We are strongly involved in the Atacama Large Millimetre Array (ALMA) – a worldwide collaborative project to build a high-resolution millimetre-wave telescope in Chile.
The primary goal of the AMI Digital Correlator (AMIDC) project is to equip the AMI telescope with a highly channelized digital correlator system giving more flexibility in the location of this band and a much more uniform response across it.
The CAMbridge Emission Line Surveyor (CAMELS) is a pathfinder program to demonstrate on-chip spectrometry at millimetre wavelengths. CAMELS will observe at frequencies from 103–114.7GHz, providing 512 channels with a spectral resolution of R = 3000.
The CHaracterizing ExOPlanet Satellite (CHEOPS) will be the first mission dedicated to search for transits by means of ultrahigh precision photometry on bright stars already known to host planets.The CHEOPS project is a partnership between european team members, including the University of Cambridge.
Our pioneering work in optical interferometry has led to our group being partners in the development and construction of a major new instrument, the Magdalena Ridge Optical Interferometer (MROI) being constructed in New Mexico.
We are heavily involved in the technical and scientific activities of MOONS,
the near-IR multi-object spectrograph selected by ESO as third generation instrument for the Very Large Telescope.
The Next-Generation Transit Survey (NGTS) is a wide-field photometric survey designed to discover transiting Neptune-size and smaller exoplanets around bright stars (magnitude V<13). The NGTS project is a partnership between the University of Cambridge, Queen’s University Belfast, University of Warwick, University of Leicester, Observatoire de Geneve, DLR (Berlin) and Universidad Catolica de Chile.
A further major, and developing, area of the Group’s activity lies in our involvement in the Square Kilometre Array (SKA). This is a worldwide endeavour to create a telescope spanning frequencies from 50 MHz up to at least 10 GHz, with a total collecting area of more than 1 square kilometre, and with the possibility of simultaneous observation of many patches on the sky. Such a telescope would enable fundamental advances in many areas of astrophysics and cosmology. Alongside with our work on SKA we participate in the development of precursor and related telescopes. Currently our group is involved in the development of RAPID, a portable interferometer.
In this project we seek to exploit a novel liquid crystal technology, which allows a controllable true time delay to be applied to an RF signal of frequencies up to tens of GHz. The basic technology has already been demonstrated and has a wide variety of applications. We now intend to use this technology to construct a real astronomical demonstration system for delay lines and show that these can be integrated into the beamforming module of an existing Phased Array Feed (PAF) instrument, dramatically improving its capabilities.