Emission-Line Datacubes of the HH 32 Stellar Jet
  We analyze datacubes of over 60 emission lines in the HH 32 stellar jet
acquired with the Keck Cosmic Web Imager (KCWI). The data cover the
less-explored blue portion of the spectrum between 3586A and 6351A , and have
both high spectral (R $\sim$ 10000) and spatial ($\lesssim$ 1" ) resolution.
The study includes all three major ionization states of oxygen, three Balmer
lines, multiple lines of Fe II and Fe III, as well as the first datacubes ever
acquired for important unblended diagnostic lines such as He II $\lambda$4686,
Ca I $\lambda$3933, and Mg I] $\lambda$4571. The data cubes generally sort
according to excitation, and have a relatively continuous progression from the
highest-excitation ions (He II, O III) through the intermediate-excitation ions
(O I and H I) to the lowest-excitation ions (Ca II and Mg I). Merging the KCWI
cubes with HST images leads to several new insights about the flow, including
evidence for bow shocks, partial bow shocks, spur shocks, Mach disks, jet
deflection shocks, a wiggling jet, and potential shock precursors. The most
surprising result is that one of the velocity components of Fe II in the Mach
disk suddenly increases in flux relative to other lines by a factor of two,
implying that the Mach disk vaporizes dust in the jet. Hence, jets must
accelerate or entrain dust to speeds of over 300 km/s without destroying the
grains.
