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arxiv: 1312.4801 · v1 · pith:QX6NBHSQnew · submitted 2013-12-17 · 🌌 astro-ph.IM

The NIKA instrument: results and perspectives towards a permanent KID based camera for the Pico Veleta observatory

A. D'Addabbo (1) , R. Adam (2) , A. Adane (3) , P. Ade (4) , P. Andr\'e (5) , A. Beelen (6) , B. Belier (7) , A. Benoit (1)
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A. Bideaud (4) N. Billot (8) O. Bourrion (2) M. Calvo (1) A. Catalano (2) G. Coiffard (3) B. Comis (2) F.-X. D\'esert (9) S. Doyle (4) J. Goupy (1) C. Kramer (8) S. Leclercq (3) J. Macias-Perez (2) J. Martino (6) P. Mauskopf (4 10) F. Mayet (2) A. Monfardini (1) F. Pajot (6) E. Pascale (4) N. Ponthieu (9) V. Rev\'eret (5) L. Rodriguez (5) G. Savini (4 11) K. F. Schuster (3) A. Sievers (8) C. Tucker (4) R. Zylka (3) ((1) Institut N\'eel CNRS Universit\'e de Grenoble France (2) Laboratoire de Physique Subatomique et de Cosmologie (LPSC) (3) Institut de RadioAstronomie Millim\'etrique (IRAM) Grenoble (4) Astronomy Instrumentation Group University of Cardiff UK (5) Laboratoire AIM EA/IRFU CNRS/INSU Universit\'e Paris Diderot CEA-Saclay (6) Institut d'Astrophysique Spatiale (IAS) Universit\'e Paris Sud Orsay (7) Institut d'Electronique Fondamentale (IEF) (8) Instituto Radioastronomia Milim\'etrica (IRAM) Granada Spain (9) Institut de Plan\'etologie et d'Astrophysique de Grenoble (IPAG) (10) SESE Dept. of Physics Arizona State University Tempe AZ USA (11) University College London (UCL) UK)
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classification 🌌 astro-ph.IM
keywords cameradevotedinstrumentiramnikapicoveletaaccuracy
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The New IRAM KIDs Array (NIKA) is a pathfinder instrument devoted to millimetric astronomy. In 2009 it was the first multiplexed KID camera on the sky; currently it is installed at the focal plane of the IRAM 30-meters telescope at Pico Veleta (Spain). We present preliminary data from the last observational run and the ongoing developments devoted to the next NIKA-2 kilopixels camera, to be commissioned in 2015. We also report on the latest laboratory measurements, and recent improvements in detector cosmetics and read-out electronics. Furthermore, we describe a new acquisition strategy allowing us to improve the photometric accuracy, and the related automatic tuning procedure.

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