Surveys for z > 3 Damped Lyα Absorption Systems: The Evolution of Neutral Gas

By L. Storrie-Lombardi, A. Wolfe. 2000

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We have completed spectroscopic observations using LRIS on the Keck 1 telescope of 30 very high redshift quasars, 11 selected for the presence of damped Lyα absorption systems and 19 with redshifts z > 3.5 not previously surveyed for absorption systems. We have surveyed an additional 10 QSOs with the Lick 120'' and the Anglo-Australian Telescope. We have combined these with previous data, resulting in a statistical sample of 646 QSOs and 85 damped Lyα absorbers with column densities N ≥ 2 × 1020 atoms cm-2 covering the redshift range 0.008 ≤ z ≤ 4.694. Four main features of how the neutral gas in the universe evolves with redshift are evident from these data.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/33e80d143b441504252d5324fe7cf3bf6cbdbb5d

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Citations in the corpus

Reconciling the local galaxy population with damped Lyman α cross-sections and metal abundances (2005, methodology): “9 by a dashed line is the fitdN/dz = 0.055(1 + z)1.11 from Storrie-Lombardi & Wolfe (2000), which agrees reasonably well with thez = 0 value.”
The VLT-UVES survey for molecular hydrogen in high-redshift damped Lyman α systems: physical conditions in the neutral gas (2005, background): “For an Einstein–de Sitter cosmology, dN/dX = 3 × 10−5 for the mean redshift of our sample (Storrie-Lombardi & Wolfe 2000).”
The corals survey I: new estimates of the number density and gas content of damped lyman alpha systems free from dust bias (2001, methodology): “Since there are relatively few bright QSOs in our sample, we also show the statistics for the LBQS DLA survey (Wolfe et al. 1995) which has a limit B <∼ 19, using the column densities reported by Wolfe et al. (1995) and Storrie-Lombardi & Wolfe (2000).”
The Distribution of Metallicity in the Intergalactic Medium at z ~ 2.5: O VI and C IV Absorption in the Spectra of Seven QSOs (2003, unknown): “We use the measurements in Storrie-Lombardi & Wolfe (2000) for 2 z 3, ΩDLA = 0.0009 ± 0.0003h −1 70 .”
The Age-Metallicity Relation of the Universe in Neutral Gas: The First 100 Damped Lyα Systems (2003, background): “…census of the H I mass density Ωgas from z = 0 to 5 and found damped Lyα systems to comprise most of the neutral gas out to at least z = 4 (Wolfe et al. 1986; Lanzetta et al. 1995; Wolfe et al. 1995; Storrie-Lombardi and Wolfe 2000; Rao & Turnshek 2000; Péroux et al. 2001; Djorgovski et al. 2003).”
The HIPASS catalogue: ΩH i and environmental effects on the H i mass function of galaxies (2005, background): “…and these measurements have shown that the comoving neutral gasdensity atz = 2−5 is approximately a tenth of a percent of the present critical density of the Universe and about half of the mass density in stars at the present epoch (e.g., Storrie-Lombardi & Wolfe 2000; Péroux et al. 2003).”
The UCSD HIRES/Keck I Damped Lyα Abundance Database. II. The Implications (2001, background): “…the founding principle of the Ðrst DLA surveys (Wolfe et al. 1986) and is well supported by the correspondence of the inferred baryonic mass density of damped systems at zD 2 and the mass density in stars today (Lanzetta, Wolfe, & Turnshek 1995 ; Wolfe et al. 1995 ; Storrie-Lombardi & Wolfe 2000).”
The physics of the intergalactic medium (2007, background): “…were conducted by Wolfe et al. (1986), Lanzetta et al. (1991), Lu et al. (1993), Lu and Wolfe (1994), Lanzetta et al. (1995b), Wolfe et al. (1995), Storrie-Lombardi and Wolfe (2000), Ellison et al. (2001), Ellison et al. (2002), Colbert and Malkan (2002), Akerman et al. (2005), Srianand et al.…”
Science with ASKAP (2008, background): “1 since it relies on an interpolation between the measured number densities of damped Lyman α (DLA) absorbers at z ∼ 0 [231] and z > 2 [216, 252].”
A Population of Faint Extended Line Emitters and the Host Galaxies of Optically Thick QSO Absorption Systems (2007, background): “Interestingly, the observed dN /dz for our emitters and the one for DLAS with neutral hydrogen column densities NH i > 2 ; 1020 cm 2 (dN /dzDLA ¼ 0:26; Peroux et al. 2005; Storrie-Lombardi & Wolfe 2000) are comparable.”
New Constraints on the Lyman Continuum Escape Fraction at z ~ 1.3 (2007, background): “…and redshift distributions of the Lyα Forest (Kim et al. 1997), Lyman Limit Systems (LLSs, Storrie-Lombardi et al. 1994) and Damped Lyα systems (DLAs, Storrie-Lombardi & Wolfe 2000) to simulate the effects of IGM Lyman line and continuum absorption on the observed fluxes of galaxies at z ∼ 1.”
The ESO UVES advanced data products quasar sample: II. Cosmological evolution of the neutral gas mass density (2013, methodology): “For this reason, aΓ-function (power-law with an exponential turn-over), analogous to the Schechter function, was used to reasonably describe the observations (e.g., Storrie-Lombardi & Wolfe 2000; Péroux et al. 2003b; Noterdaeme et al. 2009).”
The evolution of ΩHI and the epoch of formation of damped Lyman α absorbers (2001, methodology): “…1.665 2.178 4 Q 2356+0139 2.07 1.661 2.039 4 Q 2356+0237 2.50 1.634 2.465 4 Q 2359+0653 3.238 1.632 3.203 21 Q 2359+0023 2.897 1.714 2.857 21 aReferences: 1) Storrie-Lombardi & Wolfe 2000; 2) Storrie-Lombardi & Hook 2000; 3) Lanzetta, Wolfe, & Turnshek 1995; 4) Wolfe et al. 1995; 5) Sargent,…”
The HI content of star-forming galaxies at z = 0.24 (2007, background): “Observations of damped Lyα absorption in QSO spectra have proven very effective at measuring the density of atomic hydrogen at high redshifts, z > 1.5 (Storrie-Lombardi & Wolfe 2000; Prochaska et al. 2005).”