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Tracing the Evolution of the Cool Gas in CGM and IGM Environments through Mg ii Absorption from Redshift z = 0.75 to z = 1.65 Using DESI-Y1 Data
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Tracing the Evolution of the Cool Gas in CGM and IGM Environments through Mg ii Absorption from Redshift z = 0.75 to z = 1.65 Using DESI-Y1 Data
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Journal Article
Tracing the Evolution of the Cool Gas in CGM and IGM Environments through Mg ii Absorption from Redshift z = 0.75 to z = 1.65 Using DESI-Y1 Data
2025
Overview
We present a measurement of the mean absorption of cool gas traced by Mg ii (λλ2796, 2803) around emission line galaxies (ELGs), spanning spatial scales from 20 kpc to 10 Mpc. The measurement is based on crossmatching the positions ELGs at z = 0.75–1.65 and the metal absorption in the spectra of background quasars with data provided by the Year 1 sample of the Dark Energy Spectroscopic Instrument. The ELGs are divided into two redshift intervals: 0.75 < z < 1.0 and 1.0 < z < 1.65. We find that the composite quasar spectra constructed by stacking the ELG-QSO pairs evolve with redshift, with z > 1 having a systematically higher signal of Mg ii absorption. Within 1 Mpc, the covering fraction of the cool gas at z > 1 is higher than that of z < 1. The enhancement becomes less apparent especially if the projected distance rp > 1 Mpc. ELGs with higher stellar mass and star formation rate (SFR) yield higher clustering of Mg ii absorbers at z < 1. For z > 1, the covering fractions with different SFRs show little difference. The higher Mg ii absorption at higher redshift supports the observations of higher star formation at cosmic noon. Converting the Mg ii absorbers to unsaturated Si ii, our estimate indicates that the metal abundance of Si ii ranges from 0.7 to 1.2 × 10−6 from z = 0.9 to 1.3. The growth of low-ionization metal abundance strongly suggests a metal-enriched circumgalactic medium and an increased presence of cool gas in the intergalactic medium toward higher redshifts.
Publisher
IOP Publishing
Subject
