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Comptes Rendus Physique
Volume 18, n° 5-6
pages 323-330 (mai 2017)
Doi : 10.1016/j.crhy.2017.05.002
Superconducting millimetre-wave cameras
Caméras supraconductrices millimétriques pour l'astronomie

Fig. 1

Fig. 1 : 

NIKA2 angular resolution (150 GHz) and field of view compared to one Planck beam. The famous Cygnus A radio-galaxy, mapped by NIKA, is shown in the inset (real data). While NIKA and NIKA2 maps are clearly showing the morphology of the jets and the radio-lobes, Planck only sees a single blob.

Fig. 2

Fig. 2 : 

KID working principle.

Fig. 3

Fig. 3 : 

A classical (single-polarisation) LEKID pixel micrograph. Dark regions are silicon, bright areas are the thin aluminium film making the detector itself.

Fig. 4

Fig. 4 : 

The big (1.3 tons, 2.5 m in length) NIKA2 camera. Left: the optics scheme characterised by the presence of a dichroic to split the two bands (lower frequencies are reflected on the 2.0-mm array) and a polarizer projecting the modulated polarisation onto two arrays H and V operating at 1.15 mm. Right: a picture of NIKA2 in the telescope receivers cabin.

Fig. 5

Fig. 5 : 

The NIKA2 detectors are microstrip-feed resonators. I show here a picture of one of the 1.15-mm arrays actually mounted in NIKA2. The connections to the readout electronics are provided by superconducting micro-bondings, 50-Ω launchers pads and SMA connectors.

Fig. 6

Fig. 6 : 

Multi-wavelength image of the galaxies cluster MACS J0717.5+3745 showing the galaxy distribution (green, Hubble Space Telescope data), the gas electron density (red, Chandra X-ray data), the gas electron pressure (blue, NIKA) and the kSZ signal (yellow contours, NIKA). Solid yellow contours indicate regions of the clusters that are moving toward us, dotted lines show regions moving farther. Taken from [18].

Fig. 7

Fig. 7 : 

Preliminary map of DR21OH observed at 1.15 and 2 mm. Maps are 13 arcmin large, the angular resolution in each band is represented as a white disk at the bottom of the images.

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