CONCERTO at APEX On-sky performance in continuum

被引：0

作者：

Hu, W. ^{[1
,2
]}

Beelen, A. ^{[1
]}

Lagache, G. ^{[1
]}

Fasano, A. ^{[1
,3
,4
]}

Lundgren, A. ^{[1
]}

Ade, P. ^{[5
]}

Aravena, M. ^{[6
]}

Barria, E. ^{[7
]}

Benoit, A. ^{[7
]}

Bethermin, M. ^{[1
,8
]}

Bounmy, J. ^{[9
]}

Bourrion, O. ^{[9
]}

Bres, G. ^{[7
]}

De Breuck, C. ^{[10
]}

Calvo, M. ^{[7
]}

Catalano, A. ^{[9
]}

Desert, F.-X. ^{[11
]}

Dubois, C. ^{[1
]}

Duran, C.A. ^{[12
]}

Fenouillet, T. ^{[1
]}

Garcia, J. ^{[1
]}

Garde, G. ^{[7
]}

Goupy, J. ^{[7
]}

Hoarau, C. ^{[9
]}

Lambert, J.-C. ^{[1
]}

Lellouch, E. ^{[13
]}

Levy-Bertrand, F. ^{[7
]}

Macias-Perez, J. ^{[9
]}

Marpaud, J. ^{[9
]}

Monfardini, A. ^{[7
]}

Pisano, G. ^{[5
]}

Ponthieu, N. ^{[11
]}

Prieur, L. ^{[1
]}

Quinatoa, D. ^{[14
]}

Roni, S. ^{[9
]}

Roudier, S. ^{[9
]}

Tourres, D. ^{[9
]}

Tucker, C. ^{[5
]}

Van Cuyck, M. ^{[1
]}

机构：

[1] Aix-Marseille Univ, CNRS, CNES, LAM, Marseille, France

[2] Department of Physics and Astronomy, University of the Western Cape, Robert Sobukhwe Road, Bellville,7535, South Africa

[3] Instituto de Astrofísica de Canarias, La Laguna, Tenerife,38205, Spain

[4] Departamento de Astrofísica, Universidad de La Laguna (ULL), La Laguna, Tenerife,38206, Spain

[5] Astronomy Instrumentation Group, University of Cardiff, The Parade, CF24 3AA, United Kingdom

[6] Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile

[7] Univ. Grenoble Alpes, CNRS, Grenoble INP, Institut Néel, Grenoble,38000, France

[8] Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, Strasbourg,67000, France

[9] Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 53, avenue des Martyrs, Grenoble,38000, France

[10] European Southern Observatory, Karl Schwarzschild Straße 2, Garching,85748, Germany

[11] Univ. Grenoble Alpes, CNRS, IPAG, Saint-Martin-d’Hères,38400, France

[12] Instituto de Radioastronomía Milimétrica (IRAM), Granada, Spain

[13] LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universite, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cite, 5 place Jules Janssen, Meudon,92195, France

[14] Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña 1111, Valparaíso, Chile

来源：

Astronomy and Astrophysics | 2024年 / 689卷

关键词：

Besides the authors; the technicians and engineers more involved in the experimental setup development have been Maurice Grollier; Olivier Exshaw; Anne Gerardin; Gilles Pont; Guillaume Donnier-Valentin; Philippe Jeantet; Mathilde Heigeas; Christophe Vescovi; and Marc Marton. We acknowledge the crucial contributions of the whole Cryogenics and Electronics groups at Institut Nu00E9el and LPSC. We acknowledge the contribution of Hamdi Mani; Chris Groppi; and Philip Mauskopf (from the School of Earth and Space Exploration and Department of Physics; Arizona State University) to the cold electronics. The KID arrays of CONCERTO have been produced at the PTA Grenoble microfabrication facility. We warmly thank the support from the APEX staff for their help in CONCERTO pre-installations and design. The flexible pipes; in particular; have been routed under the competent coordination of Jorge Santana and Marcelo Navarro. We acknowledge support from the European Research Council (ERC) under the European Unionu2019s Horizon 2020 research and innovation programme (project CONCERTO; grant agreement No 788212); from the Excellence Initiative of Aix-Marseille University-A*Midex; a French u201CInvestissements du2019Aveniru201D programme; from the LabEx FOCUS ANR- 11-LABX-0013; and from the ECOS-ANID French and Chilian cooperation program. DQ acknowledges support from the National Agency for Research and Development (ANID)/Scholarship Program/Doctorado Nacional/2021-21212222 and ECOS-ANID NECOS220016. This work has also been supported by the GIS KIDs. We are grateful to our administrative staff in Grenoble and Marseille; in particular Patricia Poirier; Mathilde Berard; Lilia Todorov and Valu00E9rie Favre; and the Protisvalor team. We acknowledge the crucial help of the Institut Nu00E9el and MCBT Heads (Etienne Bustarret; Klaus Hasselbach; Thierry Fournier; Laurence Magaud) during the COVID-19 restriction period. M.A. acknowledges support from FONDECYTgrant 1211951 and ANID BASAL project FB210003;

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摘要：

Context. CarbON CII line in post-rEionisation and ReionisaTiOn epoch (CONCERTO) instrument is a low-resolution mapping spectrometer based on lumped element kinetic inductance detector (LEKIDs) technology, operating at 130-310 GHz. It was installed on the 12-metre APEX telescope in Chile in April 2021 and was in operation until May 2023. CONCERTO’s main goals were the observation of [CII]-emission line fluctuations at high redshift and of the Sunyaev-Zel’dovich (SZ) signal from galaxy clusters. Aims. We present the data processing algorithms and the performance of CONCERTO in continuum by analysing the data from the commissioning and scientific observations. Methods. We developed a standard data processing pipeline to proceed from the raw data to continuum maps. Using a large dataset of calibrators (Uranus, Mars, and quasars) acquired in 2021 and 2022 at the APEX telescope across a wide range of atmospheric conditions, we measured the CONCERTO continuum performance and tested its stability against observing conditions. Further, using observations on the COSMOS field and observations targeting a distant sub-millimetre galaxy in the UDS field, we assessed the robustness of the CONCERTO performance on faint sources and compared our measurements with expectations. Results. The beam pattern is characterised by an effective full width at half maximum (FWHM) of 31.9 ± 0.6′′ and 34.4 ± 1.0′′ for high-frequency (HF) and low-frequency (LF) bands, respectively. The main beam is slightly elongated with a mean eccentricity of 0.46. Two error beams of ∼65′′ and ∼130′′ are characterised, allowing us to estimate a main beam efficiency of ∼0.52. The field of view is accurately reconstructed and presents coherent distortions between the HF and LF arrays. LEKID parameters were robustly determined for 80% of the read tones. Cross-talks between LEKIDs are the first cause of flagging, followed by an excess of eccentricity for ∼10% of the LEKIDs, all located in a given region of the field of view. Of the 44 scans of Uranus selected for the absolute photometric calibration, 72.5% and 78.2% of the LEKIDs were selected as valid detectors with a probability >70%. By comparing the Uranus measurements with a model, we obtain calibration factors of 19.5±0.6 Hz Jy−1 and 25.6±0.9 Hz Jy−1 for HF and LF, respectively. The point-source continuum measurement uncertainties are 3.0% and 3.4% for the HF and LF bands, ignoring the uncertainty in the model (which is −1 s1/2 and 95±1 mJy beam−1 s1/2, respectively, obtained using CONCERTO data on the COSMOS field for a mean precipitable water vapour (pwv) and elevation of 0.81 mm and 55.7 deg. Conclusions. CONCERTO has unique capabilities in fast dual-band spectral mapping at ∼30 arcsec resolution and with a ∼18.5 arcmin instantaneous field of view. CONCERTO’s performance in continuum is perfectly in line with expectations. © The Authors 2024.

引用

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