[PDF] Top 20 A high resolution study of the high redshift intergalactic medium

... spectral resolution we have employed high-quality ESI and HIRES spectra of ...per resolution element except to introduce a spike in the autocorrelation at zero ...the resolution FWHM increases ... See full document

... Inspired by recent studies that suggest that galaxies grow primarily by acquiring gas through cold accretion, we studied the covering frac- tion of Lyα absorbing gas with different properties within 200 proper kpc from ... See full document

... the high redshift universe using a combination of observational data and numerical simulations/theoretical ...a redshift as high as z ∼ 12. An iconic high-redshift galaxy survey ... See full document

... of high-resolution hydrody- namical simulations, combined with accurate measurements of the mean transmitted flux in the Ly α forest (Becker et ...the high value of the power-law slope, ( γ − 1), at ... See full document

... the high-redshift IGM, using our model coeval stellar population, comprising main- sequence stars formed in a single burst followed by a later HMXB ... See full document

... A B S T R A C T We report ultra-high-resolution observations ðR < 9 10 5 Þ of Na I , Ca II , K I , CH and CH 1 for interstellar sightlines towards 12 bright stars in Orion. These data enable the detection ... See full document

... The pipeline-derived uncertainties on the PACS spectra are known to be unreliable. 25 Therefore, we weigh each wave- length bin equally for fi tting purposes. The uncertainty on the line fl uxes are determined from 1000 ... See full document

... In Figure 8 (fig 8.1–8.13) we show the individual spectral observations for each lensed SMG observed in OT2 jwardlow 1. Figure 8. 1 Observed spectra (black) at native PACS resolution, and the best-fit continuum or ... See full document

... very high resolution ðR ¼ 400 000 and R ¼ 880 000Þ observations of interstellar Ca II absorption lines towards eight early-type stars situated within 158 of a Oph on the ...these high- ... See full document

... Assuming that the effective thermal conductivity can be expressed as a multiple, f c , of the Spitzer value, this parameter provides a mea- sure of the stability of the gas to local cooling. For large values of η min , ... See full document

... Assuming that the effective thermal conductivity can be expressed as a multiple, f c , of the Spitzer value, this parameter provides a mea- sure of the stability of the gas to local cooling. For large values of η min , ... See full document

... Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as ... See full document

... unique study of relatively faint and small galaxies at high ...other high-redshift IFU ...have high velocity dispersion σ = 50–100 km s −1 , consistent with all other resolved ... See full document

... to study the environment of high-z quasars and radio galaxies through submillimetre and CO spectral line observations and to contribute to the effort of uncovering the underlying processes that shape the ... See full document

... Spergel 2012). Here, we adopt a complementary approach that reduces the sen- sitivity of the flux PDF to the continuum fitting. Assuming that the continuum uncertainty is well approximated by a multiplicative parameter, ... See full document

... In their work in fact, Faucher-Gigu`ere et al. evaluated the relative percentages of metal absorption in their measurements of τ eff when applying two different corrections: the one obtained with the direct ... See full document

... To ensure that the traditional value of 1176 ˚ A is sufficiently stringent as to remove all proximity zone influence, we first plot a stacked spectrum of our entire catalog in the range 1100 < λ < 1215 ˚ A (Fig V.5). The ... See full document

... While quasar feedback is a well accepted idea, there are still questions about how big of a role this plays in the evolution of the quasar and of the host galaxy, particularly in the early universe. To address this ... See full document

... the redshift evolution parameter k z , it is possible to calculate the expected number of objects from the LF up to a given magnitude in a given area of the ...a redshift and a template spectrum are ... See full document

... 1) and E < 18.6 (the POSS blue limit is O ≈ 21.7). Trial Figure 2. Distribution in colour and magnitude of starlike (POSSI/APM) optical identifications of FIRST radio sources. Objects with no O magnitude have been ... See full document