aršâyeš-e tafsanji, ~ tafsanjik
Fr.: correction bolométrique
1) aršâ; 2) aršâyidan
Fr.: 1) correct; 2) corriger
1) Free from error; conforming to an acknowledged or accepted standard or fact;
true or accurate.
From L. correctus, p.p. of corrigere "make straight, put right," from → com- intens. prefix + regere "to guide, direct, rule," cf. Av. raz- "to direct, lead," razišta- "straightest, most correct," erezu- "correct, straight," râzayeiti "directs," O.Pers. râs- "to be right, straight, true," râsta- "staright, true," Mod.Pers. râst "right, straight, true," Skt. raj- "to direct, stretch," rjuyant- "walking straight," Gk. orektos "stretched out," Ger. recht, E. right; PIE base *reg- "right, just; to move in a straight line."
1) Aršâ, from Av. arš, ereš, erež "rightly, truly," as in arš.dâta- "rightly made," arš.manah-
"whose thinking is right," arš.vacah- "whose speaking is right,"
erešya- "righteous, just," cf. O.Pers. arta- "law, justice,"
Skt. rta- "cosmic order," Gk. arti "just," artios "complete;"
PIE base ar- "to fit together, join."
tiqe-ye aršâyandé, ~ aršâgar
Fr.: lame correctrice
A large glass plate placed at the entrance of a Schmidt telescope to correct for spherical aberration over the large field of view.
1) The act or process of correcting.
Noun form of → correct.
aršâyandé, ~ aršâgar
A thin lens-like optical piece which removes certain optical aberrations.
Fr.: correction d'extinction
In → photometric calibration, the correction for energy loss undergone by radiation due to the → atmospheric extinction. Extinction correction is done using → standard stars observed at different → airmasses.
ionization correction factor (ICF)
karvand-e aršâyeš-e yoneš
Fr.: facteur de correction d'ionisation
A quantity used in studies of → emission nebulae to convert the → ionic abundance of a given chemical element to its total → elemental abundance. The elemental abundance of an element relative to hydrogen is given by the sum of abundances of all its ions. In practice, not all the ionization stages are observed. One must therefore correct for unobserved stages using ICFs. A common way to do this was to rely on → ionization potential considerations. However, → photoionization models show that such simple relations do not necessarily hold. Hence, ICFs based on grids of photoionization models are more reliable. Nevertheless here also care should be taken for several reasons: the atomic physics is not well known yet, the ionization structure of a nebula depends on the spectral energy distribution of the stellar radiation field, which differs from one model to another, and the density structure of real nebulae is more complicated than that of idealized models (see, e.g., Stasińska, 2002, astro-ph/0207500, and references therein).
Fr.: correction K
A → color index correction applied to the photometric magnitudes and colors of a distant galaxy to compensate for the "reddening" of the galaxy due to → cosmological redshift. K correction is intended to derive the magnitudes in the → rest frame of the galaxy. Typically it is given as K(z) = az + bz2, where a and b depend on galaxy types. Conversely, one may deduce the redshift of a galaxy by its colors and a K-correction model.
The term K correction, probably stems from the K-term used by C. W. Wirtz (1918, Astron. Nachr. 206, 109), where K stands for Konstante, the German word for constant. The K-term was a constant offset in the redshift applied to diffuse nebulae in that epoch (source: A. L. Kinney, 1996, ApJ 467, 38); → correction.
Fr.: correction de Malmquist
A correction introduced into star counts distributed by apparent magnitude.
Fr.: correction de Rydberg
A term inserted into a formula for the energy of a single electron in the outermost shell of an atom to take into account the failure of the inner electron shells to screen the nuclear charge completely.
aršâyeš-e pišân-e mowj
Fr.: correction de front d'onde