Precise cosmological measurements coupled with astronomical evidence has allowed us to piece together a model of the Universe that explains much of what we observe. This model is known as the ΛCDM model and tells us that we live in an inflationary universe that is made up of contributions from 'Dark Energy' (68%), responsible for the accelerating expansion of the Universe, baryonic 'normal' matter (5%), and a 'Dark Matter' component, which makes up the remaining 27%. However, the nature of the dark elements remains unknown and consequently, fundamental questions still cloud the model. From both astrophysical and particle physics considerations, stable and heavy Weakly Interacting Massive Particle (WIMP) candidates that arise naturally from extensions to the Standard Model of particle physics are particularly compelling.
WIMPs, interacting with regular matter only very rarely, would satisfy the requisite abundance today, be stable on the timescales of the Universe, and would have been non-relativistic at the time of decoupling - providing the gravitational seeds for large scale structure formation. Its presence today acts as the glue holding galaxies such as our own together. Confirmation of the WIMP hypothesis would cast light not only on Beyond Standard Model physics and extrapolation to GUT scales, but would considerably advance our understanding of the matter composition and evolution of the Universe. For these reasons, the discovery of Dark Matter has been identified as among the most important scientific missions of the 21st century.
Three avenues are presently pursued with the aim to identify Dark Matter: indirect, accelerator, and direct searches. Indirect methods deploy space-based and terrestrial instruments to search for signals from decay products following WIMP annihilations in regions of high density. Accelerator searches such as at the LHC seek to achieve sufficient collision energies to be able to produce WIMPs and observe missing reconstructed energy in the final states to infer their mass. However, neither of these techniques is by itself capable of providing a robust statement on the nature of Dark Matter. Expected annihilation signatures from indirect searches are easily mimicked by standard sources, and accelerator searches cannot address stability of the inferred particles and conclude that they represent galactic WIMPs. Instead, it is direct observation of WIMPs within our own Milky Way that is recognised as the definitive channel for detection. Internationally, meeting this challenge and detecting galactic WIMPs is recognised as one of the highest priorities in science, featuring often above all else in roadmaps and research recommendations worldwide.
Direct Dark Matter Searches
Galactic rotation curves suggest the Dark Matter forms an extended halo around galaxies such that our solar system, moving through this halo, is exposed to an apparent flux of WIMPs. These WIMPs may be directly detected by recording the energy deposition made by a recoiling nucleus following a WIMP scatter. However, given the kinematics, the recoil would generate energies of only a few keV. Moreover, the event rate is dictated by the coupling of a Dark Matter particle through the Weak force, resulting in extremely rare signals. Experiments must, therefore, operate detectors with very low thresholds, very low intrinsic and external radiological background, located in deep underground sites shielded from cosmic rays. Despite these challenges, several technologies have been developed and deployed successfully over the past 30 years in attempts to be the first to discover WIMPs. Where no signal has been detected, constraints on the WIMP-nucleon interaction cross-section have been derived. As yet, no unambiguous discovery of Dark Matter has been made.
Here at UCL we work on the leading experiments in the search for Dark Matter. These experiments use liquified noble gas targets, operated as two-phase time projection chambers. Such technology has rapidly accelerated the race for Dark Matter over recent years, with xenon detectors in particular dominating the field and emerging as the most promising detector technology for a first detection. At this very moment the LUX detector, containing 350 kg of ultra-pure liquid xenon, is operating underground in the Homestake Mine in S. Dakota, USA. Building on the progress with the technology to-date, LUX is the most sensitive detector in the hunt for Dark Matter particles, having demonstrated world-leading sensitivity with results from its very first exposure of only 85 days in 2013.
Within the LUX-ZEPLIN (LZ) project we are developing a detector with a mammoth 7 tonnes of liquid xenon to provide unrivalled search capability for Dark Matter. It will be housed using the same infrastructure as LUX at Homestake, and will have the sensitivity to sweep virtually all the theoretically favoured parameter space for WIMPs. LZ will have the power to confirm any detection or hint thereof from LUX with a statistically significant result, or return the world's definitive positive result to solve the Dark Matter problem.
We are also conducting leading R&D to tackle the challenges for the next generation of detectors and multi-tonne noble liquid observatories. This includes measurements of the fundamental properties of liquid xenon and argon - particularly light and charge generation mechanisms at low energies; development of ultra-low background photosensors; novel solutions for high voltage operation and charge transport; and development of low background material screening techniques.
For more information on any of the activities of the Dark Matter Group at UCL, please contact Dr. Chamkaur Ghag.