We have designed and built three cost effective observatories, in distinct models, which can house Schmidt -Cassegrain type small telescopes having aperture sizes up to 16 inches. Using the available small telescopes, we provided the people of Manipura State in the far north-east corner of India the opportunity to observe directly with their own eyes the rare, spectacular events of the solar eclipse of
In this paper we present a determination of the optical luminosity function of Quasi Stellar Objects (QSOs) and its evolution, using data from the 2 Degree Field (2dF) QSO Redshift Survey (2QZ) and the associated 6 Degree Field (6dF) QSO Redshift Survey (6QZ) over the redshift range 0.3 ≤ z ≤ 2.4 in a flat universe with Ωm = 0.3 and ΩΛ = 0.7. The shape of the luminosity function is best fitted by a Schechter function model of the form, where L * b J is the break or characteristic luminosity. Using the Levenberg-Marquardt method of nonlinear least square fit we find the luminosity evolution model of the form L * b J (z) ∝ 10 1.56z−0.34z 2 .
A study of the optical luminosity function of Quasi Stellar Objects (QSOs) and its evolution with redshift is carried out using the data from the Sloan Digital Sky Survey Data Release Seven (SDSS DR7). It is shown that the observed QSO luminosity function is well fitted by a Schechter function model of the form α , where i L * is the break or characteristic luminosity with luminosity evolution characterized by a second order polynomial in red shift. The best fit parameters are determined by using the Levenberg-Marquardt method of nonlinear least square fit.
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 ≤ ≤ 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 m =0.3 and Ω Λ =0.7, we determine the best-fitting optical luminosity function model parameters.
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