mm Universe @ NIKA2
Observations with KIDs Interferometer Spectrum Survey (KISS)
A. Fasano1[1], A. Catalano2, J. F. Macías-Pérez2, M. Aguiar4,5, A. Beelen1, A. Benoit3, A. Bideaud3, J. Bounmy2, O. Bourrion2, G. Bres3, M. Calvo3, J. A. Castro-Almazán4,5, P. de Bernardis6, M. De Petris6, A. P. de Taoro4,5, M. Fernández-Torreiro4,5, G. Garde3, R. Génova-Santos4,5, A. Gomez7, M. F. Gómez-Renasco4,5, J. Goupy3, C. Hoarau2, R. Hoyland4,5, G. Lagache1, J. Marpaud2, M. Marton2, A. Monfardini3, M. W. Peel4,5, G. Pisano8, N. Ponthieu9, R. Rebolo4,5, S. Roudier2, J. A. Rubiño-Martín4,5, D. Tourres2, C. Tucker8, and C. Vescovi2
1Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
2Univ. Grenoble Alpes, CNRS, LPSC/IN2P3, 38000 Grenoble, France
3Univ. Grenoble Alpes, CNRS, Grenoble INP, Institut Néel, 38000 Grenoble, France
4Instituto de Astrofísica de Canarias, C/Vía Láctea, E-38205 La Laguna, Tenerife, Spain
5Universidad de La Laguna, Dept. Astrofísica, E-38206 La Laguna, Tenerife, Spain
6Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, I-00185 Roma, Italy
7Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, E-28850, Madrid, Spain
8Astronomy Instrumentation Group, University of Cardiff, The Parade CF24 3AA, UK
9Univ. Grenoble Alpes, CNRS, IPAG, 38400 Saint Martin d’Hères, France
Abstract. We describe the preliminary on-sky results of the KIDs Interferometer Spectrum Survey (KISS), a spectral imager with a 1 deg field of view (FoV). The instrument operates in the range 120–180 GHz from the 2.25 m Q-U-I JOint TEnerife telescope in Teide Observatory (Tenerife, Canary Islands), at 2 395 m altitude above sea level. Spectra at low resolution, up to 1.45 GHz, are obtained using a fast (3.72 Hz mechanical frequency) Fourier transform spectrometer, coupled to a continuous dilution cryostat with a stabilized temperature of 170 mK that hosts two 316-pixel arrays of lumped-element kinetic inductance detectors. KISS generates more than 3 000 spectra per second during observations and represents a pathfinder to demonstrate the potential for spectral mapping with large FoV. We give an overall description of the spectral mapping paradigm and we present recent results from observations, in this paper.
1 Introduction
In the millimeter (mm) astronomy domain, there is a strong demand from the scientific community to develop multi-band instruments for component separation, foreground characterization, cosmic microwave background spectral distortions and line intensity mapping [1]. An interesting instrumental candidate to meet these demands is the exploitation of Fourier transform spectrometers (FTSs) and, in particular, the Martin-Puplett interferometer (MPI)
- ↑ Corresponding author: Alessandro Fasano, alessandro.fasano@lam.fr
© The Authors, published by EDP Sciences. This is an open access article distributed under the terms of the Creative Commons Attribution License 4.0 (http://creativecommons.org/licenses/by/4.0/).
