We present a novel, fast method to recover the density field through the statistics of the transmitted flux in high-redshift quasar absorption spectra. The proposed technique requires the computation of the probability distribution function of the transmitted flux (PF) in the Lyα forest region and, as a sole assumption, the knowledge of the probability distribution function of the matter density field (PΔ). We show that the probability density conservation of the flux and matter density unveils a flux-density (F-Δ) relation which can be used to invert the Lyα forest without any assumption on the physical properties of the intergalactic medium. We test our inversion method at z = 3 through the following steps: (i) simulation of a sample of synthetic spectra for which PΔ is known; (ii) computation of PF; and (iii) inversion of the Lyα forest through the F-Δ relation. Our technique, when applied to only 10 observed spectra characterized by a signal-to-noise ratio ≥ 100, provides an exquisite (relative error ɛΔ≲ 12 per cent in ≳50 per cent of the pixels) reconstruction of the density field in ≳90 per cent of the line of sight. We finally discuss strengths and limitations of the method.

We present a novel, fast method to recover the density field through the statistics of the transmitted flux in high-redshift quasar absorption spectra. The proposed technique requires the computation of the probability distribution function of the transmitted flux (PF) in the Lyα forest region and, as a sole assumption, the knowledge of the probability distribution function of the matter density field (PΔ). We show that the probability density conservation of the flux and matter density unveils a flux-density (F-Δ) relation which can be used to invert the Lyα forest without any assumption on the physical properties of the intergalactic medium. We test our inversion method at z = 3 through the following steps: (i) simulation of a sample of synthetic spectra for which PΔ is known; (ii) computation of PF; and (iii) inversion of the Lyα forest through the F-Δ relation. Our technique, when applied to only 10 observed spectra characterized by a signal-to-noise ratio ≥ 100, provides an exquisite (relative error ɛΔ≲ 12 per cent in ≳50 per cent of the pixels) reconstruction of the density field in ≳90 per cent of the line of sight. We finally discuss strengths and limitations of the method.

Cosmic density field reconstruction from Lya forest data

Gallerani, S.;FERRARA, ANDREA
2011

Abstract

We present a novel, fast method to recover the density field through the statistics of the transmitted flux in high-redshift quasar absorption spectra. The proposed technique requires the computation of the probability distribution function of the transmitted flux (PF) in the Lyα forest region and, as a sole assumption, the knowledge of the probability distribution function of the matter density field (PΔ). We show that the probability density conservation of the flux and matter density unveils a flux-density (F-Δ) relation which can be used to invert the Lyα forest without any assumption on the physical properties of the intergalactic medium. We test our inversion method at z = 3 through the following steps: (i) simulation of a sample of synthetic spectra for which PΔ is known; (ii) computation of PF; and (iii) inversion of the Lyα forest through the F-Δ relation. Our technique, when applied to only 10 observed spectra characterized by a signal-to-noise ratio ≥ 100, provides an exquisite (relative error ɛΔ≲ 12 per cent in ≳50 per cent of the pixels) reconstruction of the density field in ≳90 per cent of the line of sight. We finally discuss strengths and limitations of the method.
Cosmic density field reconstruction from Ly alpha forest data
2011
astro-ph.CO; astro-ph.CO; Statistics - Applications
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11384/565
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