Speckle Suppression Through Dual Imaging Polarimetry, and a Ground-Based Image of the HR 4796A Circumstellar Disk

TL;DR

This paper demonstrates how dual imaging polarimetry combined with adaptive optics significantly improves the detection sensitivity of circumstellar disks and planets by suppressing speckle noise, with a case study on HR 4796A.

Contribution

It introduces a novel application of polarimetric speckle suppression in ground-based imaging, achieving the first definitive near-IR polarimetric image of HR 4796A's debris disk.

Findings

Achieved 3-4 magnitudes greater sensitivity for polarized sources within 0.5 arcsec.

Detected the HR 4796A debris disk with 6.5 sigma significance in H-band.

Constrained disk properties including scale height and scattering asymmetry parameter.

Abstract

We demonstrate the versatility of a dual imaging polarimeter working in tandem with a Lyot coronagraph and Adaptive Optics to suppress the highly static speckle noise pattern--the greatest hindrance to ground-based direct imaging of planets and disks around nearby stars. Using a double difference technique with the polarimetric data, we quantify the level of speckle suppression, and hence improved sensitivity, by placing an ensemble of artificial faint companions into real data, with given total brightness and polarization. For highly polarized sources within 0.5 arcsec, we show that we achieve 3 to 4 magnitudes greater sensitivity through polarimetric speckle suppression than simply using a coronagraph coupled to a high-order Adaptive Optics system. Using such a polarimeter with a classical Lyot coronagraph at the 3.63m AEOS telescope, we have obtained a 6.5 sigma detection in the H-band of the 76 AU diameter circumstellar debris disk around the star HR 4796A. Our data represent the first definitive, ground-based, near-IR polarimetric image of the HR 4796A debris disk and clearly show the two outer ansae of the disk, evident in Hubble Space Telescope NICMOS/STIS imaging. We derive a lower limit to the fractional linear polarization of 29% caused by dust grains in the disk. In addition, we fit simple morphological models of optically thin disks to our data allowing us to constrain the dust disk scale height to 2.5{+5.0}_{-1.3} AU and scattering asymmetry parameter (g=0.20^{+.07}_{-.10}). These values are consistent with several lines of evidence suggesting that the HR 4796A disk is dominated by a micron-sized dust population, and are indeed typical of disks in transition between those surrounding the Herbig Ae stars to those associated with Vega-like stars.