EPJ Web Conf.
Volume 228, 2020mm Universe @ NIKA2 - Observing the mm Universe with the NIKA2 Camera
|Number of page(s)||6|
|Published online||27 January 2020|
NIKA2 mapping and cross-instrument SED extraction of extended sources with Scanamorphos
Institut d’Astrophysique de Paris, Sorbonne Université, CNRS (UMR7095), 75014 Paris, France
2 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
3 LLR (Laboratoire Leprince-Ringuet), CNRS, École Polytechnique, Institut Polytechnique de Paris, Palaiseau, France
4 Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, planta 2, E-44001, Teruel, Spain
5 Astronomy Instrumentation Group, University of Cardiff, UK
6 AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, France
7 Institut d’Astrophysique Spatiale (IAS), CNRS and Université Paris Sud, Orsay, France
8 Institut Néel, CNRS and Université Grenoble Alpes, France
9 Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 53, avenue des Martyrs, 38000 Grenoble, France
10 Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 5, I-00185 Roma, Italy
11 Institut de RadioAstronomie Millimétrique (IRAM), Grenoble, France
12 Centro de Astrobiología (CSIC-INTA), Torrejón de Ardoz, 28850 Madrid, Spain
13 Instituto de Radioastronomía Milimétrica (IRAM), Granada, Spain
14 Aix Marseille Univ, CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille), Marseille, France
15 LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, 75014 Paris, France
16 School of Earth and Space Exploration and Department of Physics, Arizona State University, Tempe, AZ 85287
17 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
* e-mail: firstname.lastname@example.org
Published online: 27 January 2020
The steps taken to tailor to NIKA2 observations the Scanamorphos algorithm (initially developed to subtract low-frequency noise from Herschel on-the-fly observations) are described, focussing on the consequences of the different instrument architecture and observation strategy. The method, making the most extensive use of the redundancy built in the multi-scan coverage with large arrays of a given region of the sky, is applicable to extended sources, while the pipeline is so far optimized for compact sources. An example of application is given. A related tool to build consistent broadband SEDs from 60 microns to 2 mm, combining Herschel and NIKA2 data, has also been developed. Its main task is to process the data least affected by low-frequency noise and coverage limitations (i.e. the Herschel data) through the same transfer function as the NIKA2 data, simulating the same scan geometry and applying the same noise and atmospheric signal as extracted from the 1mm and 2mm data.
© The Authors, published by EDP Sciences, 2020
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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