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FältnamnIndikatorerMetadata
00005969naa a2200613 4500
001oai:research.chalmers.se:97425faa-c543-4014-97b7-00477a2c6b97
003SwePub
008230603s2023 | |||||||||||000 ||eng|
0247 a https://doi.org/10.1051/0004-6361/2022456332 DOI
0247 a https://research.chalmers.se/publication/5360572 URI
040 a (SwePub)cth
041 a engb eng
042 9 SwePub
072 7a art2 swepub-publicationtype
072 7a ref2 swepub-contenttype
1001 a Gasman, Dannyu Katholieke Universiteit Leuven4 aut
2451 0a JWST MIRI/MRS in-flight absolute flux calibration and tailored fringe correction for unresolved sources
264 c 2023-03-17
264 1b EDP Sciences,c 2023
338 a electronic2 rdacarrier
520 a Context. The Medium Resolution Spectrometer (MRS) is one of the four observing modes of JWST/MIRI. Using JWST in-flight data of unresolved (point) sources, we can derive the MRS absolute spectral response function (ASRF) starting from raw data. Spectral fringing, caused by coherent reflections inside the detector arrays, plays a critical role in the derivation and interpretation of the MRS ASRF. The fringe corrections implemented in the current pipeline are not optimal for non-extended sources, and a high density of molecular features particularly inhibits an accurate correction. Aims. In this paper, we present an alternative way to calibrate the MIRI/MRS data. Firstly, we derive a fringe correction that accounts for the dependence of the fringe properties on the MIRI/MRS pupil illumination and detector pixel sampling of the point spread function. Secondly, we derive the MRS ASRF using an absolute flux calibrator observed across the full 5- 28 µm wavelength range of the MRS. Thirdly, we apply the new ASRF to the spectrum of a G dwarf and compare it with the output of the JWST/MIRI default data reduction pipeline. Finally, we examine the impact of the different fringe corrections on the detectability of molecular features in the G dwarf and K giant. Methods. The absolute flux calibrator HD 163466 (A-star) was used to derive tailored point source fringe flats at each of the default dither locations of the MRS. The fringe-corrected point source integrated spectrum of HD 163466 was used to derive the MRS ASRF using a theoretical model for the stellar continuum. A cross-correlation was run to quantify the uncertainty on the detection of CO, SiO, and OH in the K giant and CO in the G dwarf for different fringe corrections. Results. The point-source-tailored fringe correction and ASRF are found to perform at the same level as the current corrections, beating down the fringe contrast to the sub-percent level in the G dwarf in the longer wavelengths, whilst mitigating the alteration of real molecular features. The same tailored solutions can be applied to other MRS unresolved targets. Target acquisition is required to ensure the pointing is accurate enough to apply this method. A pointing repeatability issue in the MRS limits the effectiveness of the tailored fringe flats is at short wavelengths. Finally, resulting spectra require no scaling to make the sub-bands match, and a dichroic spectral leak at 12.2 µm is removed.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
650 7a NATURVETENSKAPx Fysikx Atom- och molekylfysik och optik0 (SwePub)103022 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Atom and Molecular Physics and Optics0 (SwePub)103022 hsv//eng
653 a Instrumentation: detectors
653 a Infrared: stars
653 a Methods: data analysis
653 a Instrumentation: spectrographs
7001 a Argyriou, Ioannisu Katholieke Universiteit Leuven4 aut
7001 a Sloan, G. C.u The University of North Carolina System,Space Telescope Science Institute (STScI)4 aut
7001 a Aringer, B.u Universität Wien,University of Vienna4 aut
7001 a Álvarez-Márquez, J.u European Space Astronomy Centre (ESAC)4 aut
7001 a Fox, Ori D.u Space Telescope Science Institute (STScI)4 aut
7001 a Glasse, A.u UK Astronomy Technology Centre4 aut
7001 a Glauser, A. M.u Eidgenössische Technische Hochschule Zürich (ETH),Swiss Federal Institute of Technology in Zürich (ETH)4 aut
7001 a Jones, O. C.u UK Astronomy Technology Centre4 aut
7001 a Justtanont, Kay,d 1965u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)justtano
7001 a Kavanagh, Patricku Dublin Institute for Advanced Studies4 aut
7001 a Klaassen, Pamelau UK Astronomy Technology Centre4 aut
7001 a Labiano, A.u European Space Astronomy Centre (ESAC)4 aut
7001 a Larson, K.u Space Telescope Science Institute (STScI)4 aut
7001 a Law, David R.u Space Telescope Science Institute (STScI)4 aut
7001 a Mueller, M.u Rijksuniversiteit Groningen,University of Groningen4 aut
7001 a Nayak, Omnarayaniu Space Telescope Science Institute (STScI)4 aut
7001 a Noriega-Crespo, A.u Space Telescope Science Institute (STScI)4 aut
7001 a Patapis, P.u Eidgenössische Technische Hochschule Zürich (ETH),Swiss Federal Institute of Technology in Zürich (ETH)4 aut
7001 a Royer, Pierreu Katholieke Universiteit Leuven4 aut
7001 a Vandenbussche, B.u Katholieke Universiteit Leuven4 aut
7102 a Katholieke Universiteit Leuvenb The University of North Carolina System4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 673q 673x 0004-6361x 1432-0746
8564 u https://research.chalmers.se/publication/536057/file/536057_Fulltext.pdfx primaryx freey FULLTEXT
8564 8u https://doi.org/10.1051/0004-6361/202245633
8564 8u https://research.chalmers.se/publication/536057

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