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http://hdl.handle.net/20.500.12666/233
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Campo DC | Valor | Idioma |
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dc.rights.license | © ESO 2020 | - |
dc.contributor.author | Argyriou, I. | - |
dc.contributor.author | Wells, M. | - |
dc.contributor.author | Glasse, A. | - |
dc.contributor.author | Lee, D. | - |
dc.contributor.author | Royer, P. | - |
dc.contributor.author | Vandenbussche, B. | - |
dc.contributor.author | Malamuth, E. | - |
dc.contributor.author | Glauser, A. | - |
dc.contributor.author | Kavanagh, P. J. | - |
dc.contributor.author | Labiano, Á. | - |
dc.contributor.author | Lahuis, F. | - |
dc.contributor.author | Mueller, M. | - |
dc.contributor.author | Patapis, P. | - |
dc.contributor.other | Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737 | - |
dc.date.accessioned | 2021-04-12T09:52:42Z | - |
dc.date.available | 2021-04-12T09:52:42Z | - |
dc.date.issued | 2020-09-23 | - |
dc.identifier.citation | Astronomy and Astrophysics | es |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.other | https://www.aanda.org/articles/aa/full_html/2020/09/aa37535-20/aa37535-20.html | - |
dc.identifier.uri | http://hdl.handle.net/20.500.12666/233 | - |
dc.description.abstract | Context. As is common for infrared spectrometers, the constructive and destructive interference in different layers of the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) detector arrays modulate the detected signal as a function of wavelength. The resulting “fringing” in the Medium-Resolution Spectrometer (MRS) spectra varies in amplitude between 10% and 30% of the spectral baseline. A common method for correcting for fringes relies on dividing the data by a fringe flat. In the case of MIRI MRS, the fringe flat is derived from measurements of an extended, spatially homogeneous source acquired during the thermal-vacuum ground verification of the instrument. While this approach reduces fringe amplitudes of extended sources below the percent level, at the detector level, point source fringe residuals vary in a systematic way across the point spread function. The effect could hamper the scientific interpretation of MRS observations of unresolved sources, semi-extended sources, and point sources in crowded fields. Aims. We find MIRI MRS point source fringes to be reproducible under similar observing conditions. We want to investigate whether a generic and accurate correction can be determined. Therefore, we want to identify the variables, if they exist, that would allow for a parametrization of the signal variations induced by point source fringe modulations. Methods. We determine the point source fringe properties by analyzing MRS detector plane images acquired on the ground. We extracted the fringe profile of multiple point source observations and studied the amplitude and phase of the fringes as a function of field position and pixel sampling of the point spread function of the optical chain. Results. A systematic variation in the amplitude and phase of the point source fringes is found over the wavelength range covered by the test sources (4.9 − 5.8 μm). The variation depends on the fraction of the point spread function seen by the detector pixel. We identify the non-uniform pixel illumination as the root cause of the reported systematic variation. This new finding allows us to reconcile the point source and extended source fringe patterns observed in test data during ground verification. We report an improvement after correction of 50% on the 1σ standard deviation of the spectral continuum. A 50% improvement is also reported in line sensitivity for a benchmark test with a spectral continuum of 100 mJy. The improvement in the shape of weak lines is illustrated using a T Tauri model spectrum. Consequently, we verify that fringes of extended sources and potentially semi-extended sources and crowded fields can be simulated by combining multiple point source fringe transmissions. Furthermore, we discuss the applicability of this novel fringe-correction method to the MRS data (and the data of other instruments). | es |
dc.description.sponsorship | Ioannis Argyriou, Pierre Royer, and Bart Vandenbussche thank the European Space Agency (ESA) and the Belgian Federal Science Policy Office (BELSPO) for their support in the framework of the PRODEX Programme. Patrick Kavanagh thanks the European Space Agency (ESA) and Enterprise Ireland for their support in the framework of the PRODEX Programme. Alvaro Labiano acknowledges the support from Comunidad de Madrid through the Atraccion de Talento grant 2017-T1/TIC-5213. Ioannis Argyriou also thanks Clio Gielen (KU Leuven, Belgium) for many useful and stimulating discussions. The work presented is the effort of the entire MIRI team and the enthusiasm within the MIRI partnership is a significant factor in its success. MIRI draws on the scientific and technical expertise of the following organisations: Ames Research Center, USA; Airbus Defence and Space, UK; CEA-Irfu, Saclay, France; Centre Spatial de Liege, Belgium; Consejo Superior de Investigaciones Cientificas, Spain; Carl Zeiss Optronics, Germany; Chalmers University of Technology, Sweden; Danish Space Research Institute, Denmark; Dublin Institute for Advanced Studies, Ireland; European Space Agency, Netherlands; ETCA, Belgium; ETH Zurich, Switzerland; Goddard Space Flight Center, USA; Institute d'Astrophysique Spatiale, France; Instituto Nacional de Tecnica Aeroespacial, Spain; Institute for Astronomy, Edinburgh, UK; Jet Propulsion Laboratory, USA; Laboratoire d'Astrophysique de Marseille (LAM), France; Leiden University, Netherlands; Lockheed Advanced Technology Center (USA); NOVA Opt-IR group at Dwingeloo, Netherlands; Northrop Grumman, USA; Max-Planck Institut fur Astronomie (MPIA), Heidelberg, Germany; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique (LESIA), France; Paul Scherrer Institut, Switzerland; Raytheon Vision Systems, USA; RUAG Aerospace, Switzerland; Rutherford Appleton Laboratory (RAL Space), UK; Space Telescope Science Institute, USA; Toegepast- Natuurwetenschappelijk Onderzoek (TNO-TPD), Netherlands; UK Astronomy Technology Centre, UK; University College London, UK; University of Amsterdam, Netherlands; University of Arizona, USA; University of Bern, Switzerland; University of Cardiff, UK; University of Cologne, Germany; University of Ghent; University of Groningen, Netherlands; University of Leicester, UK; University of Leuven, Belgium; University of Stockholm, Sweden; Utah State University, USA. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration We would like to thank the following National and International Funding Agencies for their support of the MIRI development: NASA; ESA; Belgian Science Policy Office; Centre Nationale D'Etudes Spatiales (CNES); Danish National Space Centre; Deutsches Zentrum fur Luft-und Raumfahrt (DLR); Enterprise Ireland; Ministerio De Economia y Competividad; Netherlands Research School for Astronomy (NOVA); Netherlands Organisation for Scientific Research (NWO); Science and Technology Facilities Council; Swiss Space Office; Swedish National Space Board; UK Space Agency. We take this opportunity to thank the ESA JWST Project team and the NASA Goddard ISIM team for their capable technical support in the development of MIRI, its delivery and successful integration; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737). | es |
dc.language.iso | eng | es |
dc.publisher | EDP Sciences | es |
dc.rights | Attribution-NonCommercial-NoDerivatives 4.0 International | * |
dc.rights.uri | https://creativecommons.org/licenses/by-nc-nd/4.0/ | * |
dc.subject | Instrumentation: detectors | es |
dc.subject | Instrumentation: spectrographs | es |
dc.subject | Methods: data analysis | es |
dc.subject | Infrared: general | es |
dc.title | The nature of point source fringes in mid-infrared spectra acquired with the James Webb Space Telescope | es |
dc.type | info:eu-repo/semantics/article | es |
dc.contributor.orcid | Argyriou, I. [0000-0003-2820-1077] | - |
dc.contributor.orcid | Patapis, P. [0000-0001-8718-3732] | - |
dc.identifier.doi | 10.1051/0004-6361/202037535 | - |
dc.identifier.e-issn | 1432-0746 | - |
dc.contributor.funder | Comunidad de Madrid | - |
dc.description.peerreviewed | Peer review | es |
dc.identifier.funder | http://dx.doi.org/10.13039/100012818 | - |
dc.type.hasVersion | info:eu-repo/semantics/publishedVersion | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
dc.type.coar | http://purl.org/coar/resource_type/c_6501 | - |
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