Solar wind reconnection exhaust observed on 1997 November 23. Panel (a) shows the thermal noise spectrum from the Wind/WAVES TNR, with the electron densities derived from the plasma line shown as white diamonds. Panel (b) shows the magnetic field observed at Wind in LMN minimum variance coordinates. Panel (c) shows the proton LMN velocity, while panel (d) shows the proton density. The core electron perpendicular temperature is shown in panel (e), the core parallel temperature in panel (f), and the ratio of parallel to perpendicular core temperature in panel (g). Temperatures derived from automated fitting techniques are shown as black dots; temperatures derived from hand optimization of the fitting technique are indicated by red asterisks. Dashed vertical lines denote the boundaries of the exhaust.