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MONFARDINI Alessandro

Explore the groundbreaking NIKA2 project in Grenoble, boasting a powerful mm-wave camera on a single dish, split into three arrays for astrophysical observations. Learn about low-resolution spectroscopy and future CMB experiments still in discussion. Discover the technology, array cosmetics, and post-processing involved in the project. Dive deeper into the pixel arrays, noise cuts, and stability measures for publishing accurate maps. Unveil the advancements in SKID and material studies alongside the innovative SKID vs KID comparison. Gain insights into the operational status, science cases, and strategic spectrometry approaches of NIKA2. Find out how NIKA2 is revolutionizing astronomy with its high-frequency observations and potential future cosmic breakthroughs.

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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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