Near-infrared polarization images of the Orion proplyds

TL;DR

This study uses high-resolution near-infrared polarimetric imaging and simulations to map circumstellar material and constrain disk parameters of Orion proplyds, revealing limitations of simple dust models and demonstrating the effectiveness of polarimetric techniques.

Contribution

It introduces AO-assisted high-resolution polarimetry combined with 3D radiation transfer simulations to analyze Orion proplyds, providing new insights into disk structures and dust properties.

Findings

Polarimetric imaging maps circumstellar material despite limited resolution.

Larger grain models do not match observed polarization spectra.

Polarimetric differential imaging is effective for studying proplyd structures.

Abstract

We performed AO-assisted high-resolution imaging polarimetry on selected Orion proplyds close to the Trapezium stars in the J, H, and K bands. Differential polarimetric images of one of the largest and brightest proplyds are interpreted using 3D radiation transfer simulations based on the Monte Carlo method. Although not fully resolvable by ground-based observations, the circumstellar material can be mapped with polarimetry. We present constraints on the disk parameters of the giant proplyd 177-341. We tested whether dust models with different grain size distributions could explain the observed extent of the polarization patterns and find that simple models with larger grains will not reproduce the spectral polarization behavior. The technique of polarimetric differential imaging (PDI) in the NIR provides a good opportunity to study the structure of the Orion proplyds.