Polarization in microlensing towards the Galactic bulge

TL;DR

This paper evaluates the polarization signals during microlensing events towards the Galactic bulge, suggesting that current technology could detect these signals, which vary with source star type and magnification.

Contribution

It provides the first detailed estimates of polarization signals in microlensing events for different star types and assesses their detectability with existing instruments.

Findings

Polarization signals can reach up to 0.04% for late type stars.

Signals can be a few percent for cool giants.

Detection is feasible with current polarimeters like FORS2 on VLT.

Abstract

Gravitational microlensing, when finite size source effects are relevant, provides an unique tool for the study of source star stellar atmospheres through an enhancement of a characteristic polarization signal. This is due to the differential magnification induced during the crossing of the source star. In this paper we consider a specific set of reported highly magnified, both single and binary exoplanetary systems, microlensing events towards the Galactic bulge and evaluate the expected polarization signal. To this purpose, we consider several polarization models which apply to different types of source stars: hot, late type main sequence and cool giants. As a result we compute the polarization signal P,which goes up to P=0.04% for late type stars and up to a few percent for cool giants, depending on the underlying physical polarization processes and atmosphere model parameters. Given a I band magnitude at maximum magnification of about 12, and a typical duration of the polarization signal up to 1 day, we conclude that the currently available technology, in particular the polarimeter in FORS2 on the VLT, potentially may allow the detection of such signals. This observational programme may take advantage of the currently available surveys plus follow up strategy already routinely used for microlensing monitoring towards the Galactic bulge (aimed at the detection of exoplanets). In particular, this allows one to predict in advance for which events and at which exact time the observing resources may be focused to make intensive polarization measurements.