PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS
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...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | en_US |
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2014
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| Online Access: | http://hdl.handle.net/1721.1/88552 https://orcid.org/0000-0003-3769-9559 |
| _version_ | 1826205552960602112 |
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| author | Seyffert, Eduardo N. Cooksey, Kathy Simcoe, Robert A. O'Meara, John M. Kao, Melodie M. Prochaska, J. Xavier |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Seyffert, Eduardo N. Cooksey, Kathy Simcoe, Robert A. O'Meara, John M. Kao, Melodie M. Prochaska, J. Xavier |
| author_sort | Seyffert, Eduardo N. |
| collection | MIT |
| description | 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). |
| first_indexed | 2024-09-23T13:14:58Z |
| format | Article |
| id | mit-1721.1/88552 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T13:14:58Z |
| publishDate | 2014 |
| record_format | dspace |
| spelling | mit-1721.1/885522022-09-28T12:54:31Z PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS Seyffert, Eduardo N. Cooksey, Kathy Simcoe, Robert A. O'Meara, John M. Kao, Melodie M. Prochaska, J. Xavier Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Seyffert, Eduardo N. Cooksey, Kathy Simcoe, Robert A. 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). National Science Foundation (U.S.) (Grant AST-0908920) National Science Foundation (U.S.) (Grant AST-1109915) 2014-08-06T18:10:30Z 2014-08-06T18:10:30Z 2013-12 2013-08 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/88552 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. https://orcid.org/0000-0003-3769-9559 en_US http://dx.doi.org/10.1088/0004-637x/779/2/161 The Astrophysical Journal Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf arXiv |
| spellingShingle | Seyffert, Eduardo N. Cooksey, Kathy Simcoe, Robert A. O'Meara, John M. Kao, Melodie M. Prochaska, J. Xavier PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS |
| title | PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS |
| title_full | PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS |
| title_fullStr | PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS |
| title_full_unstemmed | PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS |
| title_short | PRECIOUS METALS IN SDSS QUASAR SPECTRA. II. TRACKING THE EVOLUTION OF STRONG, 0.4 < z < 2.3 Mg II ABSORBERS WITH THOUSANDS OF SYSTEMS |
| title_sort | precious metals in sdss quasar spectra ii tracking the evolution of strong 0 4 z 2 3 mg ii absorbers with thousands of systems |
| url | http://hdl.handle.net/1721.1/88552 https://orcid.org/0000-0003-3769-9559 |
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