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Using HST/COS/STIS and HIRES/Keck high-resolution spectra, we have studied aremarkable HI absorbing complex at z=0.672 toward the quasar Q1317+277. The HIabsorption has a velocity spread of 1600 km/s, comprises 21 Voigt profilecomponents, and resides at an impact parameter of D=58 kpc from a bright, highmass [log(M_vir/M_sun) ~ 13.7] elliptical galaxy that is deduced to have a 6Gyr old, solar metallicity stellar population. Ionization models suggest themajority of the structure is cold gas surrounding a shock heated cloud that iskinematically adjacent to a multi-phase group of clouds with detected CIII, CIVand OVI absorption, suggestive of a conductive interface near the shock. Thededuced metallicities are consistent with the moderate in situ enrichmentrelative to the levels observed in the z ~ 3 Ly-alpha forest. We interpret theHI complex as a metal-poor filamentary structure being shock heated as itaccretes into the halo of the galaxy. The data support the scenario of an earlyformation period (z > 4) in which the galaxy was presumably fed by cold-modegas accretion that was later quenched via virial shocking by the hot halo suchthat, by intermediate redshift, the cold filamentary accreting gas iscontinuing to be disrupted by shock heating. Thus, continued filamentaryaccretion is being mixed into the hot halo, indicating that the star formationof the galaxy will likely remain quenched. To date, the galaxy and the HIabsorption complex provide some of the most compelling observational datasupporting the theoretical picture in which accretion is virial shocked in thehot coronal halos of high mass galaxies.

Quenched Cold Accretion of a Large Scale Metal-Poor Filament due to Virial Shocking in the Halo of a Massive z=0.7 Galaxy