The Luminosity Function of Galaxies as Modeled by a Left Truncated Beta Distribution

Zaninetti, L.

doi:10.4236/ijaa.2014.41013

Cited by 4 publications

(4 citation statements)

References 29 publications

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“…This LF contains the five parameters α, β, M a , M b , Ψ * which can be derived from the operation of fitting the observational data and M which characterize the considered band, see [43]. The number of variables can be reduced to three once M a and M b are identified with the maximum and the minimum absolute magnitude of the considered sample.…”

Section: Evolutionary Effectsmentioning

confidence: 99%

On the Number of Galaxies at High Redshift

Zaninetti

2015

Galaxies

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The number of galaxies at a given flux as a function of the redshift, z, is derived when the z-distance relation is non-standard. In order to compare different models, the same formalism is also applied to the standard cosmology. The observed luminosity function for galaxies of the zCOSMOS catalog at different redshifts is modeled by a new luminosity function for galaxies, which is derived by the truncated beta probability density function. Three astronomical tests, which are the photometric maximum as a function of the redshift for a fixed flux, the mean value of the redshift for a fixed flux, and the luminosity function for galaxies as a function of the redshift, compare the theoretical values of the standard and non-standard model with the observed value. The tests are performed on the FORS Deep Field (FDF) catalog up to redshift z = 1.5 and on the zCOSMOS catalog extending beyond z = 4. These three tests show minimal differences between the standard and the non-standard models.

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Section: Evolutionary Effectsmentioning

confidence: 99%

On the Number of Galaxies at High Redshift

Zaninetti

2015

Galaxies

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“…The mass of the stars in the IMF, the luminosity of galaxy in the LF and the absolute magnitude of galaxy in a given range of redshift vary between a minimum and a maximum value. This discussion suggests the introduction of finite boundaries for the Lindley IMF and LF rather than the usual zero and infinity following a pattern similar to the introduction of a left truncated beta LF; see [27], and for a left and right truncated Schechter LF luminosity function, see [28].…”

Section: Introductionmentioning

confidence: 99%

The Truncated Lindley Distribution with Applications in Astrophysics

Zaninetti¹

2019

Galaxies

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This paper reviews the Lindley distribution and then introduces the scale and the double truncation. The unknown parameters of the truncated Lindley distribution are evaluated with the maximum likelihood estimators. An application of the Lindley distribution with scale is done to the initial mass function for stars. The magnitude version of the Lindley distribution with scale is applied to the luminosity function for the Sloan Digital Sky Survey (SDSS) galaxies and to the photometric maximum of the 2MASS Redshift Survey (2MRS) galaxies. The truncated Lindley luminosity function allows us to model the Malquist bias of the 2MRS galaxies.

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“…The above line of research allows exploring the LF for galaxies in the framework of well studied PDFs. Some examples are represented by the mass-luminosity relationship, see [9], some models connected with the generalized gamma (GG) distribution, see [10,11], the truncated beta LF, see [12], the lognormal LF, see [13], the truncated lognormal LF, see [14], and the Lindley LF, see [15]. This paper brings up the GG and introduces the scale in Section 2.…”

Section: Introductionmentioning

confidence: 99%

New Probability Distributions in Astrophysics: I. The Truncated Generalized Gamma

Zaninetti¹

2019

IJAA

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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.

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The Luminosity Function of Galaxies as Modeled by a Left Truncated Beta Distribution

Cited by 4 publications

References 29 publications

On the Number of Galaxies at High Redshift

On the Number of Galaxies at High Redshift

The Truncated Lindley Distribution with Applications in Astrophysics

New Probability Distributions in Astrophysics: I. The Truncated Generalized Gamma

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