Cross-calibrated VLA observations of H_2O maser and 1.3 CM continuum emission in IRAS 18162-2048 (= HH 80-81 IRS)

Details Cross-calibrated VLA observations of H_2O maser and 1.3 CM continuum emission in IRAS 18162-2048 (= HH 80-81 IRS) Cross-calibrated VLA observations of H_2O maser and 1.3 CM continuum emission in IRAS 18162-2048 (= HH 80-81 IRS)

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...345l...5m&link_type=abstract

Astronomy and Astrophysics, v.345, p.L5-L8 (1999)

Astronomy and Astrophysics

Astrophysics

17

Stars: Individual: Iras 18162-2048, Stars: Individual: Hh 80-81 Irs, Stars: Formation, Ism: Herbig-Haro Objects, Ism: Jets And Outflows

Scientific paper

We report simultaneous continuum (1.3 cm) and H_2O maser line observations, made with the Very Large Array (A configuration), toward IRAS 18162-2048, the luminous exciting source of the HH 80-81 complex. The continuum observations, cross-calibrated with the H_2O maser emission, provide information of the thermal jet of this young massive star with unprecedented angular resolution and fidelity. We find that the jet is already collimated on scales smaller than 100 AU. The analysis of the new 1.3 cm data and of previously obtained 3.6 cm data show that the source has the frequency dependences in major axis and flux density that characterize biconical jets. In particular, we find theta_maj ~ nu (-0.7+/-0.1) and S_ν ~ nu (0.8+/-0.1) . An improved determination of the mass loss rate in ionized gas, dot M_ion =~ 9 x 10(-7) M_sun yr(-1) , is provided with these new observations. As it was known from previous studies, the H_2O maser emission does not coincide with the thermal jet but with a faint source of radio continuum emission displaced by ~ 7'' to the northeast of the thermal jet. The H_2O masers appear in two compact clusters separated by ~ 20 mas. One of the clusters is formed by spots in a linear geometry. The kinematics of these maser spots and their large blueshift with respect to the radial velocity of the parental molecular cloud suggest that they trace material accelerated by outflow phenomena, instead of a possible disk.

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