The Mid-Infrared Instrument for the James Webb Space Telescope, II: Design and Build

被引：126

作者：

Wright, G. S. ^{[1
]}

Wright, David ^{[2
]}

Goodson, G. B. ^{[3
]}

Rieke, G. H. ^{[4
]}

Aitink-Kroes, Gabby ^{[5
]}

Amiaux, J. ^{[6
]}

Aricha-Yanguas, Ana ^{[7
]}

Azzollini, Ruyman ^{[8
,9
]}

Banks, Kimberly ^{[10
]}

Barrado-Navascues, D. ^{[9
]}

Belenguer-Davila, T. ^{[7
]}

Bloemmart, J. A. D. L. ^{[11
,12
,13
]}

Bouchet, Patrice ^{[6
]}

Brandl, B. R. ^{[14
]}

Colina, L. ^{[9
]}

Detre, Oers ^{[15
]}

Diaz-Catala, Eva ^{[7
]}

Eccleston, Paul ^{[16
]}

Friedman, Scott D. ^{[17
]}

Garcia-Marin, Macarena ^{[18
]}

Guedel, Manuel ^{[19
,20
]}

Glasse, Alistair ^{[1
]}

Glauser, Adrian M. ^{[20
]}

Greene, T. P. ^{[21
]}

Groezinger, Uli ^{[15
]}

Grundy, Tim ^{[16
]}

Hastings, Peter ^{[1
]}

Henning, Th ^{[15
]}

Hofferbert, Ralph ^{[15
]}

Hunter, Faye ^{[22
]}

Jessen, N. C. ^{[23
]}

Justtanont, K. ^{[24
]}

Karnik, Avinash R.

Khorrami, Mori A. ^{[3
]}

Krause, Oliver ^{[15
]}

Labiano, Alvaro ^{[20
]}

Lagage, P. -O. ^{[6
]}

Langer, Ulrich ^{[25
]}

Lemke, Dietrich ^{[15
]}

Lim, Tanya ^{[16
]}

Lorenzo-Alvarez, Jose ^{[26
]}

Mazy, Emmanuel ^{[27
]}

McGowan, Norman ^{[22
]}

Meixner, M. E. ^{[17
,28
]}

Morris, Nigel ^{[16
]}

Morrison, Jane E. ^{[4
]}

Mueller, Friedrich ^{[15
]}

Rgaard-Nielson, H. -U. No ^{[23
]}

Olofsson, Goran ^{[24
]}

O'Sullivan, Brian ^{[29
]}

机构：

[1] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[2] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA

[3] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[4] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[5] NOVA Opt IR Grp, NL-7990 AA Dwingeloo, Netherlands

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

[7] INTA, Madrid 28850, Spain

[8] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland

[9] Ctr Astrobiol INTA CSIC, Dept Astrofis, Madrid 28850, Spain

[10] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[11] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium

[12] Vrije Univ Brussel, Astron & Astrophys Res Grp, Dept Phys & Astrophys, B-1050 Ixelles, Belgium

[13] Flemish Inst Technol Res VITO, B-2400 Mol, Belgium

[14] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[15] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[16] Rutherford Appleton Lab, STFC, RAL Space, Didcot OX11 0QX, Oxon, England

[17] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[18] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany

[19] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria

[20] ETH, Inst Astron, CH-8093 Zurich, Switzerland

[21] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[22] Airbus Def & Space, Portsmouth PO3 5PU, Hants, England

[23] Tech Univ Denmark, Natl Space Inst DTU Space, DK-2100 Copenhagen, Denmark

[24] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden

[25] RUAG Space, CH-8052 Zurich, Switzerland

[26] Estec, NL-2201 AZ Noordwijk, Netherlands

[27] Ctr Spatial Liege, B-4031 Angleur, Belgium

[28] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[29] Airbus Def & Space, Portsmouth PO3 5PU, Hants, England

[30] Univ Groningen, Kapteyn Inst, NL-9700 Groningen, Netherlands

[31] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA

[32] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England

[33] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England

[34] UCL, Dept Phys & Astron, London WC1E 6BT, England

[35] Airbus Def & Space, Stevenage SG1 2AS, Herts, England

[36] Paul Scherrer Inst, CH-5232 Villigen, Switzerland

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 2015年 / 127卷 / 953期

关键词：

RESOLUTION SPECTROMETER; MIRI;

D O I：

10.1086/682253

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) provides measurements over the wavelength range 5 to 28: 5 mu m. MIRI has, within a single "package," four key scientific functions: photometric imaging, coronagraphy, single-source low-spectral resolving power (R similar to 100) spectroscopy, and medium-resolving power (R similar to 1500 to 3500) integral field spectroscopy. An associated cooler system maintains MIRI at its operating temperature of <6.7 K. This paper describes the driving principles behind the design of MIRI, the primary design parameters, and their realization in terms of the "as-built" instrument. It also describes the test program that led to delivery of the tested and calibrated Flight Model to NASA in 2012, and the confirmation after delivery of the key interface requirements.

引用

页码：595 / 611

页数：17

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