Improved mm-wave photometry for kinetic inductance detectors

¹ Institut Néel, CNRS & Université Joseph Fourier, BP 166, 38042 Grenoble, France
e-mail: martino.calvo@grenoble.cnrs.fr
² Institut de RadioAstronomie Millimétrique, 300 rue de la Piscine, 38406 Saint-Martin d’ Hères, France
³ IPAG, Observatoire de Grenoble, BP 53, 38041 Grenoble, France
⁴ Cardiff School of Physics and Astronomy, Cardiff University, CF24 3AA, UK
⁵ LPSC, UJF Grenoble 1, CNRS/IN2P3, INPG, 53 rue des Martyrs, 38026 Grenoble Cedex, France
⁶ Università di Roma La Sapienza, 00185 Roma, Italy
⁷ Dept. of Physics and SESE, Arizona State University, Tempe, Arizona, 85287, USA

Received: 3 December 2012
Accepted: 7 February 2013

Abstract

Context. We have developed a dual-band (140 and 220 GHz) mm-wave imaging camera based on superconducting kinetic inductance detector (KID) arrays. Each array contains 132 superconducting resonators whose resonant frequencies are shifted by mm-wave photons absorption. The read out is achieved with a single electronics chain per band, taking advantage of the intrinsic KID frequency-domain multiplexability. The arrays are easily scalable and well adapted for future large format focal plane instruments. NIKA (formerly Néel IRAM KID Array, now New IRAM KID Array) has been specifically designed for the IRAM 30 m telescope at Pico Veleta, and is one of the first instruments using KIDs to have made measurements of astronomical sources.

Aims. In this Letter we describe the solutions adopted to improve the calibration accuracy and the sensitivity of the instrument, and we report on the outcome of the 3rd NIKA observing run of October, 2011.

Methods. We use a fast electronic modulation of the readout tone for each KID pixel in order to linearize the instrument calibration, which we track with measurements of planets. We also adopt a new design of the KIDs, sensitive to both polarizations, to increase the amount of radiation absorbed and thus the optical efficiency of the system.

Results. We measured an average sensitivity on the sky of 21 mJys^0.5 per beam at 140 GHz and 140 mJys^0.5 at 220 GHz in the best observing conditions (τ₂₂₀ ≃ 0.2) after atmospheric noise decorrelation. The sensitivity at 220 GHz was limited by the atmospheric attenuation and loading as well as a reduction in the spectral bandwidth due to a misplaced filter. We found the repeatability in the photometry over the entire observing run to be better than 10% in both bands, thus demonstrating a significant improvement over the previous runs. We also find good agreement between NIKA measurements of faint astronomical sources and previous measurements of the same sources.