Black holes and neutron stars (referred to as ‘compact objects’) are the end-products of stars which are at least eight times more massive than our Sun, and which die in a violent super-nova explosion. Unlike our Sun, the vast majority of stars live with a companion in a binary (though triple systems are also common). Should the supernova explosion -- which leaves behind the neutron star or black hole -- not tear the binary system apart, then we’re left with a compact object and ‘normal’ star orbiting around their common centre of mass. Over a very long period of time, the orbital separation of the binary can shrink and the compact object can accrete material from the companion star. This phase of accretion is only a very small fraction of the system’s lifetime, but has allowed us to locate ~30 binary systems containing black holes and 100-200 containing neutron stars. However, these numbers are dwarfed into insignificance when we consider that computer-based simulations of our Galaxy predict hundreds of thousands of binary systems should be present but not actively accreting. These black holes and neutron stars are surely out there, but how do we go about finding them?
When a foreground object such as a black hole or neutron star, passes in front of a much more distant, normal background star, we observe the effect of ‘micro-lensing’. Lensing more generally occurs due to the curvature of space-time caused by the mass of the compact object or ‘lens’ bending the paths of photons from the source such that the source appears to have a larger area and is therefore brighter. If we could observe a lens passing directly in front of a source we would observe what’s called an ‘Einstein ring’ and the time it spends passing in front of the source and acting as a lens, is called the ‘Einstein crossing time’. Microlensing is an important tool in modern astronomy as it can be used to constrain the nature of dark matter and even search for exoplanets.
A special case of lensing takes place when we observe a binary system containing a normal star and compact object, close to edge-on. As the compact object passes in front of its binary companion on an orbital period, the normal star’s light will be lensed and we will detect a characteristic periodic increase in the light (see Figure 1). If we can estimate the mass and radius of the normal star, then knowledge of the period and magnification leads us to a direct estimate for the mass of the compact object. This effect is called self-lensing and has been shown to work as white dwarfs have already ; the stage is now set to discover neutron stars and black holes which are not accreting and otherwise hidden from us.
Figure 1: The light from a star is magnified when the black hole passes in front of it. This creates a distinctive peak in the lightcurve.
SuperWASP is the Wide Angle Search for Planets; due to the combination of sky coverage (all latitudes above and below the Galactic plane), observing cadence (how regularly each star is observed) and long temporal baseline (the overall lengths of the lightcurves for each star) the archive is the ideal place to start searching for periodic lensing on the timescales of hours to years.
The signals you're looking for are extremely rare. Even though we think there are lots of hidden black holes in our galaxy, only a handful will be orbiting in a plane that means they pass in front of their companion star when viewed from the Earth using SuperWASP. The rarity of these perfectly aligned systems means we will be lucky if we find a handful of signals among the millions of stellar lightcurves that SuperWASP has assembled. So far, nobody has seen conclusive evidence of a self-lensing signal from a black hole. If you help to find one you will be making science history!
While you work on this project, you'll see a mixture of real and simulated subjects. We've included the simulated subjects for two reasons. The first is to give you examples of what shapes to look for in the SuperWASP data, so that you won't miss one of the extremely rare real lensing event when you see one. The second reason is that including simulated lightcurves lets us work out the lowest lensing magnification that should be detectable by Zooniverse volunteers.