Results 321 to 330 of about 10,502,106 (355)

Performance of short and long bent crystals for the TWOCRYST experiment at the Large Hadron Collider. [PDF]

Eur Phys J C Part Fields
Bandiera L, Cai R, Carsi S, Cesare S, Dewhurst KA, D'Andrea M, Salvador D, Gandini P, Guidi V, Hermes P, Lezzani G, Malagutti L, Marangotto D, Maccani C, Mazzolari A, Merli A, Mirarchi D, Monti-Guarnieri P, Montanari CE, Negrello R, Neri N, Prest M, Redaelli S, Romagnoni M, Selmi A, Tonani G, Vallazza E, Veres D, Zangari F, Zielińska M.   +29 more
europepmc   +1 more source

A large, long-lived, slowly-expanding superbubble across the Perseus arm. [PDF]

Nat Commun
Chen B, Li G, Yuan H, Xiang M, Zhou J, Chen P, Krause M, Coombs A.   +7 more
europepmc   +1 more source

Theory and Early Results from the Large Binocular Telescope Interferometer

, 2014
Denis Defrère
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The ESO Extremely Large Telescope instrumentation programme

Micro + Nano Materials, Devices, and Applications, 2020
The ESO Extremely Large Telescope (ELT) has been in construction since 2014. In parallel with the construction of the telescope, ESO has entered into agreements with consortia in the ESO member states to build the first instruments for that telescope. To
S. Ramsay, P. Amico, N. Bezawada, M. Cirasuolo, F. Dérie, S. Egner, E. George, F. Gonté, Juan Carlos González Herrera, P. Hammersley, C. Haupt, J. Heijmans, D. Ives, G. Jakob, F. Kerber, B. Koehler, V. Mainieri, A. Manescau, S. Oberti, P. Padovani, C. Péroux, R. Siebenmorgen, R. Tamai, J. Vernet   +23 more
semanticscholar   +1 more source

The final design for the Extremely Large Telescope prefocal stations

Astronomical Telescopes + Instrumentation, 2020
Located at the Nasmyth Platforms A and B, the Prefocal Stations of the Extremely Large Telescope (ELT) are the last opto-mechanical components before the light from the giant telescope comes to a focus. The mission of the Prefocal Stations are threefold.
Asier Larringan, Amaya Mugica, G. Murga, P. Jolley, S. Lewis   +4 more
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Large Space Telescope

IBM Journal of Research and Development, 1976
The Large Space Telescope, which is scheduled to be put into orbit above the Earth's atmosphere by NASA in the early 1980s, is a large, multipurpose optical instrument that is being designed to provide an increase in observational capability of nearly 100× with respect to brightness, 10× in resolving power, and a substantial bandwidth improvement over ...
Don Fuqua, Larry Winn
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Extremely Large Telescope Prefocal Station A system concept

Astronomical Telescopes + Instrumentation, 2018
The Prefocal Station (PFS) is the last opto-mechanical unit before the telescope focal plane in the Extremely Large Telescope (ELT) optical train. The PFS distributes the telescope optical beam to the Nasmyth and Coudé instrument focal stations and it ...
S. Lewis, E. Brunetto, A. Förster, C. Frank, I. Guidolin, S. Guisard, P. Hammersley, R. Holzlöhner, P. Jolley, J. Kosmalski, U. Lampater, E. Marchetti, P. La Penna, T. Pfrommer, P. Zuluaga   +14 more
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Cosmology and large telescopes

Astrophysics and Space Science, 1989
Assuming a large collecting area, a good angular resolution and a large field of view expected for the Japanese National Large Telescope (JNLT), we demonstrate that JNLT will provide a useful means of studying cosmological objects of interest. Among them I discuss how cosmological parameters and evolutionary effects can be obtained from redshift ...
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The Large Binocular Telescope

Applied Optics, 2010
The Large Binocular Telescope (LBT) Observatory is a collaboration among institutions in Arizona, Germany, Italy, Indiana, Minnesota, Ohio, and Virginia. The telescope on Mount Graham in Southeastern Arizona uses two 8.4 m diameter primary mirrors mounted side by side. A unique feature of the LBT is that the light from the two Gregorian telescope sides
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Adaptive optics for large telescopes

Astrophysics and Space Science, 1989
The performance of large telescopes is determined both by their angular resolution and by their collection area. It is, therefore, important to achieve as high an angular resolution as possible by site selection, by avoiding image deterioration by the telescope and its environment, and by real time image restoration by adaptive optics. We summarize the
Jacques M. Beckers, Fritz Merkle
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