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  2. Mass–luminosity relation - Wikipedia

    en.wikipedia.org/wiki/Massluminosity_relation

    The relationship is represented by the equation: = where L ⊙ and M ⊙ are the luminosity and mass of the Sun and 1 < a < 6. [2] The value a = 3.5 is commonly used for main-sequence stars. [ 3 ] This equation and the usual value of a = 3.5 only applies to main-sequence stars with masses 2 M ⊙ < M < 55 M ⊙ and does not apply to red giants ...

  3. Mass-to-light ratio - Wikipedia

    en.wikipedia.org/wiki/Mass-to-light_ratio

    The luminosity thus obtained is known as the bolometric luminosity. Masses are often calculated from the dynamics of the virialized system or from gravitational lensing . Typical mass-to-light ratios for galaxies range from 2 to 10 ϒ ☉ while on the largest scales, the mass to light ratio of the observable universe is approximately 100 ϒ ...

  4. Galaxy color–magnitude diagram - Wikipedia

    en.wikipedia.org/wiki/Galaxy_color–magnitude...

    A mock-up of the galaxy color–magnitude diagram with three populations: the red sequence, the blue cloud, and the green valley. The galaxy color–magnitude diagram shows the relationship between absolute magnitude (a measure of luminosity) and mass of galaxies.

  5. Fundamental plane (elliptical galaxies) - Wikipedia

    en.wikipedia.org/wiki/Fundamental_plane...

    The fundamental plane is a set of bivariate correlations connecting some of the properties of normal elliptical galaxies.Some correlations have been empirically shown. The fundamental plane is usually expressed as a relationship between the effective radius, average surface brightness and central velocity dispersion of normal elliptical galaxies.

  6. Tully–Fisher relation - Wikipedia

    en.wikipedia.org/wiki/Tully–Fisher_relation

    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. [ 8 ] 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.

  7. Initial mass function - Wikipedia

    en.wikipedia.org/wiki/Initial_mass_function

    Therefore, the stellar luminosity function is used to derive a mass function (a present-day mass function, PDMF) by applying massluminosity relation. [2] The luminosity function requires accurate determination of distances, and the most straightforward way is by measuring stellar parallax within 20 parsecs from the earth.

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  9. Faber–Jackson relation - Wikipedia

    en.wikipedia.org/wiki/Faber–Jackson_relation

    Velocity dispersion (y-axis) plotted against absolute magnitude (x-axis) for a sample of elliptical galaxies, with the Faber–Jackson relation shown in blue.. The Faber–Jackson relation provided the first empirical power-law relation between the luminosity and the central stellar velocity dispersion of elliptical galaxy, and was presented by the astronomers Sandra M. Faber and Robert Earl ...