Identification of the High-Energy Gamma-Ray Source 3FGL J1544.6-1125 as a Transitional Millisecond Pulsar Binary in an Accreting State

TL;DR

This paper identifies the gamma-ray source 3FGL J1544.6-1125 as a transitional millisecond pulsar binary in an accreting state, based on multi-wavelength observations showing accretion signatures and variability similar to known systems.

Contribution

It provides the first detailed multi-wavelength characterization linking the gamma-ray source to a transitional millisecond pulsar binary in an accreting state, expanding the known population.

Findings

X-ray and optical variability consistent with accretion states

Identification of the source as a transitional millisecond pulsar binary

First association of this gamma-ray source with an accreting pulsar system

Abstract

We present X-ray, ultraviolet, and optical observations of 1RXS J154439.4-112820, the most probable counterpart of the unassociated Fermi LAT source 3FGL J1544.6-1125. The optical data reveal rapid variability, which is a feature of accreting systems. The X-rays exhibit large-amplitude variations in the form of fast switching (within ~10 s) between two distinct flux levels that differ by a factor of $\approx$10. The detailed optical and X-ray behavior is virtually identical to that seen in the accretion-disk-dominated states of the transitional millisecond pulsar binaries PSR J1023+0038 and XSS J12270-4859, which are also associated with $\gamma$-ray sources. Based on the available observational evidence, we conclude that 1RXS J154439.4-112820 and 3FGL J1544.6-1125 are the same object, with the X-rays arising from intermittent low-luminosity accretion onto a millisecond pulsar and the $\gamma$-rays originating from an accretion-driven outflow. 1RXS J154439.4-112820 is only the fourth $\gamma$-ray emitting low-mass X-ray binary system to be identified and is likely to sporadically undergo transformations to a non-accreting rotation-powered pulsar system.