Diagnosing shock temperature with NH${}_3$ and H${}_2$O profiles

Abstract

In a previous study of the L1157 B1 shocked cavity, a comparison between NH${}_3$(1${}_0$-$0_0$) and H${}_2$O(1${}_{10}$--1${}_{01}$) transitions showed a striking difference in the profiles, with H${}_2$O emitting at definitely higher velocities. This behaviour was explained as a result of the high-temperature gas-phase chemistry occurring in the postshock gas in the B1 cavity of this outflow. If the differences in behaviour between ammonia and water are indeed a consequence of the high gas temperatures reached during the passage of a shock, then one should find such differences to be ubiquitous among chemically rich outflows. In order to determine whether the difference in profiles observed between NH${}_3$ and H${}_2$O is unique to L1157 or a common characteristic of chemically rich outflows, we have performed Herschel-HIFI observations of the NH${}_3$(1${}_0$-0${}_0$) line at 572.5 GHz in a sample of 8 bright low-mass outflow spots already observed in the H${}_2$O(1${}_{10}$--1${}_{01}$) line within the WISH KP. We detected the ammonia emission at high-velocities at most of the outflows positions. In all cases, the water emission reaches higher velocities than NH${}_3$, proving that this behaviour is not exclusive of the L1157-B1 position. Comparisons with a gas-grain chemical and shock model confirms, for this larger sample, that the behaviour of ammonia is determined principally by the temperature of the gas.

Accepted for publication in the Monthly Notices of the Royal Astronomical Society

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• Sulfur Chemistry in L1157-B1
• Nitrogen oxide in protostellar envelopes and shocks: the ASAI survey
• Tracing shock type with chemical diagnostics: an application to L1157
• History-independent tracers: Forgetful molecular probes of the physical conditions of the dense interstellar medium
• Shock-type inference of L1157 B2 using methanol desorption