A supernova remnant associated with a nascent black hole low-mass X-ray binary

Abstract

Energy released when the core of a high-mass star collapses into a black hole often powers an explosion that creates a supernova remnant. Black holes have limited windows of observability, and consequently are rarely identified in association with supernova remnants. Analysing multi-messenger data, we show that MAXI J1535−571 is the black hole produced in the stellar explosion that gave rise to the supernova remnant G323.7−1.0, making it the first case of an association between a black hole low-mass X-ray binary and a supernova remnant. Given this connection, we can infer from our modeling that the progenitor system was a close binary whose primary star had an initial mass of ∼23-35 solar masses with a companion star about 10 times less massive.

The Black Hole Candidate Swift J1728.9–3613 and the Supernova Remnant G351.9–0.9

“…The binary evolution that is required if Swift J1728.9−3613 is physically associated with G351.9−0.9 is broadly consistent with that described by Maxted et al (2020). Motivated by the possible association of MAXI J1535−571 with G323.7−1.0, Maxted et al (2020) employed the population synthesis code "StarTrack" (Belczynski et al 2008). This code has been used to model X-ray binary populations in other galaxies; in NGC 1569, it predicts a luminosity function that is within a factor of 2 of the observed luminosity function (Belczynski et al 2004).…”

“…This would represent observational support for numerical simulations that predict a subset of core-collapse supernovae can leave black holes and remnants (Ugliano et al 2012). It is worth repeating here that SS 433 in W50, MAXI J1535−571, and W49B may also represent such cases (Blundell et al 2008;Kubota et al 2010;Lopez et al 2013;Cherepashchuk et al 2018;Maxted et al 2020). Unlike SS 433 and W49B, however, X-rays clearly detect a compact object and strongly favor a black hole primary in Swift J1728.9−3613, and for these reasons it may represent the strongest case for a distinct black hole formation channel.…”

“…The binary evolution that is required if Swift J1728.9−3613 is physically associated with G351.9−0.9 is broadly consistent with that described by Maxted et al (2020). Motivated by the possible association of MAXI J1535−571 with G323.7−1.0, Maxted et al (2020) employed the population synthesis code "StarTrack" (Belczynski et al 2008).…”

“…ray bursts to mergers of BH-BH/BH-NS/NS-NS binaries that were confirmed LIGO in 2017 (Abbott et al 2017). Using StarTrack, Maxted et al (2020) found three different binary evolution paths that could lead to a low-mass X-ray binary or IMXB in an SNR. The evolutionary paths start with a ∼25 M e primary and ∼3 M e companion, and result in a system with a 5-11 M e black hole and a companion with a mass of 2.6-4.5 M e (an A-or B-type star) in a very close orbit, such that mass transfer begins approximately τ ; 24,000 yr after the supernova.…”

Wind-powered ultraluminous X-ray sources

“…We note that, only in rare situations it is possible that the donor in a RLOF-powered ULX fills its RL immediately after the compact object formation as a result of favorably directed natal kick (see e.g. Maxted et al 2020), so that its MT phase can be the longest possible. In a typical case, the RL is filled only after the star expands as a result of nuclear evolution, typically shortly ( 100 Myr) before TAMS.…”