A Survey of MgII Absorption at 2 < z < 6 with Magellan / FIRE: I: Sample and Evolution of the MgII Frequency

TL;DR

This survey of MgII absorption lines at high redshift reveals the evolution of absorber strength and density, indicating early establishment of MgII halo structures and their connection to star formation activity over cosmic time.

Contribution

First systematic high-redshift MgII survey using infrared spectra, discovering the most distant MgII system and analyzing its evolution from z=2.5 to 6.3.

Findings

Weak MgII systems show no evolution from z=0.4 to 5.5.

Strong MgII systems increase in density until z~3 then decline.

MgII absorber properties suggest early halo formation and link to star formation rates.

Abstract

We present initial results from the first systematic survey for MgII quasar absorption lines at z > 2.5. Using infrared spectra of 46 high-redshift quasars, we discovered 111 MgII systems over a path covering 1.9 < z < 6.3. Five systems have z > 5, with a maximum of z = 5.33 - the most distant MgII system now known. The comoving MgII line density for weaker systems (Wr < 1.0A) is statistically consistent with no evolution from z = 0.4 to z = 5.5, while that for stronger systems increases three-fold until z \sim 3 before declining again towards higher redshifts. The equivalent width distribution, which fits an exponential, reflects this evolution by flattening as z approaches 3 before steepening again. The rise and fall of the strong absorbers suggests a connection to the star formation rate density, as though they trace galactic outflows or other byproducts of star formation. The weaker systems' lack of evolution does not fit within this interpretation, but may be reproduced by extrapolating low redshift scaling relations between host galaxy luminosity and absorbing halo radius to earlier epochs. For the weak systems, luminosity-scaled models match the evolution better than similar models based on MgII occupation of evolving CDM halo masses, which greatly underpredict dN/dz at early times unless the absorption efficiency of small haloes is significantly larger in the early universe. Taken together, these observations suggest that the general structure of MgII-bearing haloes was put into place early in the process of galaxy assembly. Except for a transient appearance of stronger systems near the peak epoch of cosmic star formation, the basic properties of MgII absorbers have evolved fairly little even as the (presumably) associated galaxy population grew substantially in stellar mass and half light radius.