Abstract
We study the shape of the optical luminosity function of Quasi Stellar Objects (QSOs) from the Sloan Digital Sky Survey Data Release Seven (SDSS DR7) over the redshift range 0.3 ≤ Z ≤ 2.4. By using the Levenberg-Marquardt method of nonlinear least square fit, the observed QSO luminosity function is fitted by a double power-law model with luminosity evolution characterized by a second order polynomial in redshift. For a flat universe with Ω<sub>m</sub>=0.3 and Ω <sub>Λ</sub>=0.7, we determine the best-fitting optical luminosity function model parameters.
Highlights
Quasi Stellar Objects (QSOs) or quasars are intrinsically luminous subclass of Active Galactic Nuclei (AGNs) and these objects represent a fascinating and unique population of objects at the intersection of cosmology and astrophysics [1]
The QSO luminosity function is calculated at absolute magnitude intervals of 0.3 mag in nine separate redshift bins over the redshift range 0.3 z 2.4
The luminosity function of the QSOs in the Sloan Digital Sky Survey (SDSS) DR7 and its evolution with redshift are studied by using the double power-law model with pure luminosity evolution (PLE)
Summary
Quasi Stellar Objects (QSOs) or quasars are intrinsically luminous subclass of Active Galactic Nuclei (AGNs) and these objects represent a fascinating and unique population of objects at the intersection of cosmology and astrophysics [1]. Soon after the discovery of QSOs their population was observed to be evolving [2] As a result these objects provide a unique tool in the study of galaxies and large-scale structure formation throughout the history of the universe [3]. Due to strong evolution of QSOs with cosmic time the luminosity function of the QSOs must be of particular importance in the understanding of formation and evolution of the QSOs. The QSO luminosity function and its evolution with redshift are the most important tools to constrain the accretion history of supermassive black holes (SMBHs) [6] and provide important clues about the demographics of the AGN population and constraints on physical models and evolutionary theories of AGN [7,8,9].
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