1, 2, 3, 4) pâyé (#), 5) pâygâh (#), 6) bâz (#)
1) The bottom support of anything; a fundamental principle or groundwork.
M.E., from O.Fr. bas, from L. basis "foundation," from Gk. basis "step, pedestal," from bainein "to step."
Pâyé "base," from pâ, pây "foot," from Mid.Pers. pâd, pây;
Av. pad-, cf. Skt. pat: Gk. pos, genitive podos;
L. pes; PIE *pod-/*ped-.
Fr.: ligne de base
1) In radio interferometry, the separation between the electrical,
or phase centers of two interferometer elements.
pâygâh-e dâdehâ (#)
Fr.: base de données
A combined and coordinated set of data that supplies information for a specific purpose in a variety of forms.
The altitude at which the atmosphere becomes collisionless.
federated database system (FDBS)
râžmân-e pâygâh-e dâdehâ-ye hiyâvidé
Fr.: système de base de données fédéré
A composition of different databases which work in an integrated manner while preserving their autonomy.
fuzzy rule base
pâygâh-e razan-e porzvâr
nepâheš az zamin
Fr.: observation au sol
An astronomical observation carried out using a telescope on Earth, as opposed to that from an orbiting satellite.
Very Large Baseline Array (VLBA)
ârast bâ pâye-xatt-e besyâr bozorg
Fr.: Very Large Baseline Array (VLBA)
A network of ten 25-m radio telescopes for → very-long-baseline interferometry (VLBI), operated by the U.S. National Radio Astronomy Observatory. Eight of the VLBA telescopes are distributed across the continental United States, while the other two are in Hawaii and the Virgin Islands, giving a maximum baseline of about 8,000 km and a resolution better than a milliarcsecond at its shortest wavelength.
very-long-baseline interferometry (VLBI)
andarzanešsanji bâ pâye-xatt-e besyâr bozorg
Fr.: interférométrie à très longue base
A technique in radio interferometry in which the individual telescopes are not directly connected together, but instead make their observations separately with very accurate timings. The data are later sent to a central correlator to be combined. With this technique the individual telescopes can be arbitrarily far apart, and so the technique provides the highest resolution images in astronomy, typically down to a few milliarcseconds.