tokens: so that the sightline passes through multiple separate structures with different ionization conditions and metallicities. In contrast, Veilleux et al. ( 2005 ) suggest that large variations in metallicity and ionization conditions between clouds across an absorption profile might be a signature of outflows in addition to broad complex kinematics spanning a few hundred kilometers per second, kinematics that are not consistent with rotation, α -rich abundances, and dual-trough absorption with weak absorption between. There have been few studies thus far with detailed metallicity and kinematic analyses in order to investigate this further. To improve the metallicity measurement and better determine the structures along the line of sight, a multiphase and multicomponent modeling approach would be best. Several works have undertaken such a study and found differing metallicities in each component and/or phase (e.g., Tripp et al. 2011 ; Crighton et al. 2015 , 2016 ; Muzahid et al. 2015 , 2016 ; Rosenwasser et al. 2018 ; Zahedy et al. 2019a ) and these insights could be used to determine if outflows, inflows, tidal material, etc., are present along the same sightline. In particular, a multiphase analysis would provide insights into whether outflows are primarily traced by hot, high-ionization gas with metallicities similar to the galaxy ISM metallicity and whether the lower ions along the same sightline trace cooler, more metal-poor gas entrained by the hot outflow, which is a possible solution to the total metallicity problem suggested by Kacprzak et al. ( 2019a ) that might fit the scenario we observe here. The difficulty with this method is that it requires partitioning each ion between VP components and phases, and modeling a consistent set of VP components across transitions with similar ionization phase. This is particularly challenging when absorption is saturated and the selection of lines is limited, i.e., the only H i line observed is saturated as in the system presented here. While much of our sample has coverage of multiple H i Lyman series lines and in some cases the full series to properly do a multiphase and multicomponent analysis, the J1430+014, z = 2.071 absorber is not a good candidate for this method. Without obtaining new spectra to better cover the H i Lyman series, we would need to make assumptions on how to partition the saturated H i between components and phases, which would result in over-interpreting the absorption. Furthermore, the vast majority of metallicities in the literature are total metallicities. To study the evolution of the CGM from Cosmic Noon to today, we have focused on total metallicities here. Even though metallicity is a useful diagnostic for ruling out some scenarios of gas flow origins, especially at higher redshift where CGM mixing appears to be less efficient, a variety of properties such as kinematics and galaxy morphologies must also be considered for a more accurate picture, which we have done here.
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