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University of Cambridge
Institute of Astronomy
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23.5m space telescope
soyuz telescope image

SUPER-SHARP: Space-based Unfolding Primary for Exoplanet  Research via Spectroscopic High Angular Resolution Photography
    The top picture on the left shows a concept for a 23.5m telescope that can fit into the 4.57m diameter fairing of an Ariane 6 rocket. To see how such a large telescope can fit into an Ariane 6 go to Youtube animation #1. Each of the 4 mirrors in the cross-shaped primary is 10m x 2.8m. The picture underneath shows another version of SUPERSHARP that fits in a Soyuz rocket fairing. The primary mirror for this is 24x3.3m (see Youtube animation #2). SUPER-SHARP will directly image exoplanets and its instrumentation includes active mirror control, a coronograph (to remove the light from the central star for exoplanet observations) and an integral field spectrograph (to give R=100 spectra for every pixel in the 2x2 arcsec FOV). The 23.5m mirror baseline gives an inner working angle (IWA) of 16 mas at 750nm with 8 mas spatial resolution and an IWA of just 2.7 mas at ultra-violet wavelengths.

    The SUPER-SHARP design philosophy is to push extremely hard on spatial resolution and IWA while at the same time keeping within an affordable budget. SUPER-SHARP will therefore maximise primary mirror baseline, use the shortest possible operating wavelength and be pragmatic about everything else (number of instruments, field of view, thermal management, raw speckle contrast, etc.). Some mirror deployment strategies (i.e unfolding mechanisms) can achieve even greater baselines than 23m.

    The mission's main science goals are:
    • Carry out a "quick-look" reconnaissance of the ~500-1000 stars with the most readily observed habitable zones (HZ) making a census (including spectroscopy) of the number of Earths, Super-Earths, Neptunes and Jupiters in each system.
    • Directly image many exoplanets already discovered through the radial velocity technique (e.g the "hot Jupiter", Ups And b) or by GAIA. The hot-jupiter science is enabled by the very small IWA.
    • Do deep follow-up imaging and spectroscopy of the most interesting ~50-100 systems to thoroughly characterise them chemically, physically and dynamically. For a subset of these, with Earth-like planets in their HZ, this will include looking for the A-band oxygen bio-signature.
The telescope will also, of course, be very powerful for many other non-exoplanet programs.

    HR8799 P1640 S4 map
    This is a near infrared integral-field spectrograph placed behind a high order AO system and a coronograph for direct imaging-spectroscopy of faint stellar companions including self-luminous extra-solar planets. P1640 is currently operational on the 5m Hale telescope at the Palomar Observatory. The top picture on the left shows our detection of all 4 of the known exoplanets orbiting the star HR8799. The second picture shows the P1640 spectra we obtained for these exoplanets. See Oppenheimer et al, 2013, Ap J, 768 for details. P1640 is a collaboration between the American Museum of Natural History, New York (PI: Rebecca Oppenheimer), Caltech, JPL and the IoA. Eleanor Bacchus is my PhD student at the IoA working on P1640.

MOONS image
    MOONS is a NIR fibre-fed multi-object spectrograph for the VLT. It will have 1024 fibres, a FOV of 25 arcmins diameter, spectral resolutions between R=4000 and R=20000 and a wavelength coverage of 0.8 to 1.8 microns. The project recently passed its preliminary design review and the next steps are detailed design and construction. This project is led by the UKATC (PI: Michele Cirasuolo). My MOONS collaborators in Cambridge are Roberto Maiolino, Chris Haniff, David Buscher, Martin Fisher and David Sun. Science drivers for MOONS include galactic archaeology (especially the obscured bulge), Galaxy evolution at z>1, reionisation z>~7 and cosmology via RSD at z>1.

    MOONS description paper.

    MOONS updated optical design paper.


This is the high resolution spectrograph for the European Extremely Large Telescope. Currently the project is in the conceptual design phase. There are numerous science drivers but the key ones are:
    • Exoplanet transit spectroscopy (including the possibility of detecting life)
    • Looking for the chemical signature of population-III stars
    • Cosmology and fundamental physics

My HIRES collaborators in Cambridge are Roberto Maiolino, Didier Queloz, Martin Haehnelt, Max Pettini, Chris Haniff, David Buscher, Martin Fisher and David Sun.


           Last updated on Feb 11th 2016.