Spectropolarimetry of the tidal disruption event AT 2019qiz: a quasispherical reprocessing layer

TL;DR

This study uses spectropolarimetry to reveal the structure and evolution of the reprocessing layer in the tidal disruption event AT 2019qiz, showing a large, nearly spherical scattering photosphere that recedes over time.

Contribution

First spectropolarimetric evolution observed in a TDE, providing new insights into the geometry and dynamics of the reprocessing layer around the black hole.

Findings

Continuum polarization was 0% at peak brightness and increased to ~1% after 29 days.

The scattering photosphere is approximately 100 au, much larger than the tidal and thermalization radii.

Polarization changes over time indicate a receding, aspherical interior and the formation of the Hα line near the scattering radius.

Abstract

We present optical spectropolarimetry of the tidal disruption event (TDE) AT 2019qiz on days $+0$ and $+29$ relative to maximum brightness. Continuum polarization, which informs the shape of the electron-scattering surface, was found to be consistent with 0 per cent at peak brightness. On day $+29$, the continuum polarization rose to $\sim 1$ per cent, making this the first reported spectropolarimetric evolution of a TDE. These findings are incompatible with a naked eccentric disc that lacks significant mass outflow. Instead, the spectropolarimetry paints a picture wherein, at maximum brightness, high-frequency emission from the accretion disc is reprocessed into the optical band by a nearly spherical, optically thick, electron-scattering photosphere located far away from the black hole. We estimate the radius of the scattering photosphere to be $\sim 100\rm\, au$ at maximum brightness -- significantly larger than the tidal radius ($\sim 1\rm\, au$) and the thermalisation radius ($\sim 30\rm\, au$) where the optical continuum is formed. A month later, as the fallback rate drops and the scattering photosphere recedes, the continuum polarization increases, revealing a moderately aspherical interior. We also see evidence for smaller-scale density variations in the scattering photosphere, inferred from the scatter of the data in the Stokes $q-u$ plane. On day $+29$, the H$\alpha$ emission-line peak is depolarized to $\sim 0.3$ per cent (compared to $\sim 1$ per cent continuum polarization), and displays a gradual rise toward the line's redder wavelengths. This observation indicates the H$\alpha$ line formed near the electron-scattering radius.