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• W3100721648 abstract "We present the first large sample of metal absorption systems in pairs of QSOs with sightlines separated by about 1 Mpc at z = 2. We found 691 absorption systems in the spectra of 310 QSOs in 170 pairings. Most of the systems contain C IV or MgII absorption. We see 17 cases of absorption in one line-of-sight within 200 km s 1 (1 Mpc) of absorption in the paired line-of-sight. When we see absorption in one line-of-sight, the probability of also seeing absorption within about 500 km s 1 in the partner line-ofsight is at least � 50% at < 100 kpc, declining rapidly to 23% at 100 – 200 kpc and 0.7% by 1 – 2 Mpc. Although we occasionally probe an individual absorbing halo with two lines-of-sight, the absorber-absorber correlation is primarily a probe of the large scale distribution of metals around galaxies and galaxy clustering. With redshifts errors of � 23 km s 1 , we detect clustering on 0.5 Mpc scales and we see a hint of the “fingers of God” redshift-space distortion. The distribution is consistent with absorbers arising in galaxies at z = 2 with a normal correlation function, normal systematic infall velocities and unusually low random pair-wise velocity differences, more consistent with blue than with red galaxies. Absorption in gas flowing out from galaxies with a mean velocity of 250 km s 1 would produce vastly more redshift elongation than we see. The UV absorption from fast winds that Adelberger et al. (2005) see in spectra of LBGs is not representative of UV absorption that we see. Either the winds are confined to the UV luminous star forming regions of LBGs and account for under 1/3 of the absorption systems, or if they are common to all galaxies, they can not extend to 40 kpc with large velocities, while continuing to make UV absorption that we can detect. This suggests that the metals were in place in the IGM long before z = 2. Separately, we examine the absorption seen when a sight line passes a second QSO. We see 19 absorbers within ±400 km s 1 of the redshifts of the partner QSO and 30 within 1000 km s 1 . These transverse absorbers are more tightly clustered about the QSO redshift than are associated C IV absorbers seen in individual QSO spectra. The probability of seeing absorption when a sight line passes a QSO is approximately constant for impact parameters 0.1 – 1.5 Mpc. Perhaps we do not see a rapid rise in the probability at small impact parameters, because the UV from QSOs destroys some absorbers near to the QSOs. The 3D distribution of 64 absorbers around 313 QSOs is to first order isotropic, with just a hint of the anisotropy expected if the QSO UV emission is beamed into coaxial cones of half apex angle � 20 degrees towards and away from the Earth. Alternatively, QSOs might emit UV isotropically but for a surprisingly short time of only 0.3 Myr. Anisotropy is obscured because some zem values have large errors, we do not know the distance from the QSOs at which a given absorber will be destroyed, and the axis of the cone of UV radiation has an unknown angle to our line-of-sight." @default.
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• W3100721648 date "2008-01-01" @default.
• W3100721648 modified "2023-09-27" @default.
• W3100721648 title "Metal Absorption Systems in Spectra of Pairs of QSOs" @default.
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