Rupert Croft

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We measure clustering in 1 dimension, along a sightline. How is this related to 3D clustering? (Kaiser and Peacock 1991) 3D power spectrum
First application, to a single quasar spectrum (RC et al, 1998) From the lyman alpha flux power spectrum to the matter power spectrum
Page 1 and 2: Rupert Croft QuickTime and a decomp
Page 3 and 4: Plan for lecture 2: • Recap : - T
Page 5 and 6: Gunn and Peterson (1965)
Page 7 and 8: We are interested in the transmitte
Page 10 and 11: First published high-z QSO spectrum
Page 12 and 13: What is the mean density of baryons
Page 14 and 15: QuickTime and a decompressor are ne
Page 16: • If we take a spectrum of a quas
Page 19 and 20: The width of the clouds in this ori
Page 21 and 22: Failed models QuickTime and a decom
Page 24 and 25: With the simulations we are effecti
Page 26 and 27: The baryons in a simulated universe
Page 28 and 29: absorption level in quasar spectra
Page 30 and 31: Baryons trace dark matter well on s
Page 32 and 33: For the gas in photoionization equi
Page 34 and 35: Additional physics which could disr
Page 36 and 37: How do we quantify structure in the
Page 38 and 39: Here is the galaxy power spectrum,
Page 42 and 43: SDSS quasar spectrum low quality sp
Page 44: flux power spectrum from 3400 SDSS
Page 47 and 48: From Max Tegmark’s webpage
Page 49 and 50: Massive neutrinos suppress the clus
Page 51 and 52: Constraints on neutrino mass from c
Page 53 and 54: Even better limits from Viel et al
Page 55 and 56: The Lya forest will also be used in
Page 57 and 58: Need a survey with a huge volume an
Page 59: Conclusions for part I • The lyma

Rupert Croft

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