Detectability of Self-Lensing Flares of White Dwarfs with Compact Companions

TL;DR

This paper introduces a simulation tool to analyze the detectability of self-lensing flares in white dwarf binary systems, assessing prospects for current and future sky surveys to identify these rare events and inform binary evolution models.

Contribution

It provides a new simulation method for self-lensing flare detection and evaluates survey sensitivities, highlighting the potential to discover many such systems with upcoming telescopes like LSST.

Findings

LSST could detect up to 247 double white dwarf systems

Current surveys have limited detection capabilities for these systems

Future surveys will significantly improve detection prospects

Abstract

Binaries containing compact objects, if viewed close to edge on, can produce periodic brightening events under certain conditions on the masses, radii, and binary separation. Such flares are caused by one object gravitational lensing the other, in what is known as self-lensing flares. We present a simulation tool that efficiently reproduces the main features of self-lensing flares and facilitates a detection sensitivity analysis for various sky surveys. We estimate the detection prospects for a handful of representative surveys when searching for systems of either two white dwarfs, or a white dwarf with other compact objects, i.e., neutron stars and black holes. We find only a marginal ability to detect such systems in existing surveys. However, we estimate many such systems could be detectable by surveys in the near future, including the Vera Rubin observatory. We provide a quantitative analysis of the detectability of double-compact object self-lensing flares across the landscape of system parameters, and a qualitative discussion of survey and followup approaches to distinguish such flares from confounding events, such as stellar flares, satellite glints, and cosmic rays. We estimate 0.3, 3 and 247 double white dwarf systems could be detected by TESS, ZTF, and LSST, respectively. A similar number of systems with a neutron star or black hole companion could be detected, but we caution that the number densities of such binaries is model dependent and so our detection estimates. Such binaries can be used to constrain models of the end states of binary evolution.