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Title:
A detailed study toward the Water fountain IRAS 15445-5449
Authors:
Pérez-Sánchez, Andrés F.; López, Rebeca García; Vlemmings, Wouter; Tafoya, Daniel
Affiliation:
AA(European Souther Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago de Chile ), AB(Dublin Institute for Advance Studies, 31 Fitzwilliam Place, Dublin 2, Ireland), AC(Department of Space, Earth and Environment, Chalmers University of technology, Onsala Space Obsevatory, 439 92 Onsala, Sweden.), AD(Department of Space, Earth and Environment, Chalmers University of technology, Onsala Space Obsevatory, 439 92 Onsala, Sweden.)
Publication:
Astrophysical Masers: Unlocking the Mysteries of the Universe, Proceedings of the International Astronomical Union, IAU Symposium, Volume 336, pp. 355-358
Publication Date:
08/2018
Origin:
CUP
Keywords:
stars: AGB and Post-AGB, Masers, stars: late-type
Abstract Copyright:
(c) 2018: Copyright © International Astronomical Union 2018
DOI:
10.1017/S1743921317009309
Bibliographic Code:
2018IAUS..336..355P

Abstract

Post-Asymptotic giant branch (post-ABG) sources with high-velocity spectral features of H2O maser emission detected toward their circumstellar envelopes (CSEs) are known as Water Fountain (WF) nebulae. These are low- or intermediate-mass Galactic stellar sources that are undergoing the late stages of an intense mass-loss process. The velocity and the spatial distribution of the H2O maser spectral features can provide information about the kinematics of the molecular gas component of their CSEs. Hence, observational studies toward WF nebulae could help to better understand the formation of the asymmetric structures (hundred to thousand AUs) commonly seen toward Planetary nebulae (PNe). Here we present preliminary results of observations done toward the WF IRAS 15445-5449 using the Australia Telescope Compact Array (ATCA) and the Very Large Telescope (SINFONI/VLT). Assuming that the pumping of the H2O maser transitions is a consequence of shocks between different velocity winds, the spatial distribution of the emission shed light on the scales of the regions affected by the propagation of the shock-fronts.
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