A. Monfardini, IAP A. Monfardini, IAP 30/07/2010 30/07/2010 1 NIKA (Néel IRAM KID Array) NIKA (Néel IRAM KID Array) st light at the 30-m IRAM di st light at the 30-m IRAM di NIKA collaboration: NIKA collaboration: - Institut Néel - Grenoble - AIG - Cardiff - SRON - Utrecht and Groningen - Max Planck Institute - Bonn - IRAM - Grenoble - La Sapienza – Roma + IRST - Trento - LPSC - Grenoble
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A. Monfardini, IAP 30/07/2010 1 NIKA (Néel IRAM KID Array) First light at the 30-m IRAM dish NIKA collaboration: - Institut Néel - Grenoble - AIG - Cardiff.
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A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/201011
Average optical NEP (1Hz) on telescope : Average optical NEP (1Hz) on telescope : 10 10-15 -15 W/HzW/Hz0.50.5
Real conditions, UNDER > 10pW/pixel loading.Real conditions, UNDER > 10pW/pixel loading.... actually better considering that we only have 1 polarisation... actually better considering that we only have 1 polarisation
Operating at 130-170GHzOperating at 130-170GHz
A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/201055
NIKA 2009: Mars transits (raw data)NIKA 2009: Mars transits (raw data)
A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/201066
Visible already in the first scan, also on single pixels maps. Good S/N
BL1418+546 (BL1418+546 (1.2 Jy1.2 Jy))
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Extended sources : M87Extended sources : M87
More details on the NIKA run : arxiv/1004.2209 (A&A, in press) More details on the NIKA run : arxiv/1004.2209 (A&A, in press)
A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/201088
Part of detectors noise is correlated (common mode gain variations)
SKY noise (SKY noise ( f f-2.1-2.1))
Detectors noise (Detectors noise ( f f-0.55-0.55))
Noise Spectrum (on-sky, during observations)Noise Spectrum (on-sky, during observations)
A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/201099
NIKA 2010: larger and more sensitiveNIKA 2010: larger and more sensitive
Best pixels in 2010 (June). Optical NEP (1 Hz) Best pixels in 2010 (June). Optical NEP (1 Hz) 2 2··1010-16-16 W/Hz W/Hz0.50.5
- Reduced the phase noisephase noise by playing with the design- Improved the optical responseoptical response by reducing the film thickness- Improved lithography quality and made larger arrayslarger arrays
- Optics is OK in lab (well separated beams)
- EM cross-talk shuffling the resonances. Work in progress.
Best array so far (last week). Average optical NEP Best array so far (last week). Average optical NEP 6 6··1010-16-16 W/Hz W/Hz0.50.5
ININ OUTOUT
A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/20101010
It’s READY ! First complete test (Sky Simulator) next week with :It’s READY ! First complete test (Sky Simulator) next week with :- Néel: mechanics, cryostat, lenses (HDPE)- Cardiff: (filters, optical splitter)- 2mm (IRAM/Néel) and 1.25mm (Roma/Trento) arrays
Bands : 1.25 – 2.05 mm
Pixels : 144 x 2
F/1.9
Field-of-view : 1.5 arc-min
NIKA 2010: dual-band tooNIKA 2010: dual-band too
Pre-scheduled for the end of Pre-scheduled for the end of October on the 30-m telescope.October on the 30-m telescope.
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Cosmics: first « fast MUX » measurementCosmics: first « fast MUX » measurement
For more details : L.J. Swenson et al., APPLIED PHYSICS LETTERS 96, 263511 (2010)For more details : L.J. Swenson et al., APPLIED PHYSICS LETTERS 96, 263511 (2010)
We could triangulate the interaction position (300m error for 2.2mm pixels).X-rays 6 keV photons interacting in the substrate are seen clearly (S/N >> 10). A REAL PROBLEM FOR SPACE/SENSITIVE APPLICATIONSA REAL PROBLEM FOR SPACE/SENSITIVE APPLICATIONS
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Status :Status :- Demonstrated in lab up to 160 pixels multiplexed on a single line (Grenoble setup and Bonn MPI electronics). Electronics constantly in progress.
- Best pixels exhibit NEP 2·10-16 W/Hz0.5 under under 10pW loading per pixel 10pW loading per pixel Sensitivity improvements for Bpol :Sensitivity improvements for Bpol :
- Reducing the background translates directlydirectly in NEP reduction- New materials (e.g. very promising TiN, see arxiv/1003.5584)- Horns or not horns ? So far filled arrays ... Horns to be studied in case.- Challenging but not impossible (requires a coherent R&D FR-UK-IT) - Challenging but not impossible (requires a coherent R&D FR-UK-IT)
Cosmics (a real issue !) :Cosmics (a real issue !) :- KIDs are Sensitive to a-thermal (Cooper pair breaking) substrate phonons - Not sensitive to thermal phonons ≠ bolometers≠ bolometers- Rate on 2mm pixels (and > 10-16 W sensitivity) > 0.1Hz at sea level !- Faster than bolometersFaster than bolometers (...but not enough). High Q, long qp slow resonator
- BIG questions are now: - a-thermal phonons mean free path in thin membranes ???- solid membrane OK (easy) or need spider-like structures (more difficult) ??
Electronics :Electronics : - Not a huge problem I think for up to 1000 pixels. Medium term goal is a MUX factor of 103. ADCs improvements might allow 104 in long term.
Conclusions in view of BPolConclusions in view of BPol
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THANKSTHANKS
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BONN (Max Planck Institut) FFTS (2009) BONN (Max Planck Institut) FFTS (2009) – not available for NIKA 2010– not available for NIKA 2010
Useful Bandwidth: 400 MHzMax. readout rate:Max. readout rate: 5 Hz5 HzFFT points: up to 32kTones spacing:Tones spacing: down to 12.2 kHzdown to 12.2 kHzMax number of channels tested:Max number of channels tested: 160160
Grenoble (LPSC and Néel) FPGA READOUTGrenoble (LPSC and Néel) FPGA READOUT (2010)Useful Bandwidth: 125 MHzMax. readout rate:Max. readout rate: 2 MHz2 MHzMax. number of channelsMax. number of channels 128128Tones spacing: down to 1Hz
OPEN SOURCE READOUTOPEN SOURCE READOUT (2010)Useful Bandwidth: 250 MHzMax. readout rate:Max. readout rate: > 2 MHz> 2 MHzMax. number of channelsMax. number of channels for now up to 96for now up to 96Tones spacing: down to 1HzCollaboration :Collaboration : UCSB, Berkeley, Caltech-JPL, NIST, Goddard, Grenoble, UK
Existing MUX Read-Outs Existing MUX Read-Outs
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Tool to find resonances - BEFORETool to find resonances - BEFORE
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Tool to find resonances - AFTERTool to find resonances - AFTER