An Etymological Dictionary of Astronomy and Astrophysics
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فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 76 Search : function
nested function
  کریای ِ تو-در-تو   
karyâ-ye tu-dar-tu

Fr.: fonction imbriquée   

In computer programing, a function that is defined inside the definition of another function.

nested; → function.

non-algebraic function
  کریای ِ ناجبری   
karyâ-ye nâjabri

Fr.: fonction non algébrique   

A → transcendental function. Examples are: exponential, logarithmic, and trigonometric functions.

non-; → algebraic + → function.

optical transfer function (OTF)
  کریا‌یِ تراوژ ِ نوری   
karyâ-ye tarâvaž-e nuri

Fr.: fonction de transfert optique   

The function that provides a full description of the imaging quality of an optical system. A combination of the → modulation transfer function (MTF) and the → phase transfer function (PTF) , the OTF describes the spatial (angular) variation as a function of spatial (angular) frequency.

optical; → transfer; → function.

orthogonal functions
  کریاهایِ ارداکنج   
karyâhâ-ye ardâkonj

Fr.: fonctions orthogonales   

A set of functions, any two of which, by analogy to orthogonal vectors, vanish if their product is summed by integration over a specified interval.

orthogonal; → function.

partition function
  کرپای ِ پرکش   
karâ-ye parkeš

Fr.: fonction de partition   

See → integer partition.

partition; → function.

periodic function
  کریای ِ دوره‌ای   
karyâ-ye dowreyi

Fr.: fonction périodique   

A function f(x) if for all x, f(x + P) = f(x), where P is a positive constant. The least value of P > 0 is called the period of f(x).

periodic; → function.

phase function
  کریای ِ فاز   
karyâ-ye fâz

Fr.: fonction de phase   

The variation in brightness of a target as the phase angle (the angle between Sun and observer as seen from the target) varies between 0° and 180°. The directional distribution of reflected (or scattered) radiation. The phase angle is the supplement of the scattering angle (the angle between the incident ray and the emerging ray); in other words, the sum of the phase angle and the scattering angle is always 180° (Ellis et al., 2007, Planetary Ring Systems, Springer).

phase; → function.

phase transfer function (PTF)
  کریای ِ تراوژ ِ فاز   
karyâ-ye tarâvaž-e fâz

Fr.: fonction de transfert de phase   

A measure of the relative phase in the image as function of frequency. It is the phase component of the → optical transfer function. A relative phase change of 180°, for example, results in an image with the black and white areas reversed.

phase; → transfer; → function.

piecewise continuous function
  کریای ِ پیوسته‌ی ِ تکه‌ای   
karyâ-ye peyvaste-ye tekke-yi

Fr.: fonction continue par morceaux   

A function f(x) in an interval if :1) the interval can be divided into a finite number of pieces in each of which f(x) is continuous, and 2) the limits of f(x) as x approaches the boundary point of each piece are finite. In other words, a piecewise continuous function is one that is made up of a finite number of continuous pieces.

piecewise; → continuous; → function.

Planck function
  کریای ِ پلانک   
karyâ-ye Planck

Fr.: fonction de Planck   

Same as → Planck's blackbody formula.

Planck; → function.

point spread function (PSF)
  کریای ِ گسترش ِ نقطه، ~ ~ پنده   
karyâ-ye gostareš-e noqté, ~ ~ pandé

Fr.: fonction d'étalement du point   

The two-dimensional intensity distribution about the image of a point source.

point; → spread; → function.

power function
  کریای ِ توانی   
karyâ-ye tavâni

Fr.: fonction de puissance   

A function of the form f(x) = xn, where n is a → real number.

power; → function.

present-day mass function (PDMF)
  کریای ِ جرم ِ کنونی، ~ ~ امروزی   
karyâ-ye jerm-e konuni, ~ ~ emruzi

Fr.: fonction de masse actuelle   

The present number of stars on the → main sequence per unit logarithmic mass interval per square parsec. The PDMF is the basis for deriving the → initial mass function (IMF). This mass function is not corrected for stellar evolution nor losses through stellar deaths.

present; → day; → mass; → function.

probability density function
  کریای ِ چگالی ِ شوانایی   
karyâ-ye cagâli-ye šavânâyi

Fr.: fonction de densité de probabilité   

A mathematical function whose integral over any interval gives the probability that a continuous → random variable has values in this interval. Also known as → density function, frequency function, → probability function.

probability; → density; → function.

probability function
  کریای ِ شوانایی   
karyâ-ye šavânâyi

Fr.: fonction de probabilité   

A function that represents a probability distribution in terms of integrals. Also called probability density function or density function.

probability; → function.

reddening function
  کریای ِ سرخش   
karyâ-ye sorxeš

Fr.: fonction de rougissement   

The normalized interstellar extinction at a given wavelength. It is defined by f(λ) = A(λ)/A(Hβ) - 1, where A(λ) is the extinction at the given wavelength and A(Hβ) the extinction at Hβ, with f(Hβ) = 0. It is used to → de-redden observed fluxes: I(λ)/I(Hβ) = F(λ)/F(Hβ).10c(Hβ).f(λ), where I represents the flux in the absence of extinction and F the observed flux affected by extinction, c(Hβ) being the → reddening coefficient.

reddening; → function.

regression function
  کریای ِ وایازش   
karyâ-ye vâyâzeš

Fr.: fonction de régression   

A mathematical function that describes the relationship between two or more variables in a set of data.

regression, → function.

regular function
  کریای ِ باسامان   
karyâ-ye bâsâmân

Fr.: fonction régulière   

A function of a complex variable which is single-valued in a domain and which has a finite derivative at every point.

regular; → function.

Salpeter function
  کریای ِ سلپیتر   
karyâ-ye Salpeter

Fr.: équation de Salpeter   

The first mathematical description of the → initial mass function (IMF) of newly formed stars of solar to → intermediate-masses. It is proportional to M -2.35, where M is the stellar mass. → Salpeter slope.

Named after the Austrian-Australian-American astrophysicist Edwin Ernest Salpeter (1924-2008); → function.

Schechter function
  کریای ِ ششتر   
karyâ-ye Schechter

Fr.: fonction de Schechter   

A mathematical expression that describes the → luminosity function of galaxies. The function correctly reflects the facts that the luminosity function decreases with increasing luminosity and that the decrease is particularly marked at high luminosities. It is expressed as: φ(L) = φ*(L/L*)α exp (-L/L*), which has two parts and three parameters: φ* is an empirically determined amplitude, α is an empirically derived exponent, and L* is a characteristic luminosity which separates the low and high luminosity parts. For small luminosities (L much smaller than L*) the Schechter function approaches a power law, while at high luminosities (L much larger than L*) the frequency of galaxies drops exponentially. φ*, L*, and the faint-end slope α depend on the observed wavelength range, on the → redshift, and on the environment where the galaxies are observed.

Named after the American astronomer Paul Schechter (1948-), who proposed the function in 1976 (ApJ 203, 297); → function.

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