The circumgalactic medium (CGM) plays a vital role in the formation and evolution of galaxies, acting as a lifeline between galaxies and the surrounding intergalactic medium. In this study, we leverage a unique sample of quasar pairs to investigate the properties of the CGM with absorption line tomography. We present a new sample of medium-resolution Keck/ESI, Magellan/MagE, and VLT/XSHOOTER spectra of 29 quasar pairs at redshift 2 <
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Abstract z < 3. We supplement the sample with additional spectra of 32 pairs from the literature, creating a catalog of 61 quasar pairs with angular separations between 1.″7 and 132.″9 and projected physical separations (r ⊥) between 14 kpc and 887 kpc. We construct a catalog of 906 metal-line absorption doublets of Civ (λλ 1548, 1550) with equivalent widths ranging from 6 m Å ≤W r ,1550≤ 2053 m Å. The best-fit linear model to the log-space equivalent width frequency distribution ( ) of the sample yields coefficients ofm = −1.44 ± 0.16 andb = −0.43 ± 0.16. To constrain the projected extent of Civ , we calculate the transverse autocorrelation function. The flattening of the autocorrelation function at lowr ⊥provides a lower limit for the coherence length of the metal enriched CGM—on the order of 200h −1comoving kpc. This physical size constraint allows us to refine our understanding of the metals in the CGM, where the extent of Civ in the CGM depends on gas flows, feedback, timescale of metal injection and mixing, and the mass of the host galaxies. -
Abstract We use medium-resolution Keck/Echellette Spectrograph and Imager spectroscopy of bright quasars to study cool gas traced by Ca
ii λλ 3934, 3969 and Nai λλ 5891, 5897 absorption in the interstellar/circumgalactic media of 21 foreground star-forming galaxies at redshifts 0.03 <z < 0.20 with stellar masses 7.4 ≤ logM */M ⊙≤ 10.6. The quasar–galaxy pairs were drawn from a unique sample of Sloan Digital Sky Survey quasar spectra with intervening nebular emission, and thus have exceptionally close impact parameters (R ⊥< 13 kpc). The strength of this line emission implies that the galaxies’ star formation rates (SFRs) span a broad range, with several lying well above the star-forming sequence. We use Voigt profile modeling to derive column densities and component velocities for each absorber, finding that column densitiesN (Caii ) > 1012.5cm−2(N (Nai ) > 1012.0cm−2) occur with an incidencef C(Caii ) = 0.63+0.10−0.11(f C(Nai ) = 0.57+0.10−0.11). We find no evidence for a dependence off Cor the rest-frame equivalent widthsW r (Caii K) orW r (Nai 5891) onR ⊥orM *. Instead,W r (Caii K) is correlated with local SFR at >3σ significance, suggesting that Caii traces star formation-driven outflows. While most of the absorbers have velocities within ±50 km s−1of the host redshift, their velocity widths (characterized by Δv 90) are universally 30–177 km s−1larger than that implied by tilted-ring modeling of the velocities of interstellar material. These kinematics must trace galactic fountain flows and demonstrate that they persist atR ⊥> 5 kpc. Finally, we assess the relationship between dust reddening andW r (Caii K) (W r (Nai 5891)), finding that 33% (24%) of the absorbers are inconsistent with the best-fit Milky WayE (B −V)-W r relations at >3σ significance.