Chemically active outflow L 1157
IGN Observatorio Astronómico Nacional, Apartado 1143, 28800 Alcalá de Henares, Spain
Corresponding author: R. Bachiller, firstname.lastname@example.org
Accepted: 6 April 2001
We present millimeter-wave maps of the L 1157 bipolar outflow in several molecular emission lines. The CO emission traces the bulk of the outflowing gas in the red and blue shifted lobes displaying a remarkable S-shaped symmetry indicating the presence of a precessing jet. We determine the physical characteristics of the CO flow and show evidence for 3 or 4 independent episodes of mass ejection from the source. Molecules such as C3H2, N2H+ and DCO+ are seen to be abundant only in the quiescent medium, and result to be the best tracers of the high-density core surrounding the driving source of the outflow. Other molecules (SiO, CH3OH, H2CO, HCN, CN, SO, SO2) are abundant in the outflow lobes, but exhibit strong emission gradients. Multiline observations of some species indicate that these gradients are not simply due to excitation effects, but are caused by an actual stratification in the chemical composition of the shocked molecular gas. Shock tracers such as SiO, CH3OH, and sulphur-bearing molecules result to be the most promising candidates as potential chemical clocks to study the evolution of outflows. The characteristics of the L 1157 outflow, when compared to those of other outflows from Class 0 sources, indicate that L 1157 is the prototype of a category of bipolar outflows around Class 0 protostars which we denominate "chemically active outflows" .
Key words: stars: formation / interstellar medium: individual objects: L 1157 / interstellar medium: jets and outflows / interstellar medium: molecules
© ESO, 2001