Optical and near-infrared polarization of the black hole X-ray binary A0620-00 in quiescence

TL;DR

This study presents high-precision optical and near-infrared polarimetric observations of the black hole X-ray binary A0620-00 in quiescence, revealing variable intrinsic polarization linked to orbital motion and complex wavelength-dependent polarization behavior.

Contribution

It provides the first detailed analysis of intrinsic polarization variability and wavelength dependence in A0620-00, suggesting multiple polarized components and magnetic field estimates.

Findings

Intrinsic polarization varies with orbital period (~0.3% in R band).

Polarization angle rotates from infrared to blue (~53°).

Magnetic field in the plasma is estimated to be a few Gauss.

Abstract

We present simultaneous high-precision optical polarimetric and near-infrared (NIR) to ultraviolet (UV) photometric observations of low-mass black hole X-ray binary A0620-00 in the quiescent state. Subtracting interstellar polarization, estimated from a sample of field stars, we derive the intrinsic polarization of A0620-00. We show that the intrinsic polarization degree (PD) is variable with the orbital period with the amplitude of $\sim0.3\%$ at least in the $R$ band, where the signal-to-noise ratio of our observations is the best. This implies that some fraction of the optical polarization is produced by a scattering of stellar radiation off the matter that follows the black hole in its orbital motion. In addition, we see a rotation of the orbit-average intrinsic polarization angle (PA) with the wavelength from $163\deg$ in the $R$ to $177\deg$ in the $B$ band. All of the above, combined with the historical NIR-to-optical polarimetric observations, demonstrates the complex behavior of the average intrinsic polarization of A0620-00: the PA continuously rotates from the infrared to the blue band by $\sim53\deg$ in total, while the PD of $\sim1\%$ remains nearly constant over the entire spectral range. The spectral dependence of the PA can be described by Faraday rotation with the rotation measure of RM=$-0.2$ rad $\mu$m$^{-2}$, implying a few Gauss magnetic field in the plasma surrounding the black hole accretion disk. However, our preferred interpretation of the peculiar wavelength dependence is an interplay between two polarized components with different PAs. Polarimetric measurements in the UV range can help in distinguishing between these scenarios.