# Wide binary companions to massive stars and their use in constraining natal kicks

## TL;DR

This study uses Gaia data to analyze ultra-wide massive star binaries and explores their potential to constrain natal kicks of neutron stars and black holes, finding a modest binary fraction and no confirmed ultra-wide companions to compact objects.

## Contribution

It characterizes the frequency of ultra-wide binaries among massive stars and proposes a novel method to constrain natal kicks of neutron stars and black holes using wide binary survival.

## Key findings

- Ultra-wide multiplicity fraction of 4.4% among massive stars.
- Expected wide-binary fraction of ~27% extrapolated to lower masses.
- No confirmed ultra-wide companions to neutron stars or black holes.

## Abstract

The origin of ultra-wide massive binaries (orbital separations $10^3-2\times 10^5$~AU) and their properties are not well characterized nor understood. Here we use the second Gaia data release to search for wide astrometric companions to Galactic O-B5 stars which share similar parallax and proper motion with the primaries. Using the data we characterize the frequency and properties of such binaries. We find an ultra-wide multiplicity fraction of $4.4\pm0.5$ per cent, to our completeness limit (up to $\approx 17$~mag; down to G-stars at distances of 0.3-2~kpc, excluding stars in clusters). The secondary mass-function is generally consistent with a Kroupa initial stellar function; if extrapolated to lower mass companion stars we then might expect a wide-binary fraction of $\sim 27\pm5\%$. In addition we use these data as a verification sample to test the existence of ultra-wide binaries among neutron stars (NSs) and black holes (BHs). We propose that the discovery of such binary can provide unique constraints on the weakest natal kicks possible for NSs/BHs. If a compact object is formed in an ultra-wide binary and receives a very-low natal kick, such a binary should survive as a common proper motion pair. We therefore use Gaia data to search for ultra-wide companions to pulsars (normal and millisecond ones) and X-ray binaries. We find no reliable pairs. Future data could potentially provide stringent constraints through this method.