Discovery of a variable energy-dependent X-ray polarization in the accreting neutron star GX 5-1

TL;DR

This study reports variable X-ray polarization in the neutron star GX 5-1, showing energy-dependent changes linked to the source's accretion state, and confirms polarization variation as a function of its position in the color-color diagram.

Contribution

First simultaneous multi-wavelength polarization measurements of GX 5-1, revealing energy-dependent X-ray polarization variation correlated with accretion states.

Findings

X-ray polarization degree varies between 1.8% and 3.7% depending on the accretion state.

Evidence of a ~20° variation in polarization angle with energy.

Polarization variation linked to different polarization angles of disk and Comptonization components.

Abstract

We report on the coordinated observations of the neutron star low-mass X-ray binary (NS-LMXB) \gx in X-rays (IXPE, NICER, Nustar and INTEGRAL), optical (REM and LCO), near-infrared (REM), mid-infrared (VLT VISIR), and radio (ATCA). This Z-source was observed by \IXPE twice in March-April 2023 (Obs. 1 and 2). In the radio band, the source was detected, but only upper-limits to the linear polarization were obtained at a $3\sigma$ level of $6.1\%$ at 5.5 GHz and $5.9\%$ at 9 GHz in Obs.~1 and $12.5\%$ at 5.5~GHz and $20\%$ at 9~GHz in Obs.~2. The mid-IR, near-IR and optical observations suggest the presence of a compact jet which peaks in the mid- or far-IR. The X-ray polarization degree was found to be $3.7\% \pm 0.4 \%$ (at $90\%$ confidence level) during Obs.~1 when the source was in the horizontal branch of the Z-track and $1.8\% \pm 0.4 \%$ during Obs.~2 when the source was in the normal-flaring branch. These results confirm the variation of polarization degree as a function of the position of the source in the color-color diagram as for previously observed Z-track sources (Cyg~X-2 and XTE~1701$-$462). Evidence for a variation of the polarization angle $\sim 20^\circ$ with energy is found in both observations, likely related to the different, non-orthogonal polarization angles of the disk and Comptonization components which peak at different energies.