The flux power spectra of the Lyman alpha forest from a sample of 27 quasi-stellar objects (QSOs) taken with the high-resolution Ultraviolet Echelle Spectrograph (UVES) on the Very Large Telescope (VLT) are presented. We find a similar fluctuation amplitude at the peak of the '3D' flux power spectrum at ksimilar to0.03 s km(-1) as the study by Croft et al. (2002), in the same redshift range. The amplitude of the flux power spectrum increases with decreasing redshift if corrected for the increase in the mean flux level as expected if the evolution of the flux power spectrum is sensitive to the gravitational growth of matter density fluctuations. This is in agreement with the findings of McDonald et al. (2000) at larger redshift. The logarithmic slope of the '3D' flux power spectrum, P-F(k), at large scales k<0.03 s km(-1), is 1.4&PLUSMN;0.3, i.e. 0.3 shallower than that found by Croft et al. but consistent within the errors.

The power spectrum of the flux distribution in the Lyman α forest of a large sample of UVES QSO absorption spectra (LUQAS) / Kim, T. S.; Viel, Matteo; Haehnelt, M. .; Carswell, R. F.; Cristiani, S.. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 347:2(2004), pp. 355-366. [10.1111/j.1365-2966.2004.07221.x]

The power spectrum of the flux distribution in the Lyman α forest of a large sample of UVES QSO absorption spectra (LUQAS)

Viel, Matteo;
2004-01-01

Abstract

The flux power spectra of the Lyman alpha forest from a sample of 27 quasi-stellar objects (QSOs) taken with the high-resolution Ultraviolet Echelle Spectrograph (UVES) on the Very Large Telescope (VLT) are presented. We find a similar fluctuation amplitude at the peak of the '3D' flux power spectrum at ksimilar to0.03 s km(-1) as the study by Croft et al. (2002), in the same redshift range. The amplitude of the flux power spectrum increases with decreasing redshift if corrected for the increase in the mean flux level as expected if the evolution of the flux power spectrum is sensitive to the gravitational growth of matter density fluctuations. This is in agreement with the findings of McDonald et al. (2000) at larger redshift. The logarithmic slope of the '3D' flux power spectrum, P-F(k), at large scales k<0.03 s km(-1), is 1.4&PLUSMN;0.3, i.e. 0.3 shallower than that found by Croft et al. but consistent within the errors.
2004
347
2
355
366
10.1111/j.1365-2966.2004.07221.x
https://arxiv.org/abs/astro-ph/0308103
Kim, T. S.; Viel, Matteo; Haehnelt, M. .; Carswell, R. F.; Cristiani, S.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/14084
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