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Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology Gustavo Cancelo Fermilab Detector R&D Program Review 29 October 2014 MKIDs (Microwave Kinetic Inductance Devices) Pixelated micro-size resonator array.

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Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

Gustavo Cancelo Fermilab Detector R&D Program Review 29 October 2014

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MKIDs (Microwave Kinetic Inductance Devices)

  • Pixelated micro-size resonator array.
  • Superconducting sensors with meV energy gap. More than single photon detector:

– Can provide energy resolution (E/ΔE) in the visible and near infrared spectrum to do cosmology at large scale without filters and photon tagging with 1usec resolution. – Low resolution spectroscopy of >1 billion galaxies, QSO and other objects from DES & LSST data. (No other known instruments can do that). – High image rate: Allows for filtering of atmospheric fluctuations at ~100 Hz. – They must be operated at ~100mK degrees. – Need cold low noise amplifier at RF frequencies.

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A new challenge for superconducting detectors

  • Superconducting detectors have O (meV) energy gap.
  • Photons hitting a superconductor resonator will break

Cooper pairs into a few thousand quasi-particles.

  • Have been used for a long time in applications that require

few detectors.

  • The challenge is to build instruments with 10’s of thousands
  • f detectors in the near future and millions in a more distant

future.

  • The applications for such instruments include dark energy,

CMB, sub-mm science and more.

  • Note the potential science using both mid and large size

MKID instruments in the Astrophysics talks (this review).

10/28/2014 Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology 3

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  • Each pixel is tuned to a different frequency (frequency multiplexing).
  • Large array of superconducting detectors are NOW possible.
  • Channel separation ~2 MHz. Pixel bandwidth ~250 KHz

Equivalent circuit of a string of MKID resonators

Resonator’s Q ~35,000

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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MKID resonator

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  • Photons hit a pixel and move the resonance for that pixel.
  • We measure the dynamics of the phase/amplitude signal.
  • MKIDs allow photon timing information with1usec resolution.

Amplitude of S21 frequency scan around resonance fo Phase of S21 frequency scan around resonance fo Kinetic inductance changes. Resonator’s

  • temp. goes up

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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Typical MKID response to a photon. Complex (amplitude & phase) signal

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  • The resonator is excited by the DAQ at its resonant frequency.
  • The ADC of the DAQ looks at the dynamics of the S21 signal coming

back from the MKID detector at the resonant frequency.

  • The signal has a fast rise time and a slow recombination time ~100 us.

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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DAQ block diagram

  • A DAQ board will generate signals for 1K pixels.
  • A DAQ board will live stream data from 1K pixels at 1 MHz sampling per channel.
  • After generation signals are up converted to RF and down converted again before

sampling.

  • The 1st amplifier is a HEMT at 3K with a noise temperature of 5K.

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4 Gs/s A/D, channelizing, digital filtering, photon catalog

1K pixel resonator signal generator, power calibration, 4 Gs/s DAC

1pps, and 10 MHz reference. Rubidium clock, frequency synthesizer Computer

MKID HEMT

Cold Warm Warm

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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Three or two board solution (for 1K pixel, scalable)

  • Currently the ROACH2 FPGA hosts the highly complex firmware and provides

the interface to the computer.

  • CASPER collaboration (https://casper.berkeley.edu/)

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ADC DAC FPGA

Memory

LO

CLK and sync

CASPER Roach2

Fermilab electronics RF/IF RF/IF From CASPER collaboration

Ethernet USB

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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A 10K to 20K pixel DAQ

  • The existing design is for 10 K pixels

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ROACH2 Fermilab electronics

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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A 10K to 20K pixel DAQ

  • MKID signal generation:
  • 8 GB/s for 1K pixel. 80GB/s 10K pixel system.
  • Tunable frequency and power for each resonator.
  • MKID acquisition:
  • 6 GB/s for 1K pixel. 60GB/s for a 10K pixel system.
  • Scalable to 20K (even 30 K) pixel is reasonable.
  • Data output bandwidth is about 1K photons/pixel
  • A 10K pixel system outputs ~100MB/s (10 B/photon)
  • Data crunching of x1000 in the FPGA
  • Software pipeline runs on main computer.
  • Inherited from ARCONS project (UCSB)

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RF board

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RF out IF out RF in IF in LO To MKID from MKID

Up conversion, amplification, attenuation and filtering Down conversion, amplification, attenuation and filtering

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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RF/IF board specifications

  • LO generation.

– RF frequency dynamic range: 4-8.5 GHz.

– Each RF channel utilizes half of total spectrum. – LO is tuned to 5.5GHz for the 4.5-6.5 GHz RF line and tuned to 7.5GHz for the 6.5-8.5 GHz RF line. – LO can be swept in 1Hz steps to precisely match MKID resonance frequencies.

  • RF Input :

– 100 dBm. On board amplification. – ~2dB flatness over 4.5-8.5 GHz spectrum. – Only 2 different amplifiers used: Hittite HMC3587 and HMC313. – MKID power will be between -80 to -115 dBm and there will be a 35 dB gain (HEMT) (cold electronics) and some attenuation (cables and splitters). – 3 to 34 dB step attenuator to adjust to input power. – I-Q mixer.

  • RF output.

– Distortions are critical. Powers are optimized at the mixer.

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RF board measurements (loopback mode)

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To spectrum analyzer from signal or frequency comb generator 10 MHz reference

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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RF board measurements (loopback mode)

  • a

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The comb generator is an

  • ld instrument,

so powers are uneven. Important points are: No major spurs generated by the RF board. Flat noise floor at 1GHz span.

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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Very clean close in noise (200 Hz span)

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10/28/2014 Presenter | Presentation Title 15

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No spurs in the pixel channel bandwidth

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Phase noise -97 dBc/Hz at 500 KHz

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ADC and DAC design

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4 Gs/s Internally generate from DDR3 4 Gs/s

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ADC and DAC board

  • 2 x 2Gs/s 12bit ADC with JESD204B interface.
  • 2 x 2Gs/s 16bit DAC with JESD204B interface.
  • Virtex 7 FPGA. The type of FPGA is determined by the ADC and DAC

JESD204B interfaces (8 channel high speed SERDES).

  • The JESD204B interface is preferred because it eliminates many

parallel connections between the ADC/DAC and FPGA, and simplifies the data transfer process. Better synchronization.

  • Virtex 7-330T is large enough to hold the firmware that currently runs on

the Roach2 FPGA.

  • We can get rid of the Roach2 and save money.
  • The goal is $5/pixel.
  • Clock
  • 1 Hz resolution synthesizer.
  • 200 fs synchronization and distribution.

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1K pixel channelizer and photon detection firmware

  • The firmware is based on polyphase filter banks, digital

down converters and filters.

  • Photon detection is done by a matched filter.
  • The firmware has been developed at UCSB for the

ARCONS project (arXiv:1306.4674)

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  • B. Mazin, M. Strader, UCSB

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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10 K pixel DAQ schedule

  • RF board testing 80% complete.
  • ADC/DAC board is currently in schematic capture and PCB layout
  • Fabrication late January.
  • Testing February-March.
  • 10 K pixel system integration April-June
  • We should have a running system by July 2015.

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  • FERMILAB MKID pixel DAQ (per board)
  • 8 times the number of channels.
  • 8 times the RF bandwidth coverage.
  • ~1/10 the cost per channel.
  • Scalable to 10K to 20K with the same number of boards a 2K

pixel system uses today.

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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10 K pixel MKID detector and DAQ collaboration

  • University of California at Santa Barbara (UCSB), Jet Propulsion Lab.
  • MKID detector.
  • University of California at Santa Barbara (UCSB)
  • Firmware and software.
  • FERMILAB
  • RF/IF electronics.
  • ADC/DAC electronics.
  • System integration.

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This DAQ R&D will enable Fermilab and collaborators to have a 10K or 20K pixel MKID instrument at SOAR in 2016. This DAQ is aligned with the R&D needed to achieve a G4 instrument for CMB. The astronomy community is also very interested in using this design: Projects: DARKNESS, KRAKENS, SCExAO.

Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology

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Thank you

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Spare slides

10/28/2014 Presenter | Presentation Title 23

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MKIDs DAQ Phase 2: Target 100K pixels or larger systems.

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ROACH2 can be eliminated

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MKIDs DAQ Phase 2: Target 100K pixels or larger systems.

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4 to 5 K pixel per DAQ board.

FPGA CLK Distr. FPGA DRAM Mb/s Mb/s LO Gb/s Gb/s

. . . . . .

4 to 5 RF Channels Out and in

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a

  • a

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Up conversion, amplification, attenuation and filtering Down conversion, amplification, attenuation and filtering

To MKID From MKID LO

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a

  • a

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Single frequency test Noise floor 105 dBc/Hz Flat noise floor 1GHz span

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ADC test with a comb generator

  • Over 55dB SFDR and 95 dBc/Hz

10/28/2014 Presenter | Presentation Title 28