Constraints to neutron-star kicks in high-mass X-ray binaries with Gaia EDR3^⋆

¹ Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France
e-mail: fortin@apc.in2p3.fr
² Instituto Argentino de Radioastronomía (CCT La Plata, CONICET, CICPBA, UNLP), C.C.5, (1894) Villa Elisa, Buenos Aires, Argentina

Received: 22 March 2021
Accepted: 7 June 2022

Abstract

Context. All neutron star progenitors in neutron-star high-mass X-ray binaries (NS HMXBs) undergo a supernova event that may lead to a significant natal kick impacting the motion of the whole binary system. The space observatory Gaia performs a deep optical survey with exquisite astrometric accuracy, for both position and proper motions, that can be used to study natal kicks in NS HMXBs.

Aims. Our aim is to survey the observed Galactic NS HMXB population and to quantify the magnitude of the kick imparted onto their NSs, and to highlight any possible differences arising between the various HMXB types.

Methods. We performed a census of Galactic NS HMXBs and cross-matched existing detections in X-rays, optical, and infrared with the Gaia Early Data Release 3 database. We retrieved their parallaxes, proper motions, and radial velocities (when available), and performed a selection based on the quality of the parallax measurement. We then computed their peculiar velocities with respect to the rotating reference frame of the Milky Way, and including their respective masses and periods, we estimated their kick velocities through Markov chain Monte Carlo simulations of the orbit undergoing a supernova event.

Results. We infer the posterior kick distributions of 35 NS HMXBs. After an inconclusive attempt at characterising the kick distributions with Maxwellian statistics, we find that the observed NS kicks are best reproduced by a gamma distribution of mean 116₋₁₅₊₁₈ km s⁻¹. We note that supergiant systems tend to have higher kick velocities than Be HMXBs. The peculiar velocity versus non-degenerate companion mass plane hints at a similar trend, supergiant systems having a higher peculiar velocity independently of their companion mass.