The JWST tunable filter imager (TFI)

Doyon, René; Hutchings, J. B.; Neil, R. H.; Saad, Karl; Abraham, Roberto; Beaulieu, Marie; Ferrarese, Laura; Fullerton, A. W.; Jayawardhana, Ray; Johnstone, Doug; Meyer, M. R.; Pipher, J. L.; Sawicki, Marcin; Sivaramakrishnan, A.

doi:10.1117/12.789504

Cited by 31 publications

(33 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The Canadian contribution to the mission is the Fine Guidance Sensor (FGS). The FGS also incorporates a flexible narrow spectral band science imaging capability which adds to the scientific capabilities of the mission [3]. The FGS design has evolved somewhat since the concept was presented in [4], with the major changes being a reduction in the wavelength range of the science imager (removal of an imaging channel), the incorporation of the FGS software into the ICDH instead of a stand-alone FGS computer, and the adoption of a cryogenic application specific integrated circuit (SIDECAR) to readout each of the 2k x 2k infrared detector arrays, also adopted by JWST's NIRCam and NIRSpec instruments.…”

Section: Fgs Design Descriptionmentioning

confidence: 99%

JWST fine guidance sensor: guiding performance analysis

Rowlands

Vila

Evans

et al. 2008

Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter

Self Cite

View full text Add to dashboard Cite

The Engineering Test Unit (ETU) of the Fine Guidance Sensor (FGS) for the James Webb Space Telescope (JWST) is currently in fabrication. Extensive modeling of the key FGS-Guider performance parameters has been used throughout the design process and continues to be used to evaluate the expected performance of the as-built instrument. A key parameter of interest is the expected Noise Equivalent Angle (NEA) provided by the FGS.The NEA will, in part, determine the ultimate image quality of the JWST Observatory. In this paper we use updated estimates of the End-oflife impact of contamination to present the current expected NEA performance of the FGS flight model. As component test data becomes available this data will be used as input to the FGS NEA performance model to assess the expected performance of the instrument.

show abstract

Section: Fgs Design Descriptionmentioning

confidence: 99%

JWST fine guidance sensor: guiding performance analysis

Rowlands

Vila

Evans

et al. 2008

Space Telescopes and Instrumentation 2008: Optical, Infrared, and Millimeter

Self Cite

View full text Add to dashboard Cite

show abstract

“…FPIs have been selected, for their high performances, to be used in future large missions such as the James Webb Space Telescope, BepiColombo, and Solar Orbiter. [8][9][10] A wide operational spectral range is achieved due to the capacitance-stabilized piezoelectric control of the FPI 11 (which is, in that case, often referred to as CSE-FPI: capacitance-stabilized etalon-FPI) and suitable cameras.…”

Section: Key Technologies and Design Solutionsmentioning

confidence: 99%

ADAHELI+: exploring the fast, dynamic Sun in the x-ray, optical, and near-infrared

Berrilli

Soffitta

Velli

et al. 2015

J. Astron. Telesc. Instrum. Syst

View full text Add to dashboard Cite

Abstract. Advanced Astronomy for Heliophysics Plus (ADAHELI+) is a project concept for a small solar and space weather mission with a budget compatible with an European Space Agency (ESA) S-class mission, including launch, and a fast development cycle. ADAHELI+ was submitted to the European Space Agency by a European-wide consortium of solar physics research institutes in response to the "Call for a small mission opportunity for a launch in 2017," of March 9, 2012. The ADAHELI+ project builds on the heritage of the former ADAHELI mission, which had successfully completed its phase-A study under the Italian Space Agency 2007 Small Mission Programme, thus proving the soundness and feasibility of its innovative low-budget design. ADAHELI+ is a solar space mission with two main instruments: ISODY+: an imager, based on Fabry-Pérot interferometers, whose design is optimized to the acquisition of highest cadence, long-duration, multiline spectropolarimetric images in the visible/near-infrared region of the solar spectrum. XSPO: an x-ray polarimeter for solar flares in x-rays with energies in the 15 to 35 keV range. ADAHELI+ is capable of performing observations that cannot be addressed by other currently planned solar space missions, due to their limited telemetry, or by ground-based facilities, due to the problematic effect of the terrestrial atmosphere. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

show abstract

“…Near-infrared scanning Fabry-Perot imagery is provided by the FGS-TF instrument (Doyon 2008). This instrument provides a narrow-band imaging capability with the same size field of view as the NIRCam and over a similar wavelength range.…”

Section: Extracting Information From Starlightmentioning

confidence: 99%

The James Webb Space Telescope: Mission overview and status

Greenhouse

2011

2011 2nd International Conference on Space Technology

View full text Add to dashboard Cite

Abstract- l. DESIGNING FOR DISCOVERYThe science motivation for the JWST mission was developed by a succession of international science working groups and is described by Gardner et aI. 2006, with updates maintained by the lWST flight science working group 1 at: http://www.stsci.eduljwst/sciencelwhitepapersi . This science case fonns the basis from which detailed science and mission requirements were derived to guide engineering design and development of the lWST as a research tool. The science observations that are actually implemented by the lWST will be proposed by the international astronomical community in response to annual peer reviewed proposal opportunities. The discovery potential of the lWST relative to other concurrent facilities is discussed in Thronson, Stiavelli, and Tielens 2009.The emergence of the first sources of light in the universe (after decoupling) marks the end of the "Dark Ages" in cosmic history (Rees 1997). The ultraviolet radiation field produced by these sources created the ionization that is observed in the local intergalactic medium (10M). The JWST design provides Unique capability to address key questions about this era in cosmic The lWST architecture is prinuirily shaped by requirements associated with answering the above questions. In contrast to the Hubble Space Telescope (HST), the lWST is designed as an infrared optimized telescope to observe the redshifted ultraviolet radiation from the first galaxies and supernovae of the flfSt stars. To achieve the nly sensitivity needed to observe this era (z -6-20), the observatory must have a telescope aperture that is larger in diameter than the largest rocket faring, and the entire optical system must be cooled to -40-50 K. Finally, the resulting large deployable cryogenic telescope must achieve HST-like angular resolution across the SWIR spectrum. The major observatory design features trace directly from these requirements and differ markedly from those of the HST.The lWST science instrument payload is designed to probe the first galaxies with high angular resolution nearinfrared image surveys in broad-band filters. This capability enables identification of primeval galaxies by searching their Lyman continuum break with multi-filter photometry. This prominent feature occurs in the near-infrared (1.3 -2.6 um) for galaxies with redshifts in the range of 10 -20. This broad-band technique exploits the maximum sensitivity of the observatory, such that the space density of galaxies can be probed to z-20. lWST high angular resolution imagery across the 0.6 -29 um spectrum will probe the assembly and evolution of galaxy motphologies to enable observation of when and how the Hubble sequence formed.Tbe lWST is designed to enable near-infrared multiobject spectroscopy of thousands of galaxies at several spectral resolutions (_ 10' , _10'). This capability will probe the chemical evolution and metallicity of galaxies, and the ionization state of the IGM across cosmic time. Low resolution multi-object spectroscopy will enable calibration of ph...

show abstract

The JWST tunable filter imager (TFI)

Cited by 31 publications

References 0 publications

JWST fine guidance sensor: guiding performance analysis

JWST fine guidance sensor: guiding performance analysis

ADAHELI+: exploring the fast, dynamic Sun in the x-ray, optical, and near-infrared

The James Webb Space Telescope: Mission overview and status

Contact Info

Product

Resources

About