A search for pulsars in subdwarf B binary systems and discovery of giant-pulse emitting PSR J0533-4524

TL;DR

This study searched for millisecond pulsars in subdwarf B binary systems, found no pulsars in the targets but discovered a field pulsar, and discussed implications for pulsar detection and system orientation.

Contribution

Performed targeted radio searches in sdB binaries, set upper limits on pulsar presence, and identified a new pulsar in the field, providing insights into system orientations and pulsar properties.

Findings

No pulsations detected in six sdB systems down to 0.11 mJy sensitivity.

Discovered a new pulsar J0533-4524 in the field, not associated with sdB systems.

Constraints on the number of pulsars in the studied systems and implications for system geometry.

Abstract

Binary millisecond pulsars (MSPs) provide several opportunities for research of fundamental physics. However, finding them can be challenging. Several subdwarf B (sdB) binary systems with possible neutron star companions have been identified, allowing us to perform a targeted search for MSPs within these systems. Six sdBs with companions in the neutron star mass range, as determined from their optical light curves, were observed with the Green Bank and Westerbork radio telescopes. The data were searched for periodic signals as well as single pulses. No radio pulsations from sdB systems were detected, down to an average sensitivity limit of 0.11 mJy. We did, however, discover a pulsar in the field of sdB HE0532-4503. Follow-up observations with the Giant Metrewave Radio Telescope showed that this pulsar, J0533-4524, is not spatially coincident with the sdB system. The pulsar has a relatively low magnetic field but still emits giant pulses. We place an upper limit of three to the number of radio pulsars in the six sdB systems. The non-detections may be explained by a combination of the MSP beaming fraction, luminosity, and a recycling fraction <0.5. Alternatively, the assumption of co-rotation between the MSP and sdB may break down, which implies the systems are more edge-on than previously thought. This would shift the predicted companion masses into the white dwarf range. It would also explain the relative lack of edge-on sdB systems with massive companions.