The New IRAM KID Arrays (NIKA) and NIKA-2

Transcription

1 The New IRAM KID Arrays (NIKA) and NIKA-2 CONFIRMED for NIKA-2: Institut Néel, IPAG, IRAM, LPSC Grenoble University of Cardiff UK IRAM Granada Spain CEA-Irfu, IAS, IEF Saclay and Orsay France TO BE CONFIRMED: SRON, Delft TU NL Università di Roma Italy Arizona State University - USA 1

2 IRAM 30m telescope Institut de RadioAstronomie Millimetrique (CNRS, MPG/Germany, IGN/Spain) Located at 2850m altitude in the Sierra Nevada (Spain) l Observations between 74GHz and 360GHz (!) 16 arc- sec 2mm l 30- m aperture 11 arc- sec 1.25mm l Field Of View: 6.5 arc- min l A wonderful tool for millimetre Astronomy e.g. J. Staguhn (poster 304) NIKA: 150GHz and 240GHz or 2mm and 1.25mm NIKA achieved 6 technical/scientific runs 2

3 NIKA (and NIKA2?) LEKID design GOAL: efficiently absorb both polarisations NIKA SOLUTION: Hilbert fractal curve (3 rd order) M. Roesch et al., arxiv: Film: thin Al (12 25nm) 3

4 2mm NIKA array (132 pixels) 129 identified resonances 4

5 2mm NIKA array (132 pixels) 5

6 2mm NIKA array footprint NIKA Run 6 June /132 good beams (95 %) 6

7 NIKA at the 30m Cryostat Input HDPE lens Dilution pumps NIKEL rack 7

8 NIKA at the 30m Cryostat Input HDPE lens Dilution pumps NIKEL rack.. 2 arrays.. 2 Mac s.. 2 hands 8

9 NIKA sensitivity 2mm (more developed) very close to goal (20 mjy s 0.5 / beam, goal 12 mjy s 0.5 / beam) 1.25mm is approaching the specifications (30 mjy s 0.5 / beam, goal 20 mjy s 0.5 / beam) (mjy s 0.5 / beam) NIKA-2 specifications NIKA-2 goals Theoretical photon noise in best conditions 9

10 LO Modulation Stability Measure flux from Uranus (primary calibrator) + 10 h! 2 mm 1.25 mm The modulated readout works! M. Calvo et al., A&A Letters 551, id.l12 (2013) Relative accuracy in NIKA run 3 (2011) : 10% 3 times better than in 2010! 10

11 Photometry (atmosphere correction) The absolute position of each resonance (f 0 ) is linearly dependent upon the background. à A single calibration «skydip» is in principle sufficient for a whole observing campaign!! 2 weeks M. Calvo, A. Catalano et al., in preparation - 2 mm mm NIKA is also a precise, line-of-sight taumeter!! 11

12 3C279 movie 12

13 Nearby galaxies mapping/spectrum June 2013 run 6 Exposure time 18 min. under very poor observing conditions (τ 225 = 0.8) 13

14 Nearby galaxies mapping/spectrum June 2013 run 6 Exposure time 18 min. under very poor observing conditions (τ 225 = 0.8) M82 nucleus (free-free) M82 outskirts (dust) Credit: R. Adam 14

15 First SZ detection with KID NIKA run 5, November 2012 R. Adam et al., in preparation 15

16 Work in progress - IMPROVING QUANTUM EFFICIENCY: e.g. micro-fabricated AR coating - IMPROVING SENSITIVITY/RANGE OF UTILISATION: investigating new materials (e.g. NbSi in collaboration with CSNSM-Orsay and IEF-Orsay). See M. Calvo poster IMPROVING ARRAYS UNIFORMITY: find the best/easiest way to suppress the asymmetric RF modes (e.g. slotline) without adding too much complexity or phase noise. - PIXELS COUNT: producing/testing NIKA-2 arrays 16

17 NIKA-2 (2015) Goals et Varia 6.5 arc- min FoV ( IRAM 30m) Close to background- limited Dual- band imaging + polarization Derived from NIKA R&D ~ 1 ton Characteristics Dual-band (1.25mm and 2mm) 1.25mm KID Arrays Detectors: mm mm NIKEL Read-Out Electronics 2,3 m 17

18 NIKA-2 optical path 1mm H 1mm V 2mm 18

19 THE END 19

20 A faint source at z 6.5 Average sensitivity from this map 13.6 mjy s 0.5 /beam (τ = 0.1) Telescope time: 35 min, map RMS 300µJy 20

21 Noise spectrum is flat! 21

22 Ingredients for science-grade KID 1. PIXELS COUNT (NIKA: hundreds; NIKA2: thousands) 2. SENSITIVITY (ideally approaching background-limited in practice close to state-of-the-art in REAL observing conditions) 3. STABILITY (relative photometry reproducibility in different observing conditions, background etc.) 4. PHOTOMETRY (in particular for ground-based applications, measure the flux accounting for the atmosphere) 5. FRIENDLY (manageable by non-kid-experts) 22

23 LO-modulated readout Δf = (ΔI, ΔQ) (di/df, dq/df) (di/df, dq/df) 2 δf LO ΔP I Excitation tones δf LO << f 0 /Q 100 khz (I,Q) Q Conceptual limitation: only works for frequency/phase readout. à OK for NIKA LEKID S phase 10 S amplitude 23

24 LO-modulated readout Δf = (ΔI, ΔQ) (di/df, dq/df) (di/df, dq/df) 2 δf LO ΔP I Excitation tones δf LO << f 0 /Q 100 khz (I,Q) (di,dq) Q Conceptual limitation: only works for frequency/phase readout. à OK for NIKA LEKID S phase 10 S amplitude 24

25 LO-modulated readout Δf = (ΔI, ΔQ) (di/df, dq/df) (di/df, dq/df) 2 δf LO ΔP I Excitation tones δf LO << f 0 /Q 100 khz (I,Q ) (di,dq (I,Q) (di,dq) Q Conceptual limitation: only works for frequency/phase readout. à OK for NIKA LEKID S phase 10 S amplitude 25

26 Achieved milestones 11/2008 à Kick-off (Institut Néel, SRON, Cardiff, Bonn) 09/2009 à First light at the 30-m telescope, pixels (run 1). Antenna-coupled and LEKID. First KID camera (with MUX) on the sky. Jochem Baselmans Simon Doyle Loren Swenson Alain Benoit Philippe Camus Aurelien Bideaud François Xavier Désert 26

27 Achieved milestones 11/2008 à Kick-off (Institut Néel, SRON, Cardiff, Bonn) 09/2009 à First light at the 30-m telescope, pixels (run 1). Antenna-coupled and LEKID. First KID camera (with MUX) on the sky. 11/2010 à NIKA goes dual-band, 200 pixels (run 2). Sensitivity comparable to existing instruments (MAMBO-2). 11/2011 à dual-polarisation fractal LEKID à 2 better sensitivity cryogen-free cryo, better photometry (run 3). Almost an instrument!! 27

28 Achieved milestones 11/2008 à Kick-off (Institut Néel, SRON, Cardiff, Bonn) 09/2009 à First light at the 30-m telescope, pixels (run 1). Antenna-coupled and LEKID. First KID camera (with MUX) on the sky. 11/2010 à NIKA goes dual-band, 200 pixels (run 2). Sensitivity comparable to existing instruments (MAMBO-2). 11/2011 à dual-polarisation fractal LEKID à 2 better sensitivity cryogen-free cryo, better photometry (run 3). Almost an instrument!! 06/2012 à NIKA permanent installation (run 4). Tot. 356 pixels. NIKEL electronics test on-the-field (400 channels). O. Bourrion et al., JINST 7 (2012) 04/2013 à NIKA-2 Design Review à green light from IRAM 06/2013 à Commissioning (run6). IRAM could decide to open NIKA to external observers in Winter. Sensitivity approaching state-of-the-art. 28

29 2mm NIKA array (132 pixels) 29