2003/08/31 by T.- S. Kim, T. -S. Kim, Matteo Viel +5
Physics and Astronomy · #Amplitude #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Lyman-alpha forest #Optics #Physics #QSOS #Redshift #Spectral density #Spectral line #Spectrograph #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2004.07221.x
published as Mon.Not.Roy.Astron.Soc.347:355,2004 · 18 pages, 9 PS figures, 6 tables. Note that the k-values of the 1D flux power spectrum had been erroneously shifted by half a bin size (in log k) in the previous version. All the other results are unaffected. New tables can be found at http://www.ast.cam.ac.uk/~rtnigm/luqas.htm
openalex publication_date 2003/12/21 · arxiv created 2004/05/11 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The flux power spectra of the Lyman α 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 k∼ 0.03 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, PF(k), at large scales k < 0.03 s km−1, is 1.4 ± 0.3, i.e. 0.3 shallower than that found by Croft et al. but consistent within the errors.