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  • 1
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    Science Press
    In:  Professional Paper, Open-File Rept., Geological and Ecological Studies of Qinghai-Xizang Plateau, Proceedings of the Symposium on Qinghai-Xizang (Tibet) Plateau, Beijing, China, Science Press, vol. I, Geology, Geological History and Origin of the Qinghai-Xizang Plateau, no. 16, pp. 691-709, (ISBN 1-86239-165-3, vi + 330 pp.)
    Publication Date: 1981
    Keywords: Deep seismic sounding (espec. cont. crust) ; CRUST ; Tibet ; earth mantle ; BIBTEX?
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  • 2
    Publication Date: 2018-06-08
    Keywords: Instrumentation and Photography
    Type: Innovative Designs for the Next Large Aperture Optical/UV Telescope (NHST); Baltimore, MD; United States
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  • 3
    Publication Date: 2018-06-08
    Keywords: Instrumentation and Photography
    Type: Toward Other Earths: Darwin/TPF and the Search for Extrasolar Terrestrial Planets; Heidelberg; Germany
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  • 4
    Publication Date: 2011-08-24
    Description: Two alternative input sequences are commonly employed in correlation chromatography (CC). They are sequences derived according to the algorithm of the feedback shift register (i.e., pseudo random binary sequences (PRBS)) and sequences derived by using the uniform random binary sequences (URBS). These two sequences are compared. By applying the "cleaning" data processing technique to the correlograms that result from these sequences, we show that when the PRBS is used the S/N of the correlogram is much higher than the one resulting from using URBS.
    Keywords: Exobiology
    Type: Analytica chimica acta (ISSN 0003-2670); Volume 324; 1; 29-36
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  • 5
    Publication Date: 2011-08-24
    Description: Narrow-angle astrometry with long-baseline infrared interferometers can provide extremely high accuracies as required for indirect planet detection. Narrow-angle astrometric interferometry exploits the properties of atmospheric turbulence over fields smaller than the interferometer baseline divided by the atmospheric scale height. For such fields, accuracy is linear with star separation, and nearly inversely proportional to baseline length. To exploit these properties, the interferometer observes a relatively bright (less than 13 mag(sub K)) target in the near infrared at 2.2 micrometers, and uses phase referencing to find a reference star within the 2.2-micrometers isoplanatic patch. With this technique faint references can be found for most targets. With baselines greater than 100 m, which also minimize photon-noise errors, and with careful control of systematic errors by using laser metrology, accuracies of tens of microarcseconds/square root of (hour) should be possible.
    Keywords: ASTRONOMY
    Type: Astrophysics and Space Science (ISSN 0004-640X); 212; p. 385-390
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  • 6
    Publication Date: 2011-08-24
    Description: Narrow-angle astrometry has many astrophysical applications, from the measurement of parallaxes to the search for planets around nearby stars. Ground-based long-focus telescopes with photoelectric detectors have achieved accuracies of about 2-3 milliarcsec in 1 h. This accuracy is limited primarily by the atmosphere, and is consistent with models of atmospheric turbulence. However, applying these turbulence models to observations with long-baseline interferometers yields astrometric errors that are far smaller than can be achieved with long-focus telescopes. The predictions for the ultimate accuracy of ground-based narrow-angle astrometry using long-baseline IR (2.2 micron) stellar interferometers are very promising. With the excellent seeing at a high altitude site like Mauna Kea, the atmospheric limit for a 1 h astrometric measurement is expected to be of the order of 10 microarcsec for 1 h of integration. This two-order-of-magnitude improvement over conventional measurements is due to two effects. One is that a long-baseline IR interferometer can find useful reference stars very near an arbitrary target star, so that the atmospherically-induced motions of both stars are highly correlated. The second is that the baseline length can be much larger than the separation of the stellar beams in the turbulent atmosphere, resulting in a reduction in astrometric error with increasing baseline length.
    Keywords: ASTRONOMY
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 262; 1; p. 353-358.
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  • 7
    Publication Date: 2011-08-24
    Description: The long baselines of the next-generation ground-based optical stellar interferometers require optical delay lines which can maintain nm-level path-length accuracy while moving at high speeds. NASA-JPL is currently designing delay lines to meet these requirements. The design is an enhanced version of the Mark III delay line, with the following key features: hardened, large diameter wheels, rather than recirculating ball bearings, to reduce mechanical noise; a friction-drive cart which bears the cable-dragging forces, and drives the optics cart through a force connection only; a balanced PZT assembly to enable high-bandwidth path-length control; and a precision aligned flexural suspension for the optics assembly to minimize bearing noise feedthrough. The delay line is fully programmable in position and velocity, and the system is controlled with four cascaded software feedback loops. Preliminary performance is a jitter in any 5 ms window of less than 10 nm rms for delay rates of up to 28 mm/s; total jitter is less than 10 nm rms for delay rates up to 20 mm/s.
    Keywords: OPTICS
    Type: In: Active and adaptive optical systems; Proceedings of the Meeting, San Diego, CA, July 22-24, 1991 (A93-39451 15-74); p. 205-212.
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  • 8
    Publication Date: 2011-08-24
    Description: The long-period variable Mira Omicron Ceti has been observed at 800 nm wavelength with the Mk III Optical Interferometer at photometric phases 0 = 0.96, 0.05, and 0.14 in 1990; some additional data were taken in 1989. The star is not spherically symmetric, and temporal variations of the size and the position angle of the asymmetry are detected. The visibility data can be represented by two uniform elliptical disks, which could correspond to different layers in Mira's atmosphere. If the size variations are interpreted in terms of physical motion of the emitting material, an infall velocity of about 15 km/s around phi = 0 is derived.
    Keywords: ASTROPHYSICS
    Type: Astronomy and Astrophysics (ISSN 0004-6361); 259; 1; p. L19-L22.
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  • 9
    Publication Date: 2011-08-24
    Description: The orbiting stellar interferometer (OSI) is a concept for a first-generation space interferometer with astrometric and imaging goals. The OSI is a triple Michelson interferometer with articulating siderostats and optical delay lines. Two point designs for the instrument are described. The 18-m design uses an 18-m maximum baseline and aperture diameters of 40 cm; the targeted astrometric performance is a wide-field accuracy of 10 microarsec for 16-mag objects in 100 s of integration time and for 20-mag objects in 1 h. The instrument would also be capable of synthesis imaging with a resolution of 5 marcsec, which corresponds to the diffraction limit of the 18-m base line. The design uses a deployed structure, which would fold to fit into an Atlas IIAS shroud, for insertion into a 900-km sun-synchronous orbit. In addition to the 18-m point design, a 7-m point design that uses a shorter base line in order to simplify deployment is also discussed. OSI's high performance is made possible by utilizing laser metrology and controlled-optics technology.
    Keywords: SPACECRAFT INSTRUMENTATION
    Type: Applied Optics (ISSN 0003-6935); 32; 10; p. 1789-1797.
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  • 10
    Publication Date: 2011-08-24
    Description: The history and the current status of optical and infrared long-baseline interferometry are reviewed. In particular, attention is given to Michelson interferometry; the Mark III stellar interferometer and its applications to astrometry, measurement of stellar diameters, and observations of binary stars; and advanced techniques. The discussion then focuses on astrometry and imaging with space interferometers. Finally, the future of long-baseline interferometry is briefly discussed with particular reference to the interferometry of the moon.
    Keywords: ASTRONOMY
    Type: In: Annual review of astronomy and astrophysics. Vol. 30 (A93-25826 09-90); p. 457-498.
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