The James Webb Space Telescope science instrument suite: an overview of optical designs

Davila, Pamela S.; Bos, Brent J.; Contreras, James; Evans, Clinton; Greenhouse, Matthew A.; Hobbs, Gurnie; Holota, Wolfgang; Huff, Lynn W.; Hutchings, J. B.; Jamieson, Thomas; Lightsey, Paul A.; Morbey, C. L.; Murowinski, Richard; Rieke, M. J.; Rowlands, Neil; Steakley, Bruce; Wells, Martyn; Plate, Maurice B. J. te; Wright, Gillian

doi:10.1117/12.552053

Cited by 15 publications

(8 citation statements)

References 9 publications

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“…The main wavefront sensing camera is the shortwave channel of the Near Infrared Camera scientific instrument (NIRCam A). 2 Much of the discussion in this paper pertains to steps 4, 5, and 6 of the baseline wavefront commissioning process. That is, the JWST primary and secondary mirror fine-phasing and MIMF steps.…”

Section: Wavefront Commissioning Processmentioning

confidence: 99%

Presentation, analysis, and simulation of active alignment strategies for the James Webb Space Telescope

Upton

2009

SPIE Proceedings

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This paper presents three characteristics in the simulated active alignment strategy of the James Webb Space Telescope. The first includes the analysis and comparison of a baseline active alignment strategy with a damped least squares strategy. This baseline utilizes prior knowledge by means of direct human operator interaction to engage sets of telescope compensators to target specific aberration signatures. The baseline is compared to a damped least-squares strategy that utilizes simultaneous engagement of all telescope compensators without explicit human operator interaction to achieve a least-squares telescope compensation. Second, we discuss how the active alignment of the JWST is encapsulated in a linear optical model developed at the Space Telescope Science Institute. This linear optical model provides a framework for an efficient and robust description of the optical control properties of the JWST and clearly articulates the necessity for having a multi-instrument multifield wavefront sensing strategy to overcome control system non independence and the effects of non-common path errors in the main wavefront sensing camera. Finally, we present analytical results that explicitly map the telescope wavefront responses to the telescope control modes, and we present Monte-Carlo optical performance simulation results that demonstrate the efficacy of the damped least-squares active alignment and the priorknowledge active alignment schemes.

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Section: Wavefront Commissioning Processmentioning

confidence: 99%

Presentation, analysis, and simulation of active alignment strategies for the James Webb Space Telescope

Upton

2009

SPIE Proceedings

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“…the Euclid mission 14 and the James Webb Space Telescope (JWST). 15,16 The GAME 17,18 and AGP 19,20 concepts (submitted respectively to the M3 and M4 ESA Calls) also rely on a TMA derived telescope, enforcing the concepts of differential measurement of fields close to the Sun, affected by fairly large light deflection, with a dedicated design deployed around a coronagraphic subsystem. TMAs may achieve extremely good performance, but they also feature comparably high sensitivity to misalignment, 21 as understandable from their large étendue (product of aperture area and field angular coverage).…”

Section: Concept Development and Optical Designmentioning

confidence: 99%

RAFTER: Ring Astrometric Field Telescope for Exo-planets and Relativity

Riva

Gai

Vecchiato

et al. 2020

Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave

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High precision astrometry aims at source position determination to a very small fraction of the diffraction image size, in high SNR regime. One of the key limitations to such goal is the optical response variation of the telescope over a sizeable FOV, required to ensure bright reference objects to any selected target. The issue translates into severe calibration constraints, and/or the need for complex telescope and focal plane metrology. We propose an innovative system approach derived from the established TMA telescope concept, extended to achieve high filling factor of an annular field of view around the optical axis of the telescope. The proposed design is a very compact, 1 m class telescope compatible with modern CCD and CMOS detectors (EFL = 15 m). We describe the concept implementation guidelines and the optical performance of the current optical design. The diffraction limited FOV exceeds 1.25 square degrees, and the detector occupies the best 0.25 square degree with 66 devices.

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“…The James Webb Space Telescope (JWST) is expected to be launched in March 2021. A Near-Infrared Spectrometer (NIRSpec) and camera (NIRCam) are included within the instrument suite [17] and thus will provide the infrared capability that is currently missing (0.6 -5.3µm and 0.6 -5.0µm respectively). Additionally, the Mid-Infrared Instrument (MIRI) covers the wavelength range 5 -28µm and is capable of medium resolution spectroscopy whilst the Near-Infrared Imager and Slitless Spectrograph (NIRISS) will cover visible and near infrared wavelengths from 0.6 -5.0µm [72].…”

Section: Characterisation Of Exoplanet Atmospheres From Spacementioning

confidence: 99%

Exoplanet spectroscopy and photometry with the Twinkle space telescope

et al. 2018

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The Twinkle space telescope has been designed for the characterisation of exoplanets and Solar System objects. Operating in a low Earth, Sunsynchronous orbit, Twinkle is equipped with a 45 cm telescope and visible (0.4 -1µm) and infrared (1.3 -4.5µm) spectrometers which can be operated simultaneously. Twinkle is a general observatory which will provide on-demand observations of a wide variety of targets within wavelength ranges that are currently not accessible using other space telescopes or accessible only to oversubscribed observatories in the short-term future.Here we explore the ability of Twinkle's spectrometers to characterise the currently-known exoplanets. We study the spectral resolution achievable by combining multiple observations for various planetary and stellar types. We also simulate spectral retrievals for some well-known planets (HD 209458 b, GJ 3470 b and 55 Cnc e).From the exoplanets known today, we find that with a single transit or eclipse, Twinkle could probe 89 planets at low spectral resolution (R <20) as well as 12 planets at higher resolution (R >20) in channel 1 (1.3 -4.5µm). With 10 observations, the atmospheres of 144 planets could be characterised with R <20 and 81 at higher resolutions.Upcoming surveys will reveal thousands of new exoplanets, many of which will be located within Twinkle's field of regard. TESS in particular 1 arXiv:1811.08348v2 [astro-ph.EP]

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The James Webb Space Telescope science instrument suite: an overview of optical designs

Cited by 15 publications

References 9 publications

Presentation, analysis, and simulation of active alignment strategies for the James Webb Space Telescope

Presentation, analysis, and simulation of active alignment strategies for the James Webb Space Telescope

RAFTER: Ring Astrometric Field Telescope for Exo-planets and Relativity

Exoplanet spectroscopy and photometry with the Twinkle space telescope

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