Volume 569, September 2014
|Number of page(s)||15|
|Published online||09 September 2014|
Performance and calibration of the NIKA camera at the IRAM 30 m telescope
Laboratoire de Physique Subatomique et de Cosmologie, Université
Grenoble Alpes, CNRS/IN2P3, 53 rue
des Martyrs, 38026
2 Institut Néel, CNRS and Université de Grenoble, 38042 Grenoble, France
3 Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), CNRS and Université de Grenoble, 38041 Grenoble, France
4 Institut de Radio Astronomie Millimétrique (IRAM), 38406 Grenoble, France
5 Astronomy Instrumentation Group, University of Cardiff, UK
6 Laboratoire AIM, CEA/IRFU, CNRS/INSU, Université Paris Diderot, CEA-Saclay, 91191 Gif-Sur-Yvette, France
7 Institut d’Astrophysique Spatiale (IAS), CNRS and Université Paris Sud, 91405 Orsay, Cedex France
8 Institut d’Électronique Fondamentale (IEF), Université Paris Sud, 91405 Orsay, France
9 Institut de Radio Astronomie Millimétrique (IRAM), 18012 Granada, Spain
10 University College London, Department of Physics and Astronomy, Gower Street, London WC1E 6BT, UK
11 Università Sapienza di Roma, 00185 Roma Italy
12 SESE and Physics, Arizona State University, Tempe, AZ, USA
Accepted: 20 June 2014
The New IRAM KID Array (NIKA) instrument is a dual-band imaging camera operating with kinetic inductance detectors (KID) cooled at 100 mK. NIKA is designed to observe the sky at wavelengths of 1.25 and 2.14 mm from the IRAM 30 m telescope at Pico Veleta with an estimated resolution of 13 arcsec and 18 arcsec, respectively. This work presents the performance of the NIKA camera prior to its opening to the astrophysical community as an IRAM common-user facility in early 2014. NIKA is a test bench for the final NIKA2 instrument to be installed at the end of 2015. The last NIKA observation campaigns on November 2012 and June 2013 have been used to evaluate this performance and to improve the control of systematic effects. We discuss here the dynamical tuning of the readout electronics to optimize the KID working point with respect to background changes and the new technique of atmospheric absorption correction. These modifications significantly improve the overall linearity, sensitivity, and absolute calibration performance of NIKA. This is proved on observations of point-like sources for which we obtain a best sensitivity (averaged over all valid detectors) of 40 and 14 mJy s1/2 for optimal weather conditions for the 1.25 and 2.14 mm arrays, respectively. NIKA observations of well known extended sources (DR21 complex and the Horsehead nebula) are presented. This performance makes the NIKA camera a competitive astrophysical instrument.
Key words: methods: observational / submillimeter: general / submillimeter: galaxies / submillimeter: ISM
© ESO, 2014
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.