DAQs for cryogenic detectors in Cosmology Gustavo Cancelo, FERMILAB DAQ R&D Workshop 11 October 2017
Objectives • Identify the DAQ and Trigger challenges that long-term future experiments will face. • Identify detector and DAQ synergies and common efforts across our physics frontiers. • Identify breakthroughs in detector and DAQ from outside the DOE/NSF community that can facilitate our physics and computing. 2 Presenter | Presentation Title 10/10/2017
Identify the DAQ and Trigger challenges that long-term future experiments will face • Detector development is focused on physics goals and opportunities. – High-tech consumer products also generate detector breakthroughs. • Detectors drive DAQ and Trigger architectures. • Detectors, DAQ and Triggers for Cosmology overlap with other areas of our physics such as Neutrinos, HEP and computing. • Cosmology is a very diverse field. I will highlight DAQ for: – Dark matter – Dark energy 3 Presenter | Presentation Title 10/10/2017
Dark matter • Almost everybody thinks that DM exists and it is cold. – Currently and in the near future the attention will focus on WIMPs and AXIONs. – WIMPs and AXIONs are particles that interact through the weak force. – DM models cover energy scales from ueV to TeV. – The energy scale is unable to be covered by a single experiment. – Current DOE experiments are ground based and direct search. • WIMP search experiments look for nuclear or electron recoils in the detector mass. – Atmospheric neutrino background is a potential problem. Characterizing the neutrino floor is important. • AXION experiments try to detect the decay into a pair of photons. Measure power in a resonant cavity. 4 Presenter | Presentation Title 10/10/2017
Dark matter • For decades DM experiments evolved with what the technology allowed. – New technologies based on cryogenic detectors (e.g. noble gases and liquids, silicon devices at ~140K and superconducting sensors) have pushed the energy threshold to sub GeV scales. – DAQs have accompanied the trend by developing ultra low noise electronics. • Not always “bigger is better”, DM experiments must beat the radioactive backgrounds. – DM experiments have achieved a maturity that have allowed them to grow to multiple Kg or tonne of detector mass. • DOE G2 experiments: LZ (Xenon), ADMX (axions), SCDMS (superconducting germanium). • Will these technologies carry over to G3? • What other technologies are trying to gain space? – Massive “zero noise” CCDs (skipper). – Low noise CMOS detectors. – Gas TPCs for directional DM search. – Superconducting detectors: MKIDs, Josephson junction, etc. – Multi cavities for Axion detection. – Superfluid detectors for low energy DM. 5 Presenter | Presentation Title 10/10/2017
Dark matter: Future DAQ example for massive CCDs • Established detector technologies will grow in mass and number of detectors/channels. • “Zero noise” silicon detector can see nuclear and electron recoils with 1.1 eV threshold Javier Tiffenberg arXiv:1509.01598 6 Presenter | Presentation Title 10/10/2017
Particle detection with CCDs muons, electrons and diffusion limited hits. Next generation of CCDs achieve <0.1 electrons of noise !! 20,000 channel instruments for dark matter and low energy neutrino searches. Ultra low noise DAQs are needed (zero noise contribution).
CCDs for DM and neutrinos • 6K x 6K pixels, 1mm thick = 20g of mass. Can operate at 140K. Dark current 10 −3 e - pix −1 day −1 . Could achieve 10 −7 e - pix −1 day −1 . • • Radiopurity of the current package < 5 dru. 8 Presenter | Presentation Title 10/10/2017
Dark matter: FNAL DAQ • Very successful collaboration of FERMILAB, Univ. del Sur (Argentina), CNEA (Argentina), UNAM (Mexico), Univ Asuncion (Paraguay) • 4 channel DAQ is working. – The purpose of the 4 channel is CCD characterization in the labs. • 20 channel/board DAQ being designed to target detectors of up to 1000 channels. • Experiments: – DAMIC 1Kg, ~200 channels. – SENSEI: Skipper CCDs, 100g, 200 ch. – CONNIE 1Kg: ~1000 channels. 5 x 5 inches • DAQ challenges for a larger system (e.g. 1000 channels, 50 x 20 channel board) • System noise: including PCB and EMI noise must be contributing zero noise to a “zero noise” detector. • Conductive EMI from AC line, vacuum and cooling. • Each CCD channel requires 17 clocking signals at 10’s of volts and a video reading uV. • CCD bias voltages must be clean. 9 Presenter | Presentation Title 10/10/2017
Dark matter: FNAL DAQ Dewar for 2 Kg mass 4 quadrants 24 CCDs each • Clock channels can be shared. • Videos could be shared. – Skipper CCDs may need to be readout continuously. • Grounding and controlling EMI is crucial. • Data bandwidth for 1000 channels: 1 GB/s all to disk. • No triggers or data combiners needed. • Sophisticated DAQ and slow control software needed. 10 Presenter | Presentation Title 10/10/2017
DAQ electronics for 24 CCDs DC power Power DAC_H management . CLK Linear DC . DAC_L SPI Analog Generation . . . switch . . Based on Power . Matrix . 40 channel management 12 bit DACs Linear or switched Bias 1 Bias voltages . . Generation Individual . . . Based on or grouped . . VIB . Ethernet 40 channel . Bias N 12 bit DACs CCD DAQ FPGA Video Analog readout Based on MUX 20 MHz 18 bit ADCs The most challenging part is that all the data must be acquired with the level of quality. If the noise is not uniform it is hard to achieve low energy thresholds and to calculate detector efficiencies. The DAQ must work flawlessly and stably during the life of the experiment. 11 Gustavo Cancelo | CONNIE electronics 10/10/2017
Physics reach • New physics: • Dark photon • A’ boson • Neutrino magnetic moment • Large number of theoretical models can be tested 12 Gustavo Cancelo | CONNIE electronics 10/10/2017
DAQs for Dark energy and the evolution of the universe 13 Presenter | Presentation Title 10/10/2017
DAQs for Dark energy and the evolution of the universe DES CMB • The present: – DES Optical surveys and • Science reach: CMB highly – SPT3, ACT – Dark energy complementary • The near future: Other probes can also – Large scale mass. – LSST contribute – BAO. – DESI – Inflation – Simons observatory – Neutrino masses • What is in the longer term future – Light relativistic species. for CMB and optical surveys? – Etc. 14 Presenter | Presentation Title 10/10/2017
DAQs for Dark energy and the evolution of the universe LSST will generate >1 billion galaxy catalog. Opportunities for spectroscopic surveys!! • CMB future: CMB S4 – A collection of CMB telescopes at the South pole and Atacama – Superconducting detectors: Frequency Multiplexed TES or MKIDS. • Optical surveys: Electronics and DAQ – High and low resolution spectroscopy. – 100,000 channels high res spectrometer? – Low res MKIDs based instrument? Could cover the near infrared spectrum! 15 Presenter | Presentation Title 10/10/2017
DAQs for Dark energy and the evolution of the universe 1pps, and 10 MHz reference. • Superconducting detectors Rubidium clock, frequency synthesizer • Frequency multiplexed. RF • RF electronics. IF IF • Almost the same warm DAC: signal A/D, electronics. generator for channelizing, thousands of digital filtering, channels HEMT MKID • Challenges: Warm Warm Cold Computer – High number of channels per RF feed to minimize thermal load and detector wiring. – Low noise in a multi GHz RF environment with noise sources coming from mostly digital electronics. – Cost: few dollars/channel. – High input and output bandwidth. 16 Presenter | Presentation Title 10/10/2017
Fermilab DAQ: this is the most advanced electronics today 10 K pixels crate To MKID RF out Up conversion, LO amplification, IF in attenuation and filtering from MKID RF in ROACH2 Down conversion, IF out amplification, attenuation and filtering Fermilab electronics To MKID To/from ROACH2 from MKID MKIDs for optical require a detector with a BW of ~250 KHz. CMB ~100Hz. (More channels per ADC and more resolution). 17 Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology 10/10/2017
FMESSI (Frequency Multiplexed Electronics for Superconducting Sensor Instrumentation) DARKNESS at Palomar • Applications: – CMB-S4. – Quantum computing. – Low resolution spectroscopy for cosmology. • DARKNESS: 10,000 pixel instrument • 2 observation runs at Palomar • KRAKENS: 30,000 to be deployed at KECK 1 Mauna Kea coming up Oct.2017 The next step is to apply the FMESSI DAQ to CMB sensors working in frequency multiplexed mode. CMB channels are low bandwidth. 5000 ch/board is doable with current DAQ. Cost: $1/channel (5000 channels) 18 Gustavo Cancelo | Scalable 10 to 20 Kilo-pixel MKID Signal Generation and DAQ for Cosmology 10/10/2017
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