Abstract
The ESTEMA (Expanded Study on Stellar Masers) project is one of three Large Programs of the KaVA (the combined array of the Korean VLBI Network and Japanese VLBI Exploration of Radio Astrometry), and conducted in 2015-2016. It aims to publish a database of the largest sample of VLBI images of circumstellar water (H2O) and silicon-monoxide (SiO) maser sources towards circumstellar envelopes (CSEs) of 80 evolved stars in late AGB to early post-AGB phase. Here we present the specifications of the ESTEMA observations and the planned scientific goals in order to share the basic information of the ESTEMA with astronomical community and encourage future collaborations with the ESTEMA and future follow-up observations for the targeted stars.
Highlights
Using the unique specifications of the Korean VLBI Network (KVN) and Japanese VLBI Exploration of Radio Astrometry (VERA), which enable, respectively, simultaneous observations of the masers at four frequency bands (around 22, 43, 86 and 129 GHz) and high-precision astrometry using the dual-beam receiving system, as well as the form of KaVA for high
We aims to monitor ∼20 stars in VLBI intensively throughout a few pulsation cycles (2–10 years)
The first stage of the Large Projects named ESTEMA, whose name comes from Spanish “estema” (English “stemma”, meaning “a family line”), will select such 20 stars from the snapshot imaging surveys for 80 stars, whose large fraction of maser lines will be mapped through the whole stellar pulsation cycle
Summary
Using the unique specifications of the Korean VLBI Network (KVN) and Japanese VLBI Exploration of Radio Astrometry (VERA), which enable, respectively, simultaneous observations of the masers at four frequency bands (around 22, 43, 86 and 129 GHz) and high-precision astrometry using the dual-beam receiving system, as well as the form of KaVA for high Quality imaging [1], we have planned KaVA Large Projects to conduct more systematic legacy observations projects for circumstellar masers.
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