Development of Kinetic Inductance Detectors for astronomical applications
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1 Development of Kinetic Inductance Detectors for astronomical applications Faouzi Boussaha Samir Beldi Christine Chaumont Florent Reix Shan Mignot Thibaut Vacelet Piercalo Bonifacio GEPI (Galaxies, Etoiles, Physique et Instrumentation) - Observatoire de Paris, Paris - France Alessandro Traini Andrea Tartari Michel Piat APC (AstroParticule et Cosmologie) - Université Paris Diderot, Paris - France KIDs: The Next Generation, Dublin Workshop 7 th - 8 th September 2017
2 Outline (GEPI) mm Coupled Antenna MKIDs (APC)
3
4 Motivation At GEPI, all the science is done at NIR and visible wavelengths. Very promising technology for many astronomical applications. Possible application: MOSAIC-like projects.
5 MOSAIC : Multi-Object Spectrograph of the Extremely Large Telescope (ELT) PI : François Hammer (GEPI) Paris Observatory
6 MOSAIC : Multi-Object Spectrograph of the Extremely Large Telescope (ELT) A unique range of observations! SC1: FIRST LIGHT SPECTROSCOPY OF THE MOST DISTANT GALAXIES SC2: EVOLUTION OF LARGE-SCALE STRUCTURES SC3: MASS ASSEMBLY OF GALAXIES THROUGH COSMIC TIMES SC4: AGN/GALAXY CO-EVOLUTION & AGN FEEDBACK SC5: RESOLVED STELLAR POPULATIONS BEYOND THE LOCAL GROUP SC6: GALAXY ARCHAEOLOGY SC7: GALACTIC CENTRE SCIENCE SC8: PLANET FORMATION IN DIFFERENT ENVIRONMENTS ELT-MOS White Paper: Science Overview & Requirements, Evans et al., ArXiv: V1
7 MOSAIC requirements
8 3.7mm As a start point, design inspired by the University of California work (B. Mazin et al). 1GHz<f 0 <2GHz 300 m 50 CPW line 3.7mm Simulation of a TiN-based LEKID resonating within 1-2 GHz, using typical TiN parameters of : - 60 nm-thick and T c 1K - L kin =24 ph/ - n =110 cm
9 300 m 300 m In order to efficiently meet with the requirements of some astronomical applications (high spatial resolution), the KID size should be diminished typically from hundreds to a few tens of m. Increasing the fill factor. Replace the interdigitated Capacitor by a parallel plate (MIM) capacitor. 1GHz<f 0 <2GHz
10 100 m 1GHz<f 0 <2GHz 50 m 100 m Simulations of a parallel plate capacitorbased KID with r =8 (AlN) and t insolator =100 nm using TiN parameters of : - 60 nm-thick and T c 1K - L kin =24 ph/ - n =110 cm - Dielectric loss factor Tan( )=0 The frequency is tuned by removing nx4 4 μm square from the upper electrode or the bottom electrode.
11 Nb Nb/Dielectric/NB TiN Si S. Beldi et al., LTD 2017 Simulations with r =8 (AlN) and t=100 nm. Dielectric loss factor tan( ) < 10-5.
12 50 nm-thick AlN (Al 2 O 3 ) Nb/AlN/Nb Capacitor 50 nm-thick TiN First design: 5x4 pixels Nb Next step: the use of Al 2 O 3 deposited by Atomic Layer Deposition (ALD) process (G. Coiffard et al, LTD 2017)
13 New concept to increase the detection efficiency? MgF2 (t= g /4) TiN Magnesium Fluoride (MgF 2 ) is widely used as an antireflection layer. Capacitor Au/Ti Reflector (backshort) MgF 2 Transmission
14 New concept to Increase the detection efficiency? Au Reflectance
15 35 um Without MgF 2 With MgF 2 50 um 35 um Simulation of LEKID without and with a reflector and MgF2 layer.
16 Effect of the MgF 2 dielectric loss factor tan( ) MgF 2 is amorphous probably a high TLS noise Can the softening of the chemical bonds between the superconducting layer and the substrate help to decrease the TLS noise?
17 HR Si Au MgF2 Al (sacrificial layer) TiN Hard contact between the TiN layer and the substrate (acting as anchor points). Soft contact between the TiN layer and MgF 2
18 Anchor points 60 nm-thick TiN 60 nm-thick Au
19
20 mm MKIDs
21 mm MKIDs (APC applications) Goal Characterization of the polarization properties of cosmic microwave background CMB (B-Mode). Why MKIDs? high multiplexing capability (10 4 pixels)
22 mm MKIDs (APC applications) 12 pixles, 3 designs A. Traini et al., LTD GHz Antenna slotline/2um-wide microstrip) 150 GHz Bandpass Filter 220 GHz Bandpass Filter LC Resonator 1 LC Resonator nm-thick SiO 100 nm-thick Nb Interdigitated Capacitor Nb Inductance 20 nm-thick Al (absorbeur) RF coupler (2 um-wide microstrip/slotline transition)
23 mm MKIDs (APC applications) Preliminary experimental results T=295mK T=290 Qi=
24 Conclusion We are developing Near Infrared and Visible MKIDs using parallel plate capacitors. A (new) concept to increase the detection efficiency, as well as to decrease the TLS noise?
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