Evidence for Evolution in Weak MgII Absorbers at z < 1.5

Details Evidence for Evolution in Weak MgII Absorbers at z < 1.5 Evidence for Evolution in Weak MgII Absorbers at z < 1.5

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.7709e&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #77.09; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a survey of 92 weak MgII absorbers [those with Wr(2796)<0.3 Å] in 132 HIRES and UVES quasar spectra. The spectra are 97% complete to Wr(2796) = 0.02 Å over the redshift range 0.15--1.45 and have a cumulative redshift path of 76. We find pronounced evidence for evolution in the redshift path density, dN/dz, which monotonically decreases toward higher redshift. Assuming dN/dz ∝ (1+z)γ, we estimate γ = -1.0±0.5, where 0.5<γ<1.0 would represent no evolution in the population of absorbers. Similarly, assuming dN/dz ∝ (1+z)2+ɛ \Ωm(1+z)3+ΩΛ -1/2, we estimate ɛ = -2.0±1.0, where ɛ = 0 would represent no evolution. We also discovered eight MgII absorbing systems with Wr(2796)<0.02 Å and three with Wr(2796)<0.01 Å, allowing us to explore the equivalent width, column density, and Doppler b parameter distributions down to very small values of Wr(2796).

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