binary companion in this SNR, HD 37424 at a photogeometric distance of 1.45 kpc (1.40–1.50 kpc at 1σ). The presence of high-velocity absorption lines is correlated with the Hα/O [iii] emission-line flux of the SNR but not with the radio flux. 

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3. The Masses of Supernova Remnant Progenitors in M33

   https://doi.org/10.3847/1538-4357/acc249  

   Koplitz, Brad; Johnson, Jared; Williams, Benjamin F.; Díaz-Rodríguez, Mariangelly; Murphy, Jeremiah W.; Lazzarini, Margaret; Guzman, Joseph; Dalcanton, Julianne J.; Dolphin, Andrew; Durbin, Meredith (May 2023, The Astrophysical Journal)

   Abstract Using resolved optical stellar photometry from the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region survey, we measured the star formation history near the position of 85 supernova remnants (SNRs) in M33. We constrained the progenitor masses for 60 of these SNRs, finding that the remaining 25 remnants had no local star formation in the last 56 Myr, consistent with core-collapse supernovae, making them potential Type Ia candidates. We then infer a progenitor mass distribution from the age distribution, assuming single star evolution. We find that the progenitor mass distribution is consistent with being drawn from a power law with an index of − 2.9 − 1.0 + 1.2 . Additionally, we infer a minimum progenitor mass of 7.1 − 0.2 + 0.1 M ⊙ from this sample, consistent with several previous studies, providing further evidence that stars with ages older than the lifetimes of single 8 M ⊙ stars are producing supernovae. 

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4. MMT Spectroscopy of Supernova Remnant Candidates in M33

   https://doi.org/10.3847/1538-4357/aaac7e  

   Long, Knox S.; Blair, William P.; Milisavljevic, Dan; Raymond, John C.; Winkler, P. Frank (March 2018, The Astrophysical Journal)
5. Dense Molecular Clouds in the Crab Supernova Remnant

   https://doi.org/10.3847/1538-4357/ac391a  

   Wootten, Alwyn; Bentley, Rory O.; Baldwin, J.; Combes, F.; Fabian, A. C.; Ferland, G. J.; Loh, E.; Salome, P.; Shingledecker, C. N.; Castro-Carrizo, A. (January 2022, The Astrophysical Journal)

   Abstract Molecular emission was imaged with ALMA from numerous components near and within bright H₂-emitting knots and absorbing dust globules in the Crab Nebula. These observations provide a critical test of how energetic photons and particles produced in a young supernova remnant interact with gas, cleanly differentiating between competing models. The four fields targeted show contrasting properties but within them, seventeen distinct molecular clouds are identified with CO emission; a few also show emission from HCO⁺, SiO, and/or SO. These observations are compared with Cloudy models of these knots. It has been suggested that the Crab filaments present an exotic environment in which H₂emission comes from a mostly neutral zone probably heated by cosmic rays produced in the supernova surrounding a cool core of molecular gas. Our model is consistent with the observed COJ= 3 − 2 line strength. These molecular line emitting knots in the Crab Nebula present a novel phase of the ISM representative of many important astrophysical environments. 

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