a. monfardini, iap 30/07/2010 1 nika (néel iram kid array) first light at the 30-m iram dish nika...

A. Monfardini, IAP 30/07/2010A. Monfardini, IAP 30/07/201011

NIKA (Néel IRAM KID Array)NIKA (Néel IRAM KID Array)

First light at the 30-m IRAM dish First light at the 30-m IRAM dish

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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Horizontal Dilution CryostatHorizontal Dilution Cryostat

T T basebase = 60mK = 60mK


Cryostat (on anti-vibration table)

NIKA interface optics

To IRAMTo IRAM secondary mirrorsecondary mirror

… … through this holethrough this hole

Credit: L. Swenson

NIKA installed – 19/10/2009NIKA installed – 19/10/2009


Designed and fabricated in Grenoble (Néel and PTA).

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Data-sheet:Data-sheet:

- 40nm Al- fR = 1.50 - 1.55 GHz- Qc 30,000- 3dB deep resonances(large scatter)- Read-out : Grenoble FPGA electronics

NIKA: 30 pixels LEKIDs arrayNIKA: 30 pixels LEKIDs array

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


NIKA 2009: Mars transits (raw data)NIKA 2009: Mars transits (raw data)


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)


Sky noise (correlated) dominates below 0.4 Hz (average sky conditions)

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)


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


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.


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


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


THANKSTHANKS


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


Tool to find resonances - BEFORETool to find resonances - BEFORE


Tool to find resonances - AFTERTool to find resonances - AFTER

a. monfardini, iap 30/07/2010 1 nika (néel iram kid array) first light at the 30-m iram dish nika...

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