New probability distributions in astrophysics: I. The truncated generalized gamma
arXiv:1912.12053 · doi:10.4236/ijaa.2019.94027
Abstract
The gamma function is a good approximation to the luminosity function of astrophysical objects, and a truncated gamma distribution would permit a more rigorous analysis. This paper examines the generalized gamma distribution (GG) and then introduces the scale and the new double truncation. The magnitude version of the truncated GG distribution with scale is adopted in order to fit the luminosity function (LF) for galaxies or quasars. The new truncated GG LF is applied to the five bands of SDSS galaxies, to the 2dF QSO Redshift Survey in the range of redshifts between 0.3 and 0.5, and to the COSMOS QSOs in the range of redshifts between 3.7 and 4.7. The average absolute magnitude versus redshifts for SDSS galaxies and QSOs of 2dF was modeled adopting a redshift dependence for the lower and upper absolute magnitude of the new truncated GG LF.
arXiv commentFigures 9 , pages 15
References in corpus (14)
- The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III
- The Sloan Digital Sky Survey Photometric Camera
- The Galaxy Luminosity Function and Luminosity Density at Redshift z=0.1
- The 2dF QSO Redshift Survey - XII. The spectroscopic catalogue and luminosity function
- How many cosmological parameters?
- The properties and luminosity function of extremely low luminosity galaxies
- Probing the faint end of the quasar luminosity function at z ~ 4 in the COSMOS field
- Is the luminosity distribution of field galaxies really flat ?
- The truncated Lindley distribution with applications in astrophysics
- A left and right truncated Schechter luminosity function for quasars
- The truncated lognormal distribution as a luminosity function for SWIFT-BAT gamma-ray bursts
- The Luminosity Function of Galaxies as modeled by a left truncated beta distribution
- A new luminosity function for galaxies as given by the mass-luminosity relationship
- A lognormal luminosity function for SWIRE in flat cosmology