Solar-Metallicity Gas in the Extended Halo of a Galaxy at $z\sim 0.12$

We present the detection and analysis of a weak low-ionization absorber at $z = 0.12122$alongtheblazarsightlinePG$1424+240$, using spectroscopic data from both $HST$/COS and STIS. The absorber is a weak Mg II analogue, with incidence of weak C II and Si II, along with multi-component C IV and O VI. The low ions are tracing a dense ($n_H\sim {10}^{-3}$ cm${}^{-3}$) parsec scale cloud of solar or higher metallicity. The kinematically coincident higher ions are either from a more diffuse ($n_H\sim {10}^{-5}-{10}^{-4}$ cm${}^{-3}$) photoionized phase of kiloparsec scale dimensions, or are tracing a warm (T $\sim 2\times {10}^5$ K) collisionally ionized transition temperature plasma layer. The absorber resides in a galaxy overdense region, with 18 luminous ($> L^*$)galaxieswithinaprojectedradiusof$5$Mpcand$750$kms$^{-1}$ of the absorber. The multi-phase properties, high metallicity and proximity to a $1.4$ $L^{\ast }$ galaxy, at $\rho \sim 200$ kpc and $\mathrm{\mid }\mathrm{\Delta }v\mathrm{\mid }=11$ km s${}^{-1}$ separation, favors the possibility of the absorption tracing circumgalactic gas. The absorber serves as an example of weak Mg II - O VI systems as a means to study multiphase high velocity clouds in external galaxies.