A Left and Right Truncated Schechter Luminosity Function for Quasars

Zaninetti, L.

doi:10.3390/galaxies5020025

Cited by 8 publications

(7 citation statements)

References 34 publications

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“…, see [28] for more details. Figure 4 displays the observed LF for QSO as well the theoretical fit with the Weibull LF.…”

Section: The Lf For Galaxiesmentioning

confidence: 99%

New Probability Distributions in Astrophysics: V. The Truncated Weibull Distribution

Zaninetti¹

2021

IJAA

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We demonstrate that certain astrophysical distributions can be modelled with the truncated Weibull distribution, which can lead to some insights: in particular, we report the average value, the rth moment, the variance, the median, the mode, the generation of random numbers, and the evaluation of the two parameters with maximum likelihood estimators. The first application of the Weibull distribution is the initial mass function for stars. The magnitude version of the Weibull distribution 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 Weibull luminosity function allows us to model the average value of the absolute magnitude as a function of the redshift for the 2MRS galaxies.

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“…, see [28] for more details. Figure 4 displays the observed LF for QSO as well the theoretical fit with the Weibull LF.…”

Section: The Lf For Galaxiesmentioning

confidence: 99%

New Probability Distributions in Astrophysics: V. The Truncated Weibull Distribution

Zaninetti¹

2021

IJAA

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“…Theoretical parameters as in Table 1. Another case is the LF for QSO in the case 0.3 < z < 0.5, see [28] for more details. Figure 4 displays the observed LF for QSO as well the theoretical fit with the Weibull LF.…”

Section: The Lf For Galaxiesmentioning

confidence: 99%

New Probability Distributions in Astrophysics: III. The Truncated Maxwell-Boltzmann Distribution

Zaninetti

2020

IJAA

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The Maxwell-Boltzmann (MB) distribution for velocities in ideal gases is usually defined between zero and infinity. A double truncated MB distribution is here introduced and the probability density function, the distribution function, the average value, the rth moment about the origin, the root-mean-square speed and the variance are evaluated. Two applications are presented: 1) a numerical relationship between root-mean-square speed and temperature, and 2) a modification of the formula for the Jeans escape flux of molecules from an atmosphere.

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“…For our first example, we selected the catalog of the 2dF QSO Redshift Survey (2QZ), which contains 22431 redshifts of QSOs with 18.25 < b J < 20.85, see [25]. We processed them as explained in [26]. A typical example of the observed LF for QSOs when 0.3 < z < 0.5 as well the fit with the four parameters truncated GG LF is presented in Figure 6 with data as in Table 3.…”

Section: Luminosity Function For Qsosmentioning

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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A Left and Right Truncated Schechter Luminosity Function for Quasars

Cited by 8 publications

References 34 publications

New Probability Distributions in Astrophysics: V. The Truncated Weibull Distribution

New Probability Distributions in Astrophysics: V. The Truncated Weibull Distribution

New Probability Distributions in Astrophysics: III. The Truncated Maxwell-Boltzmann Distribution

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

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