SpitzerObservations of HH 54 and HH 7–11: Mapping the H₂Ortho‐to‐Para Ratio in Shocked Molecular Gas

We report the results of spectroscopic mapping observations carried out toward the Herbig-Haro objects HH 7-11 and HH 54 over the 5.2-37 μm region using the Infrared Spectrograph on the Spitzer Space Telescope . These observations have led to the detection and mapping of the S (0)- S (7) pure rotational lines of molecular hydrogen, together with emissions in fine-structure transitions of Ne + , Si + , S, and Fe + . The H 2 rotational emissions indicate the presence of warm gas with a mixture of temperatures in the range 400-1200 K—consistent with the expected temperature behind nondissociative shocks of velocity ~10-20 km s -1 —while the fine-structure emissions originate in faster shocks of velocity ~35-90 km s -1 that are dissociative and ionizing. The H 2 ortho-to-para ratio is quite variable, typically falling substantially below the equilibrium value of 3 attained at the measured gas temperatures. The nonequilibrium ortho-to-para ratios are characteristic of temperatures as low as ~50 K, and are a remnant of an earlier epoch, before the gas temperature was elevated by the passage of a shock. Correlations between the gas temperature and H 2 ortho-to-para ratio show that ortho-to-para ratios <0.8 are attained only at gas temperatures below ~900 K; this behavior is consistent with theoretical models in which the conversion of para- to ortho-H 2 behind the shock is driven by reactive collisions with atomic hydrogen, a process that possesses a substantial activation energy barrier ( E A / k ~ 4000 K) and is therefore very inefficient at low temperature. The lowest observed ortho-to-para ratios of only ~0.25 suggest that the shocks in HH 54 and HH 7 are propagating into cold clouds of temperature ≲50 K in which the H 2 ortho-to-para ratio is close to equilibrium.