The Next Generation Space Telescope (NGST)—Scientific requirements

Mather, John C.; Seery, Bernard D.; Bély, Pierre Y.; Stockman, H. S.

doi:10.1063/1.52049

Cited by 2 publications

(2 citation statements)

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“…Issues of solar system zodiacal emission, and the effects of extra-solar zodiacal emission on detection probabilities (Angel 1998), mean that precursor space missions with less ambitious goals have also been proposed (Hinz et al 1999b); telescopes with high finesse active optics to reduce rms aberrations to a few nm could detect Jupiters around a few stars with 3 m apertures and Earth-like planets around 100 stars with 30 m apertures (Malbet et al 1995). Meanwhile the capabilities of the Hubble Space Telescope (Schroeder and Golimowski 1996) (see also section 3.5 and figure 10), NASA's SIRTF (a 0.85 m cryogenically cooled infrared observatory, to be launched in 2002; Cruikshank and Werner 1997) and the planned Next Generation Space Telescope (NGST, to be launched 2009; Mather et al 1997) have been considered for their brown dwarf and planet imaging capabilities.…”

Section: Imagingmentioning

confidence: 99%

Extra-solar planets

Perryman

2000

Rep. Prog. Phys.

146

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The discovery of the first extra-solar planet surrounding a main-sequence star was announced in 1995, based on very precise radial velocity (Doppler) measurements. A total of 34 such planets were known by the end of March 2000, and their numbers are growing steadily. The newly discovered systems confirm some of the features predicted by standard theories of star and planet formation, but systems with massive planets, having very small orbital radii and large eccentricities, are common and were generally unexpected.Other techniques being used to search for planetary signatures include accurate measurement of positional (astrometric) displacements, gravitational microlensing and pulsar timing, the latter resulting in the detection of the first planetary mass bodies beyond our solar system in 1992. The transit of a planet across the face of the host star provides significant physical diagnostics, and the first such detection was announced in 1999. Protoplanetary disks, which represent an important evolutionary stage for understanding planet formation, are being imaged from space. In contrast, direct imaging of extra-solar planets represents an enormous challenge. Long-term efforts are directed towards infrared space interferometry, the detection of Earth-mass planets, and measurement of their spectral characteristics.Theoretical atmospheric models provide predictions of planetary temperatures, radii, albedos, chemical condensates and spectral features as a function of mass, composition and distance from the host star. Efforts to characterize planets occupying the 'habitable zone', in which liquid water may be present, and indicators of the presence of life are advancing quantitatively.

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Section: Imagingmentioning

confidence: 99%

Extra-solar planets

Perryman

2000

Rep. Prog. Phys.

146

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“…With the pending launch of Hubble, NASA started in 1989 to considered the next generation of large aperture space telescopes which would be required to answer the next generation of compelling science questions -this lead to the NGST (Next Generation Space Telescope) project which became the JWST (James Webb Space Telescope) program (1,2,3). From the beginning, mirror technology was identified as a critical capability necessary to enable next generation of large aperture space telescopes.…”

Section: Introductionmentioning

confidence: 99%

JWST primary mirror technology development lessons learned

Stahl

2010

An Optical Believe It or Not: Key Lessons Learned II

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Mirror technology is a critical enabling capability for the James Webb Space Telescope (JWST). JWST requires a Primary Mirror Segment Assembly (PMSA) that can survive launch, deploy and align itself to form a 6.5 meter diameter (25 square meter collecting area) primary mirror with a 131 nm rms wavefront error at temperatures < 50K and provide stable optical performance. At the inception of JWST in 1996, such a capability did not exist. A highly successful technology development program was initiated which achieved TRL-6 in 2007. This paper reviews the technology development program, the methodology for assessing that TRL-6 was achieved, and the importance of an Engineering Development Unit (EDU). Additionally, this paper captures the author"s lessons learned.

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The Next Generation Space Telescope (NGST)—Scientific requirements

Cited by 2 publications

References 4 publications

Extra-solar planets

Extra-solar planets

JWST primary mirror technology development lessons learned

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