PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS
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Simcoe_Precious metals.pdf
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Author(s)
Seyffert, Eduardo N.
Cooksey, Kathy
Simcoe, Robert A.
O'Meara, John M.
Kao, Melodie M.
Prochaska, J. Xavier
Date Issued
December 2013
Journal
The Astrophysical Journal
Citation
Seyffert, Eduardo N., Kathy L. Cooksey, Robert A. Simcoe, John M. O’Meara, Melodie M. Kao, and J. Xavier Prochaska. “PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS.” The Astrophysical Journal 779, no. 2 (December 20, 2013): 161.
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Author's final manuscript
Abstract
We have performed an analysis of over 34,000 Mg II doublets at 0.36 < z < 2.29 in Sloan Digital Sky Survey (SDSS) Data Release 7 quasar spectra; the catalog, advanced data products, and tools for analysis are publicly available. The catalog was divided into 14 small redshift bins with roughly 2500 doublets in each and from Monte Carlo simulations, we estimate 50% completeness at rest equivalent width W [subscript r] ≈ 0.8 Å. The equivalent width frequency distribution is described well by an exponential model at all redshifts, and the distribution becomes flatter with increasing redshift, i.e., there are more strong systems relative to weak ones. Direct comparison with previous SDSS Mg II surveys reveals that we recover at least 70% of the doublets in these other catalogs, in addition to detecting thousands of new systems. We discuss how these surveys came by their different results, which qualitatively agree but because of the very small uncertainties, differ by a statistically significant amount. The estimated physical cross section of Mg II-absorbing galaxy halos increased approximately threefold from z = 0.4 to z = 2.3, while the W [subscript r] ≥ 1 Å absorber line density, dN[subscript Mg II/d X, grew by roughly 45%. Finally, we explore the different evolution of various absorber populations—damped Lyα absorbers, Lyman limit systems, strong C IV absorbers, and strong and weaker Mg II systems—across cosmic time (0 < z < 6).
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637x/779/2/161
