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Cardiff University Astronomical Instrumentation Peter Ade Walter Gear Matt Griffin Philip Mauskopf

Cardiff University Astronomical Instrumentation Peter Ade Walter Gear Matt Griffin Philip Mauskopf Enzo Pascale Carole Tucker. Group Programme of Work. • Development of underlying technologies - TES detectors, KIDs, filters and optics

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Cardiff University Astronomical Instrumentation Peter Ade Walter Gear Matt Griffin Philip Mauskopf

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  1. Cardiff University Astronomical Instrumentation Peter Ade Walter Gear Matt Griffin Philip Mauskopf Enzo Pascale Carole Tucker

  2. Group Programme of Work • • Development of underlying technologies - TES detectors, KIDs, filters and optics • • Development of new instruments and techniques (integration vs. underlying technology) • Support of instrument AIV and operations • Main instrument focus - SCUBA2, CLOVER, PLANCK-HFI, HERSCHEL-SPIRE, SPICA-SAFARI, BOLOCAM/AzTEC, BLAST-Pol • + support of observations and data analysis • I.e. science exploitation • Over 40 staff and students in the group

  3. TES detectors • Facilities for optical characterisation of sub arrays - SAFARI (30 - 200 m) - SCUBA2 (450 - 850 m) - CLOVER (1400 - 3000 m) P. Ade, P. Mauskopf, D. Morozov SiN leg 5 m TES 110 m

  4. Readouts and Multiplexing • • Micromachined bolometers use CMOS multiplexed readout  can have 1000’s of pixels • Cryogenic TES bolometers (SCUBA2, CLOVER) use multiplexed SQUID readout  can have 1000’s of pixels BUT SQUID and CMOS multiplexing is complicated • Is there a simpler way to multiplex sensitive cryogenic bolometers? RF resonator readout - lots of signals on one coaxial cable Superconductors have low loss at low (readout) frequencies and high loss (absorption/detection) at THz frequencies

  5. KIDs • • New technology for large format arrays • Detectors and cold electronics simple to fabricate, small number of cables (up to 1000 detectors per coaxial cable) • Most difficult part the warm readout electronics (wide bandwidth) • Cardiff activities on KIDs: • LEKID design - Readout, optical coupling • KID test bed - cryo free • Starting work on readout electronics • Ongoing collaboration with Cambridge, SRON, Grenoble, Rome, Trento • P. Mauskopf, A. Porch, S. Doyle, C. Dunscombe

  6. Photons break Cooper pairs and change kinetic inductance Produces frequency shift in LC resonator (few GHz) Multiplexable High sensitivity Easy to fabricate … R LOSS Kinetic Inductance Detectors + L L K M

  7. Lumped element superconducting resonators Microwave model of a lumped element superconducting resonator

  8. LeKIDs fabricated and tested at Cardiff(They work)

  9. First light - 1.5 THz on a LEKID

  10. Filters • • Cardiff provides filters for most mm-wave astronomical instruments • e.g. SCUBA2, PLANCK-HFI, HERSCHEL-SPIRE, BOLOCAM, SPT, ACT, APEX-SZ, etc. • These include low pass filters, band defining filters and NIR/optical thermal filters for all temperature stages • The filter combinations are designed to minimise heat load on the cryogenic system, stray light on the detectors and maximise optical efficiency

  11. Other optical components • • Cardiff can also provide antireflection coatings of warm and cold lenses and windows • Cardiff can also provide waveplate modulators and wire grid (hot pressed) polarisers for polarisation experiments • Cardiff can provide possible other attachments such as input FTS • RF modelling, e.g. for optimisation of detector coupling and optics and stray light - HFSS, ZeMAX, GRASP - designed warm coupling optics for BOLOCAM and AzTEC and cold coupling optics for BOOMERANG, BLAST and OLIMPO P. Ade, P. Hargrave, P. Mauskopf, J. Zhang

  12. Instrument support • • Experience in instrument AIV and integration of receivers and telescopes - BOLOCAM, AzTEC, CLOVER, SCUBA2, etc. • Quick look software programming • Atmospheric removal algorithms

  13. BOLOCAM 2 (AzTEC) • Original plan - 2 BOLOCAMs • Second camera now complete - called AzTEC • Integrated on JCMT in June, 2005; observing run November - December 2005 +? • Eventually to be integrated on 50 m LMT

  14. BLAST • Test flight from Ft. Sumner, NM (2003) - 500 m array only • LDB flights from Kiruna (2005) and McMurdo (2006) - 250, 350 and 500 m arrays • Data analysis underway Sensitivity/resolution limited by optics in flight Lots of data on galactic and extragalactic sources • Cardiff participation in flight preparation, optics and filters and data analysis. (The instrument focal plane was built at Cardiff)

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