Evidence for mass-dependent peculiar velocities in compact object binaries: Towards better constraints on natal kicks

Abstract

We compile a catalogue of low-mass and high-mass X-ray binaries, some recently reported binaries that likely host a neutron star (NS) or a black hole (BH), and binary pulsars (a pulsar and a non-degenerated companion) that have measured systemic radial velocities ($\gamma$). Using Gaia and radio proper motions together with $\gamma$, we integrate their Galactic orbits and infer their post-supernova (post-SN) 3D peculiar velocities ($v_{\mathrm{pec}}^{z=0}$ at Galactic plane crossing); these velocities bear imprint of natal kicks that compact objects received at birth. With the sample totalling 85 objects, we model the overall distribution of $v_{\mathrm{pec}}^{z=0}$ and find a two-component Maxwellian distribution with a low- (${\sigma }_v\approx 21\mathrm{km}{\mathrm{s}}^{-1}$) and a high-velocity (${\sigma }_v\approx 107\mathrm{km}{\mathrm{s}}^{-1}$) component. A further comparison between distributions of binary subgroups suggests that binaries hosting high-mass donors/luminous companions mostly have $v_{\mathrm{pec}}^{z=0}\lesssim 100\mathrm{km}{\mathrm{s}}^{-1}$, while binaries with low-mass companions exhibit a broader distribution that extends up to $\sim 400\mathrm{km}{\mathrm{s}}^{-1}$. We also find significant anti-correlations of $v_{\mathrm{pec}}^{z=0}$ with binary total mass ($M_{\mathrm{tot}}$) and orbital period ($P_{\mathrm{orb}}$), at over 99% confidence. Specifically, our fit suggests $v_{\mathrm{pec}}^{z=0}\propto M_{\mathrm{tot}}^{-0.5}$ and $v_{\mathrm{pec}}^{z=0}\propto P_{\mathrm{orb}}^{-0.2}$. Discussions are presented on possible interpretation of the correlations in the context of kinematics and possible biases. The sample should enable a range of follow-up studies on compact object binary kinematics and evolution.

arXiv comment26 pages, 14 figures, 8 tables, resubmitted to MNRAS after first revision

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