Abstract:In this paper, we consider a statistical method for distance determination of stellar groups. The method depends on the assumption that the members of the group scatter around a mean absolute magnitude in Gaussian distribution. The mean apparent magnitude of the members is then expressed by frequency function, so as to correct for observational incompleteness at the faint end. The problem reduces to the solution of a highly transcendental equation for a given magnitude parameter α. For the computational develo… Show more
“…Rightly so -one should expect noisy data from signals more than half the Universe age. Precise distance determination is a problem which has plagued astronomers from time immemorial (Sharaf & Sendi, 2010). These very large errors mean the data from ancient SNe Ia play a much smaller role in determining the fit parameters Table 1.…”
“…Rightly so -one should expect noisy data from signals more than half the Universe age. Precise distance determination is a problem which has plagued astronomers from time immemorial (Sharaf & Sendi, 2010). These very large errors mean the data from ancient SNe Ia play a much smaller role in determining the fit parameters Table 1.…”
“…Rightly so -one should expect noisy data from signals more than half the Universe age. Precise distance determination is a problem which has plagued astronomers from time immemorial (Sharaf & Sendi, 2010). These very large errors mean the data from ancient SNe Ia play a much smaller role in determining the fit parameters (Hicken et al, 2009) after culling 11 outliers(387) and FP the number of free parameters.…”
Professor Antonio Alfonso-Faus holds a Diploma in Space Science (Physics and Dynamics) from the University College, London (U.K. 1965), a M.Sci. and a Ph.D. degree in Physics and Mathematics from the University of Minnesota (U.S.A., 1968), and a Ph.D. degree in Aeronautical Engineering from the Technical University
“…Moreover, empirical astrophysics researches have seen a paradigm shift in recent years in that it routinely involves data mining of large multi wavelength data sets, requiring complex automated processes that must invoke a very diverse set of statistical techniques (e.g. [2] [3]). …”
In this paper, a reliable computational tool will be developed for the determination of the parameters of the stellar density function in a region of the sky with complete error controlled estimates. Of these error estimates are, the variance of the fit, the variance of the least squares solutions vector, the average square distance between the exact and the least-squares solutions, finally the variance of the density stellar function due to the variance of the least squares solutions vector. Moreover, all these estimates are given in closed analytical forms.
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