The NIKA2 large-field-of-view millimetre continuum camera for the 30 m IRAM telescope

被引：120

作者：

Adam, R. ^{[1
]}

Adane, A. ^{[2
]}

Ade, P. A. R. ^{[3
]}

Andre, P. ^{[4
]}

Andrianasolo, A. ^{[5
]}

Aussel, H. ^{[4
]}

Beelen, A. ^{[6
]}

Benoit, A. ^{[7
,8
]}

Bideaud, A. ^{[7
,8
]}

Billot, N. ^{[9
]}

Bourrion, O. ^{[10
]}

Bracco, A. ^{[4
]}

Calvo, M. ^{[7
,8
]}

Catalano, A. ^{[10
]}

Coiffard, G. ^{[11
]}

Comis, B. ^{[10
]}

De Petris, M. ^{[12
]}

Desert, F. -X. ^{[5
]}

Doyle, S. ^{[3
]}

Driessen, E. F. C. ^{[11
]}

Evans, R. ^{[3
]}

Goupy, J. ^{[7
,8
]}

Kramer, C. ^{[9
]}

Lagache, G. ^{[6
]}

Leclercq, S. ^{[11
]}

Leggeri, J. -P. ^{[7
,8
]}

Lestrade, J. -F. ^{[13
]}

Macias-Perez, J. F. ^{[10
]}

Mauskopf, P. ^{[14
,15
]}

Mayet, F. ^{[10
]}

Maury, A. ^{[4
]}

Monfardini, A. ^{[7
,8
]}

Navarro, S. ^{[9
]}

Pascale, E. ^{[3
]}

Perotto, L. ^{[10
]}

Pisano, G. ^{[3
]}

Ponthieu, N. ^{[5
]}

Reveret, V. ^{[4
]}

Rigby, A. ^{[3
]}

Ritacco, A. ^{[9
]}

Romero, C. ^{[11
]}

Roussel, H. ^{[16
]}

Ruppin, F. ^{[10
]}

Schuster, K. ^{[11
]}

Sievers, A. ^{[9
]}

Triqueneaux, S. ^{[7
,8
]}

Tucker, C. ^{[3
]}

Zylka, R. ^{[11
]}

机构：

[1] Univ & Observ Cote Azur, CNRS, Lab Lagrange, Bd Observ, F-06304 Nice, France

[2] USTHB, BP 32 El Alia, Algiers 16111, Algeria

[3] Univ Cardiff, Astron Instrumentat Grp, Cardiff CF24 3AA, S Glam, Wales

[4] Univ Paris Diderot, CEA Saclay, Lab AIM, CEA,IRFU,CNRS,INSU, F-91191 Gif Sur Yvette, France

[5] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[6] Aix Marseille Univ, CNRS, LAM, F-13388 Marseille, France

[7] CNRS, Inst Neel, 25 Av Martyrs, F-38042 Grenoble, France

[8] UGA, 25 Av Martyrs, F-38042 Grenoble, France

[9] Inst RadioAstron Millimetr IRAM, Granada 18012, Spain

[10] Univ Grenoble Alpes, CNRS, Lab Phys Subatom & Cosmol, 53 Av Martyrs, F-38000 Grenoble, France

[11] Inst RadioAstron Millimetr IRAM, F-38000 Grenoble, France

[12] Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy

[13] Observ Paris, CNRS, LERMA, 61 Ave Observ, F-75014 Paris, France

[14] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA

[15] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA

[16] CNRS, UMR 7095, Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 609卷

基金：

欧洲研究理事会;

关键词：

instrumentation: detectors; instrumentation: photometers; instrumentation: polarimeters; submillimeter: ISM; submillimeter:galaxies; cosmic background radiation; BOLOMETER CAMERA; SCUBA-2; ARRAYS;

D O I：

10.1051/0004-6361/201731503

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Millimetre-wave continuum astronomy is today an indispensable tool for both general astrophysics studies (e.g. star formation, nearby galaxies) and cosmology (e.g. cosmic microwave background and high-redshift galaxies). General purpose, large-field-of-view instruments are needed to map the sky at intermediate angular scales not accessible by the high-resolution interferometers (e.g. ALMA in Chile, NOEMA in the French Alps) and by the coarse angular resolution space-borne or ground-based surveys (e.g. Planck, ACT, SPT). These instruments have to be installed at the focal plane of the largest single-dish telescopes, which are placed at high altitude on selected dry observing sites. In this context, we have constructed and deployed a three-thousand-pixel dual-band (150 GHz and 260 GHz, respectively 2 mm and 1.15 mm wavelengths) camera to image an instantaneous circular field-of-view of 6.5 arcmin in diameter, and configurable to map the linear polarisation at 260 GHz. Aims. First, we are providing a detailed description of this instrument, named NIKA2 (New IRAM KID Arrays 2), in particular focussing on the cryogenics, optics, focal plane arrays based on Kinetic Inductance Detectors, and the readout electronics. The focal planes and part of the optics are cooled down to the nominal 150 mK operating temperature by means of an adhoc dilution refrigerator. Secondly, we are presenting the performance measured on the sky during the commissioning runs that took place between October 2015 and April 2017 at the 30-m IRAM telescope at Pico Veleta, near Granada (Spain). Methods. We have targeted a number of astronomical sources. Starting from beam-maps on primary and secondary calibrators we have then gone to extended sources and faint objects. Both internal (electronic) and on-the-sky calibrations are applied. The general methods are described in the present paper. Results. NIKA2 has been successfully deployed and commissioned, performing in-line with expectations. In particular, NIKA2 exhibits full width at half maximum angular resolutions of around 11 and 17.5 arcsec at respectively 260 and 150 GHz. The noise equivalent flux densities are, at these two respective frequencies, 33 +/- 2 and 8 +/- 1 mJy s(1/2). A first successful science verification run was achieved in April 2017. The instrument is currently offered to the astronomy community and will remain available for at least the following ten years.

引用

页数：15

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