An X-ray-quiet black hole born with a negligible kick in a massive binary within the Large Magellanic Cloud

Shenar, T.; Sana, H.; Mahy, L.; El-Badry, Kareem; Marchant, Pablo; Langer, N.; Hawcroft, C.; Fabry, M.; Sen, K.; Almeida, L. A.; Abdul-Masih, M.; Bodensteiner, J.; Crowther, P. A.; Gieles, M.; Gromadzki, M.; Hénault-Brunet, V.; Herrero, A.; Koter, A. de; Iwanek, Patryk; Kozłowski, S.; Lennon, D. J.; Apellániz, J. Maíz; Mróz, P.; Moffat, A. F. J.; Picco, Annachiara; Pietrukowicz, P.; Poleski, R.; Rybicki, K.; Schneider, F. R. N.; Skowron, D. M.; Skowron, J.; Soszyński, I.; Szymański, M. K.; Toonen, Silvia; Udalski, A.; Ulaczyk, K.; Wrona, Marcin

doi:10.1038/s41550-022-01730-y

Cited by 40 publications

(65 citation statements)

References 87 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…obeys the contidition that its CO core mass > 1.38 M ) we draw 2000 kicks and record the models that remain bound. In addition we also consider a rotational velocity criteria as the O star in VFTS 243 was inferred to have a spin velocity at least 180 km s −1 (Shenar et al 2022a). The original STARS models in BPASS do not take into account rotation in the evolution of the stellar interior (although it is considered in the orbital evolution).…”

Section: Models and Numerical Methodsmentioning

confidence: 99%

“…The VFTS 243 system however seems to be the first undisputed discovery of a quiescent BH in a stellar binary. Reported by Shenar et al (2022a), it is found to be an O7+BH in the 30 Doradus region. The very precise measurements of the orbital components (P = 10.4031 ±0.0004 days, e = 0.017 ±0.012) and extensive observational data surrounding this object have the potential to provide improved observational constraints or clues on a number of bottle-★ E-mail: hfstevance@gmail.com necks in stellar evolution theory such as natal supernova (SN) kicks and the genealogies of the progenitor systems of BH+BH binaries.…”

Section: Introductionmentioning

confidence: 96%

“…In the supplementary material of the VFTS 243 BH discovery paper, Shenar et al (2022a) present an exemplar system calculated with (Paxton et al 2011(Paxton et al , 2013(Paxton et al , 2015(Paxton et al , 2018(Paxton et al , 2019 to show a possible progenitor route to the formation of VFTS 243-like objects. The flexibility of allows observational parameters to be reproduced rather nicely (generally speaking and in the case of VFTS 243) but in order to truly understand the most likely genealogies of such systems population synthesis is required.…”

Section: Introductionmentioning

confidence: 99%

“…In this work we search the fiducial BPASS models for predictions of VFTS243-like systems and compare our genealogies to those of the exemplar model presented in Shenar et al (2022a). In addition we investigate the natal kick velocities that best reproduce the orbital configuration of VFTS 243 and compare these to commonly used natal kick prescriptions for BH remnants.…”

Section: Introductionmentioning

confidence: 99%

“…In Section 2 we describe our models and numerical methods; in Section 3 we show our posterior kick velocities and best genealogies to VFTS 243 as predicted by BPASS. In Section 4 we discuss the differences between our channel and the model in Shenar et al (2022a), as well as the implications of our kick posteriors. Finally we summarise and conclude in Section 5.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

VFTS 243 as predicted by the BPASS fiducial models

Stevance¹,

Ghodla²,

Richards³

et al. 2022

Preprint

View full text Add to dashboard Cite

The recent discovery of an unambiguous quiescent BH and main sequence O star companion in VFTS 243 opens the door to new constraints on theoretical stellar evolution and population models looking to reproduce the progenitors of black hole -black hole binaries. Here we show that the Binary Population and Spectral Synthesis fiducial models (BPASSv2.2.1) natively predict VFTS 243-like systems: We find that VFTS 243 likely originated from a binary system in a ∼15 day orbit with primary mass ranging from 40 to 50 M and secondary star with initial mass 24-25 M . Additionally we find that the death of the primary star must have resulted in a low energy explosion 𝐸 < 10 50 ergs. With a uniform prior we find that the kick velocity of the new-born black hole was < 33 km s −1 (90 percent credible interval). The very low eccentricity reported for VFTS 243 and the subsequent conclusion by the authors that the SN kick must have been very small is in line with the peak in the posterior distribution between 0 and 5 km s −1 . Finally, the reduced Hobbs kick distribution commonly used in black hole population synthesis is strongly disfavoured, whereas the Bray kick with the most recent parameter calibration predicts 2 ± 3.5 km s −1 , which is very consistent with the posterior velocity distributions obtained for our matching VFTS 243-like models using a uniform kick prior.

show abstract

Section: Models and Numerical Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%