Ammonia observations towards molecular and optical outflows

¹ Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Av. Diagonal 647, E-08028 Barcelona, Spain
² Instituto de Astronomía, UNAM, Apdo. Postal 70-264, 04510 México DF, Mexico
³ Laboratorio de Astrofísica Espacial y Física Fundamental, INTA, Apdo. Correos 50727, E-28080 Madrid, Spain
⁴ Instituto de Astrofísica de Andalucía, CSIC, Apdo. Correos 3004, C/ Sancho Panza s/n, E-18080 Granada, Spain

Send offprint request to: G. Anglada

Received: 14 February 1996
Accepted: 20 May 1996

Abstract

We observed the and inversion transitions of the molecule towards several regions with molecular or optical outflows: RNO 43, HH 83, HH 84, HH 86/87/88, L1641-N, L100, L483, L673, IRAS 20188+3928, L1228, L1048, HHL 73, L1251 (IRAS 22343+7501 and IRAS 22376+7455) and L1262, using the 37 m radio telescope of the Haystack Observatory. Additionally, we searched for the maser line towards nine regions, detecting a weak maser near IRAS 20188+3928. We detected and mapped emission in 14 of the 15 regions observed, and we estimated physical parameters for the high density gas. We systematically found that the position of the best candidate for the outflow excitation in each region is very close to an emission peak. From a statistical study of the data presented in this paper, together with previously published data, we conclude that the line emission is more intense towards molecular outflow sources than towards sources with only optical outflows. Therefore, molecular outflows appear to be associated with larger amounts of high density gas. This result suggests a possible evolutive scheme in which young objects associated with molecular outflows lose progressively their neighboring high-density gas, weakening both the emission and the molecular outflow in the process, and making optical jets more easily detectable as the total amount of gas decreases.