Sub-mm spectroscopy and infrared interferometry of molecular layers of evolved stars

Details Sub-mm spectroscopy and infrared interferometry of molecular layers of evolved stars Sub-mm spectroscopy and infrared interferometry of molecular layers of evolved stars

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.385w&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

Astronomy and Astrophysics

Astronomy

Scientific paper

We present and discuss recent sub-mm spectroscopy of high-frequency J=7-6 SiO and SO emission toward a sample of evolved stars obtained at 5 epochs between April and December 2010 with the Atacama Pathfinder Experiment (APEX). The Figure shows the example of the SiO, J=7-6, (top left) v=1 and (top right) v=2, and 29SiO, J=7-6, (bottom left) v=0 and (bottom right) v=1 transitions toward the Mira variable R Hya. SiO maser emission shows a strongly variable spectrum as a function of pulsation phase in terms of intensities and velocity offsets, while thermal v=0 SiO lines and SO lines show less variability of the intensity and a constant velocity offset. These observations complement near- and mid-infrared interferometry of close molecular layers, most importantly water vapor and CO layers, obtained with the Very Large Telescope Interferometer (VLTI). Our observations aim at characterizing the molecular layers of evolved stars at different distances from the stellar photosphere and as a function of pulsation phase, with the ultimate goal of better understanding the mass-loss process from evolved stars. We will also discuss the importance of our APEX monitoring programme for the preparation of sub-mm interferometric mapping using ALMA.

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