Nucleosynthesis in AGB stars traced by oxygen isotopic ratios I. Determining the stellar initial mass by means of the 17O/1
Abstract
The data presented in this study were obtained with three different telescopes. The Institut de Radio Astronomie Millimetrique (IRAM) 30m telescope at Pico Veleta, Spain (Program ID 042-12, 164-12) using the EMIR heterodyne receiver in dual band observation mode in the E0(90GHz)/E2(230GHz) configuration; the Atacama Pathfinder EXperiment(APEX) 12m telescope on the Chajnantor Plateau, Chile (Program ID 090.D-0290, 091.D-0813, 094.D-0851A), in the SHeFI 230GHz band, and the Caltech Submillimeter Observatory (CSO) at Mauna Kea, Hawaii, using the 230GHz receiver. The sources were observed using position switching or wobbler switching mode to attain flat baselines. The pointing of the telescope was checked repeatedly throughout the observations using strong CO and continuum sources. The reduction and analysis of all data were performed using the GILDAS CLASS software package. After removing faulty scans and spikes, a firstorder polynomial baseline was subtracted from each scan. The individual baseline-subtracted scans obtained for a given source were then averaged using an inverse quadratic system temperature weighting. Finally the data were rebinned to obtain a suitable signal-to-noise ratio (S/N), generally S/N=3-5 for a velocity resolution of 2km/s (the typical linewidth being around 20-40km/s).
(2 data files).- Publication:
-
VizieR Online Data Catalog
- Pub Date:
- February 2017
- DOI:
- 10.26093/cds/vizier.36000071
- Bibcode:
- 2017yCat..36000071D
- Keywords:
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- Stars: late-type;
- Spectra: millimetric/submm