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Optical Lumped Element MKIDs

The Optical/UV MKID Team: UCSB: Ben Mazin, Sean McHugh, Kieran O’Brien, Seth Meeker, Erik Langman , Danica Marsden, Matt Strader Caltech : Jonas Zmuidzinas , Sunil Golwala , David Moore JPL: Bruce Bumble, Rick LeDuc. Optical Lumped Element MKIDs. Ben Mazin, February 2012.

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Optical Lumped Element MKIDs

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  1. The Optical/UV MKID Team: UCSB: Ben Mazin, Sean McHugh, Kieran O’Brien, Seth Meeker, Erik Langman, Danica Marsden, Matt Strader Caltech: Jonas Zmuidzinas, Sunil Golwala, David Moore JPL: Bruce Bumble, Rick LeDuc Optical Lumped Element MKIDs Ben Mazin, February 2012 Mazin Lab @ UCSB

  2. Microwave Kinetic Inductance Detectors Typical Single Photon Event MKID Equivalent Circuit Inductor is a Superconductor! Energy Gap Silicon – 1.10000 eV Aluminum – 0.00018eV Energy resolution: Cooper Pair

  3. SCI2-B: Demonstrated at Palomar! Mazin et al., Optics Express 2012

  4. Tapering Uniform Legs Rectangular Legs Trapezoidal Legs

  5. Measured @ 3500x Over or under etch of up to 100 nm, but leg widths consistent to 25 nm

  6. SCI2-B Energy Resolution • 20 nm TiN on Silicon • Tc = 0.8 K • QP lifetime ~ 50 μs • Qi ~ 1,000,000 • R=E/ΔE=16 at 254 nm • R limited by HEMT/power handling/Qi

  7. SCI-2B Uniformity

  8. Lessons Learned and Outstanding Questions • First MKID device with multiple feedlines (I think?) • Must have good ground planes or massive crosstalk • Floating finite CPW not OK! • Tc gradients cause resonator collisions – simulate your frequency coding scheme with gradients to avoid systematic collision issues • QP lifetime varies substantially, even on a single device. 20-100 microsecond spread! Strange! • Need more robust algorithms for setting up large arrays • Choosing resonators • Figuring out optimal powers

  9. ARCONS Overview Array Camera for Optical to Near-IR Spectrophotometery (ARCONS) First Light: July 28, 2011, Palomar 200” Coudé Lens coupled 1024 (32x32) pixel array in cryogen-free ADR (first lens coupled optical/nIR 100 mK instrument – learned a lot about IR blocking!) 0.2” pixels yields 7”x7” FOV Next run, 45x45 pixels with 0.4” plate scale yields 18”x18” FOV 400 nm to 1100 nm simultaneous bandwidth with maximum count rate of ~2000 cts/pixel/sec Next run, 350-1350 nm Energy resolution R~10-20 at 400 nm 50 Gbit/sec -> FPGA -> 32 Mbit/sec Entrance window

  10. Optics IR Blocking See Kieran O’Brien for Details 300K 4K 4K Dewar Lyot Reimaging Window Stop Optics 300K 3K (Lyot Stop) 100 mK

  11. Readout Crate Sean McHugh’s Talk Tomorrow

  12. To Palomar!

  13. 135 ft 16.67 ft ARCONS 5.67 ft

  14. ARCONS First Light Image

  15. Crab Pulsar Pulse profile measured with ARCONS Archival pulse profile for Crab (Shearer 2003)

  16. Dancing with the Stars

  17. Mega-z 6”x6” Macropixels (image not to scale) • Proposed Keck Nasmyth Instrument (dewar doesn’t tip past ~50 degrees, flexure concerns) • Uses an aperture mask in the focal plane to image objects of interest only • Maps one object to one MKID pixel • Sky subtraction done with empty Macropixels • Active mask alignment using feedback from science array • 10’x10’ or 12’ diameter FOV. 10,000 objects. • R~50 • mI< 26 • 0.32 – 1.35 μm (possibly up to 1.8 μm)

  18. Simulated Mega-Z Spectra

  19. Future Plans • Field ARCONS in fall (Lick) and winter (Palomar) with a 2025 pixel array • Detector Goals (Danica’s Talk): • Eliminate substrate events (already done?) • Increase energy resolution • Increase uniformity • Increase QE

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