PACS Oxygen Spectroscopy of High Velocity SQUARE_BRACKET_OPENCIISQUARE_BRACKET_CLOSE Outflows in PG1206+459

We have discovered extreme velocity CII 158 um line emission from the z 1.2 hyperluminous QSO PG 1206+459. The CII line emission is concentrated in twin lobes of emission roughly centered on the CO emission but displaced +/ 1500 km/s with respect to the CO line core. The mass traced in the CII line is quite large about 5E9 M(solar) in each lobe or 13% of the total molecular gas mass in the host galaxy. We interpret this symmetric CII velocity structure as an outflow, likely driven by the AGN. The velocities of the CII lobes are larger than the escape velocity, so much of this material may leave the galaxy quenching both star formation and AGN activity, and transforming it into a redanddead passive galaxy. The CO line profile also shows a broad and blueshifted component that may represent an additional molecular component to the outflow, although a merger origin is also possible. In OT1 we were awarded 2.9 hours of PACS spectroscopy (not yet scheduled) to observe the OI 63 um, OIII 52 and 88 um, and OIV 26 um lines from the blue component of the line. Here we ask for an additional 10.2 hours of PACS time to widen our spectral scan to enclose the newly discovered (March 2011) red lobe and significantly improve our detection limit over the entire velocity range. These observations will be used to constrain the physical conditions, ionization structure, total mass, and radiative environment of the outflowing material using extinctionfree probes. Our CII observations of PG1206 represent the first time that massive outflows have been detected in the CII line a well established tracer of photodissociated molecular gas. The proposed Herschel observations will lay the groundwork for future studies of molecular outflows using CII and other farIR lines inthe early universe that will soon be possible with ALMA. truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]