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N éel I RAM K IDs A rray Grenoble (Néel, IRAM, LPSC, LAOG) Cardiff SRON Roma-Trento

N éel I RAM K IDs A rray Grenoble (Néel, IRAM, LPSC, LAOG) Cardiff SRON Roma-Trento. NIKA timeline. November 2008 : Kick-off 2009 : First antenna-doupled arrays in February First demonstration of LEKIDs arrays in May Final arrays made in September

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N éel I RAM K IDs A rray Grenoble (Néel, IRAM, LPSC, LAOG) Cardiff SRON Roma-Trento

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  1. NéelIRAMKIDsArrayGrenoble (Néel, IRAM, LPSC, LAOG) Cardiff SRON Roma-Trento

  2. NIKA timeline November 2008 : Kick-off 2009 : First antenna-doupled arrays in February First demonstration of LEKIDs arrays in May Final arrays made in September 30-40 pixels, mono-band 2mm, run in October Pico Veleta Sensitivity: 1.2·10-15 W/Hz0.5 Reference: 2010 : 112 x 2 pixels Sensitivity (in progress) 36·10-16 W/Hz0.5 Sensitive to only one polarisation ! Dual-band: 125  170GHz et 180  270GHz 2011 (GOALS) : to be discussed (many options)

  3. Electronics PAST / PRESENT NIKA 2009: Bonn electronics 400MHz (ADC 8 bits), FFT, max. rate 5Hz NIKA 2009: Néel box (« Loren ») 50MHz (ADC 12 bits), 32 ch., max. rate 50 Hz NIKA 2010: ROACH board (Néel box with up-down converter and USB attenuators) 230MHz (ADC 12 bits), 112 channels, rate 22 Hz FUTURE LPSC 2011 GOAL : > 256 channels modules over > 400MHz band Fast rate (at least 20Hz are needed) First prototype funded by CNES and IN2P3 SRON 2011 see Andrey, but GOAL is >1GHz band, FFT (rate ?)

  4. Noise spectrum on (good) sky Average LEKIDs detectors noise : 2Hz / Hz0.5 at 1Hz (stable during the run

  5. Misterious 50s-period noise 100Hz steps !!! Detectots noise is less than 10Hz p-p !! Appearing from time to time, lasting for a few hours and then disappearing.

  6. 50s noise again

  7. A HUGE insect in the cabin

  8. EMIR chopper ON/OFF

  9. B-field jumps on antenna-coupled array

  10. B-field jumps on LEKIDs

  11. Laboratory (sky-simulator) performances Average 4mK/Hz0.5  4·10-16W/Hz0.5 per pixel Problem confirmed on the telescope. Can be explained by the electronics : sensitivity depends critically on power per KID. Taken into account for LPSC2011 electronics. Best pixel < 2 mK/Hz0.5 (  1.1 mK/Hz0.5 if « speed read-out »)

  12. Very rough estimation of S/N The average « very raw » S/N on Mars is: 2mm1.25mm Signal : 2-4 kHz 10 kHz Noise : 2 Hz/Hz0.5 16-20 Hz/Hz0.5 Mars flux : 40Jy 107Jy S/N 1000-2000 Hz0.5 500-625 Hz0.5 Sensitivity (1Hz) 20-40mJy/Hz0.5 170-210 mJy/Hz0.5 (per pixel) NEP (1Hz)  estimated by sky simulator !! Please take it as very raw. Then other effects might limit the noise on real maps. IN ANY CASE IT’S MORE OR LESS WHAT WE EXPECTED BASED ON THE SKY SIMULATOR RESULTS.

  13. Exemple résultat : CygA

  14. Exemple résultat : DR21(OH)

  15. Spectral response (Grenoble MPI, 11/2010)

  16. Conclusions DETECTORS Clearly better than 2009 at 2mm. A factor of 4 very raw S/N estimation. Still to be confirmed on real maps (B fields ??). Best LEKIDs pixels tested on sky simulator already almost OK. Average performances of the array to be improved: - dual-polarisation meanders (LEKIDs). Better for cross-talk too. - AR coating (LEKIDs and antennas) - electronics (same power on all pixels) - read-out on « maximum speed » (but less dynamics) - if all that not enough: TiN (or similar) for higher response - …. Andrey ? Jochem ? PIXELS COUNT Much better than in 2009 (factor 4-6). Limited by the electronics. Arrays sizes will now grow according to electronics developments. OPTICS Same cryostat/filters is OK up to 3arc-min field-of-view. Use a real dichroic for splitting (factor of  2 in power).

  17. Plans for 2011 A FURTHER TECHNICAL RUN ? TWO SEPARATE RUNS ? A MORE « USABLE » INSTRUMENT ? WORKING ON THE BIG CAMERA ? HOW BIG ? IN CASE WE GO FOR SPRING 2011 : CRYOSTAT  PULSE-TUBE (if possible) PIXELS  224 per array, over a 400MHz band ELECTRONICS  Baseline: LPSC2011. ROACH is backup if LPSC is still under development. FILTERS  from NIKA2010 SPLITTER  DICHROIC (if possible) DETECTORS 2mm  Same as NIKA2010; dual-polar if dichroic DETECTORS 1mm  Antennas or LEKIDs (the best, taking into account the number of pixels that can be actually read-out by existing electronics at that time, and sensitivity)

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