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MONFARDINI Alessandro

Some KID development in Grenoble. MONFARDINI Alessandro. Institut Néel, LPSC, IPAG + IRAM (mainly for NIKA2). NIKA1 (350 pixels): finished NIKA2 (3000 pixels): observing CNES R&Ds « low background » and « high frequencies » CNES R&D « cosmic rays » KISS : mounted at Tenerife

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MONFARDINI Alessandro

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  1. Some KID development in Grenoble MONFARDINI Alessandro Institut Néel, LPSC, IPAG + IRAM (mainly for NIKA2) • NIKA1 (350 pixels): finished • NIKA2 (3000 pixels): observing • CNESR&Ds « low background » and « high frequencies » • CNESR&D « cosmic rays » • KISS: mounted at Tenerife • CONCERTO: if everything goes well on Sky in 2021 on APEX • SKID (Sub-gap KID) and materials study • - ….. Future CMB experiment « still under discussion »

  2. NIKA1: the first kSZ map Astronomy & Astrophysics 598, A115 (2017)

  3. NIKA2 status • - Operational since January 2016 at the 30-meters telescope • Open to the astronomy community since 2017 • Currently observing (available on semester base via competitive calls) • Most powerful mm-wave camera on single dish open to the community • 3,000 pixels split into three arrays: • 150 and 260 GHz photometry • polarisation at 260GHz • FoV of 6.5 arc-min • resolution of 11arc-sec at 260GHz

  4. NIKA2 arrays After noise and stability cuts, the number used for published maps is lower

  5. NIKA2: clusters and deep fields + a recent detection of a GRB afterglow

  6. Arrays cosmetics: post-processing Shu Shibo (PhD Thesis) Starting from a typical array: 1) we obtain a map with the sky simulator 2) We identify the pixels with The resonances 3) We calculate a correction to be implemented on the last C finger 4) We do the correction by litho + etching 5) We measure again POSSIBLE TO OBTAIN PRACTICALLY PERFECT RESONANCE PLACING !!! • APL 113, Issue 8, 082603 (2018)

  7. R&T “low background” • Optical NEPs • Pixels in 100s pix arrays • Measured with MUX • f = 80 – 650 GHz Funded by CNES, realised by CNRS Grenoble

  8. R&T “cosmic rays” One NIKA1 array, under realistic background conditions (0.5 pW/pix) and sensitivity (10-17 W/Hz0.5), irradiated with 630-keV alphas. For any useful sampling frequency only one sample is affected. https://arxiv.org/abs/1606.00719 (SPIE 2016) From the functional point-of-view (array on a satellite) it seems OK already  Confirmed by OLIMPO ! Funded by CNES, realised by CNRS Grenoble

  9. Low-resolution spectroscopy • NIKA2 is already doing high-resolution large FoV mm-wave imaging. The polarisation at 260GHz is also implemented. • STRATEGY: adding the spectral dimension: •  preserving the large field-of-view and angular resolution (many pixels) • Low resolution (R  20-100), not competing with other techniques • Science cases are VERY STRONG • Feasible today (see OLIMPO and KISS) • CONCERTO is equivalent from DAQ and analysis point-of-view to 0.6Mpix !

  10. Spectroscopy strategies Heterodyne R =  /  Interstellar chemistry (et al.) 106 On-chip (filter bank) or Dispersive optics 103 Cosmology (et al.) Fourier Transform 102 103 101 100 Field-of-view (spatial pixels)

  11. ….. [1, N] 1 23 …..N-2 N-1N FFT INTERFEROMETER ….. Technological options 1 23 …..N-2 N-1N [1, N] ON-CHIP e.g. DESHIMA on ASTE e.g. CONCERTO

  12. KISS: mounted on QUIJOTE • Telescope: 2.5 m • Fied-of-view: 1 deg • Pixel on Sky: 3 arc-min • Band: (80)120300 GHz • Readout rate: 4kHz • Pixels: 632 • resolution: 20  100 Equivalent to 12  60 kpix KISS mounted on QUIJOTE at Teide Observatory Undegoing tests Goal (ambitious!): low-z SZ spectra

  13. KISS: mounted on QUIJOTE

  14. CONCERTO: C [II] line PRIMARY GOAL: map the C+ fine transition line at z = 4 – 8 from the ground SECONDARY: general use instrument (as NIKA2). In particular, ideal for SZ

  15. CONCERTO: started First CONCERTO installation at APEX Measuring te deformations of the Cassegrain cabin with wire sensors  OK for installation on the floor First visit to APEX (04/2018)

  16. CONCERTO datasheet

  17. h h h Absorption Frequency The KID Tbase < 0.2 K ·  f (GHz) / 100 GHz  Not a math demostration but based on NIKA/NIKA2/etc experience. e.g. in NIKA2 we regulate at 190mK. • fC 100 GHz · (Tc / 1.3) • e.g. Tbase< 0.2K @ 100GHz • e.g. Tbase< 0.02K @ 10GHz • e.g. Tbase< 0.002K @ 1GHz Tc Tc fCUTOFF

  18. 1 2g Low-pass filter Absorption 0 0 100 200 300 400 Frequency (GHz) Aluminium KID Lk 2 pH / 

  19. Multilayers KID Low-pass filter Ti-Al Tc= 0.9K Al Tc= 1.4K Normalized Absorption Lk 5 pH / 

  20. Another multilayer (our first) First test on a tri-layer in 2014 (CSNSM – Néel). Al-Ti-Au (cutoff at 60GHz)

  21. TiNx and NbxSi KID M. Calvo, LTD15 (2013) Lk 250 pH / 

  22. InOx KID (Tc = 2.8 K) 1 1.0 • measured also by STM 2· Absorption Frequency (GHz) Lk 1 nH / 

  23. The Sub-gap KID (SKID) O. Dupré, A. Benoît, M. Calvo, A. Catalano, J. Goupy, C. Hoarau, T. Klein, K. Le Calvez, B. Sacépé, A. Monfardini, F. Levy-Bertrand, Supercond. Scienceand Technol.30045007 (2017)

  24. Frequency selectivity R = / = 2500 < ( g / 10 ) O. Dupré et al., Supercond. Sci. Technol.30045007 (2017)

  25. SKID vs. KID • KID are wideband(imaging) , SKID are selective in energy • (spectroscopy) • SKID break the « T < 0.2 · (frequency / 100 GHz) » rule • that KID must obey • For SKID, highly-anarmonic materials (low Jc) are most • adapted. In KID the highest Jc results in better S/N • KIDhave already natural applications in low-resolution • visible-NIR spectroscopy and for mm and sub-mm continuum • Astronomy. SKID applications and competitivity with respect • to other technologies are still to be investigated.

  26. Conclusions • A « W band » camera of hundreds to thousands pixels is feasible • I think it will need a dilution or ADR (if it has to be optimised) • Polarisation splitting can be achieved on-chip, with an OMT or with a 45 deg polariser • An application for the SKID ? Probably not … but I try …

  27. 1.832 GHz 7.511 GHz 2.0 2.4 7 8 9 (GHz) LumpedDistributed Higher order resonance

  28. All resonators Distributed resonance mode

  29. J* (InO) 4·109A/m2 L. Swenson et al., J. Appl. Physics 113, 104501 (2013) J* (Al) 1012A/m2 Physics explanation •  If the system was perfectly harmonic no effect would be expected • HOWEVER, this is not the case: • J = JLE + Jd . Lk thus increases, « dragging » the LE (readout) fLE • Well-known effect in the qubit community … « cross-Kerr » • Used in the « Kinetic Inductance parametric amplifier » • Open question: dissipative mechanism ?

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