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In astronomy, the Tully–Fisher relation (TFR) is an empirical relationship between the mass or intrinsic luminosity of a spiral galaxy and its asymptotic rotation velocity or emission line width. It was first published in 1977 by astronomers R. Brent Tully and J. Richard Fisher.[1] The luminosity is calculated by multiplying the galaxy's apparent brightness by ${\displaystyle 4\pi d^{2}}$, where ${\displaystyle d}$ is its distance from us, and the spectral-line width is measured using long-slit spectroscopy.

Several different forms of the TFR exist, depending on which precise measures of mass, luminosity or rotation velocity one takes it to relate. Tully and Fisher used optical luminosity, but subsequent work showed the relation to be tighter when defined using microwave to infrared (K band) radiation (a good proxy for stellar mass), and even tighter when luminosity is replaced by the galaxy's total baryonic mass (the sum of its mass in stars and gas).[2] This latter form of the relation is known as the baryonic Tully–Fisher relation (BTFR), and states that baryonic mass is proportional to velocity to the power of roughly 3.5–4.[3]

The TFR can be used to estimate the distance to spiral galaxies by allowing the luminosity of a galaxy to be derived from its directly measurable line width. The distance can then be found by comparing the luminosity to the apparent brightness. Thus the TFR constitutes a rung of the cosmic distance ladder, where it is calibrated using more direct distance measurement techniques and used in turn to calibrate methods extending to larger distance.

In the dark matter paradigm, a galaxy's rotation velocity (and hence line width) is primarily determined by the mass of the dark matter halo in which it lives, making the TFR a manifestation of the connection between visible and dark matter mass. In Modified Newtonian dynamics (MOND), the BTFR (with power-law index exactly 4) is a direct consequence of the gravitational force law effective at low acceleration.[4]

The analogues of the TFR for non-rotationally-supported galaxies, such as ellipticals, are known as the Faber–Jackson relation and the fundamental plane.

See also

References

External links

• Scholarpedia article on the subject written by R. Brent Tully

На других языках

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[de] Tully-Fisher-Beziehung

Die Tully-Fisher-Beziehung (veröffentlicht 1977 von Richard Brent Tully und Richard Fisher) beschreibt einen Zusammenhang zwischen der Rotationsgeschwindigkeit von Spiralgalaxien und ihrer Leuchtkraft. Man kann aus der Verschiebung ihrer Spektrallinien und der daraus folgenden Rotationsgeschwindigkeit auf ihre Leuchtkraft und damit bei bekannter Helligkeit auf ihre Entfernung schließen.

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- [en] Tully–Fisher relation

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[es] Relación Tully-Fisher

La relación de Tully-Fisher es considerada una candela estándar en Astronomía. Fue publicada por los astrónomos R. Brent Tully y J. Richard Fisher en 1977 y permite estimar la distancia a la que se encuentra una galaxia espiral a partir de la anchura de las líneas de su espectro.

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[ru] Зависимость Талли — Фишера

Зависимость Талли — Фишера (англ. Tully–Fisher relation) — это эмпирически полученное соотношение, связывающее массу или собственную светимость спиральной галактики и скорость её вращения или ширину линий излучения в её спектре. Впервые была опубликована в 1977 году Ричардом Талли и Джеймсом Фишером[1]. Светимость галактики определяется по данным о видимой звёздной величине и расстоянии до галактики, ширина спектральных линий измеряется методами спектроскопии с длинной щелью.

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