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• W43287620 abstract "The effect of the absorption in the intergalactic medium due to neutral hydrogen randomly distributed along the line-of-sight -- in the form of Lyman-$alpha$ absorbers -- on the photometric properties of high-redshift galaxies is analysed. In particular, the differences in the observed colors of galaxies with otherwise identical Spectral Energy Distributions, arising from the difference in the distribution and physical properties -- density, temperature, redshift -- of the neutral hydrogen along different lines-of-sight is investigated. As a very first step, a new method to synthesize absorption line-profiles -- assuming that these are mathematically given by the Voigt-Hjerting function -- is developed. This new method is compared to existing methods and within this context it is found to be computationally faster than more accurate methods, and more accurate in the parameter range of interest than faster methods. Using this method, a model that accounts for the intergalactic absorption and its scatter due to the difference in the populations of Lyman-$alpha$ absorbers along different random lines-of-sight is presented. This model makes use of a set of input differential distribution functions for the physical properties of the Lyman-$alpha$ absorbers, i.e. their number density, column density, and Doppler parameter distribution, as obtained from observations and reported in the literature. Following the Monte Carlo approach, absorption masks which account for the intergalactic absorption along single lines-of-sight are constructed. Within this approach, the number and properties of each absorber for each absorption mask are drawn from the corresponding input distributions, and their absorption line-profiles are computed using the method previously introduced. Different sets of input distribution functions are tested by comparing the model predictions against measurements of the cosmic flux decrement, an independent observable that directly relates to the amount of neutral hydrogen along a given line-of-sight. This comparison is done using measurements found in the literature together with our own measurements performed on a sample of quasars obtained from the SDSS data archive. A particular set of input distribution functions is found which satisfactorily reproduces the evolution of the cosmic flux decrement over a large redshift range. Using this set as input for our model, the magnitude changes -- or intergalactic $k$-correction -- as a function of redshift is computed for different input galaxy spectra and in different wavelength ranges. Furthermore, the effect of the stochastic intergalactic absorption on the estimates of photometric redshifts using Spectral Energy Distributions is explored." @default.
• W43287620 created "2016-06-24" @default.
• W43287620 creator A5005812567 @default.
• W43287620 date "2022-02-20" @default.
• W43287620 modified "2023-09-24" @default.
• W43287620 title "The Stochastic Intergalactic Attenution and its Impact on High-Redshift Galaxies" @default.
• W43287620 doi "https://doi.org/10.53846/goediss-2798" @default.
• W43287620 hasPublicationYear "2022" @default.
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