使用VERA对J=1-0、v=1和v=2 SiO脉泽朝向小狮子座R的相对天体测量
Relative astrometry of the J=1-0, v=1 and v=2 SiO masers towards R Leonis Minoris using VERA
摘要：
富氧渐近巨星支（AGB）星是SiO和H $_2$ O脉泽谱线的强发射体，其脉泽谱线分别位于43（J=1-0，v=1和2）和22 GHz。VLBI对脉泽辐射的观测为AGB星拱星包层最内层的取样提供了一个独特的工具。然而，在实现天体测量对准的v=1和v=2 SiO脉泽地图的困难，传统上阻止了一个独特的解释的意见，在物理基础条件，这取决于性质的SiO泵机制。利用VERA的天体测量能力，我们对SiO和H $_2$ O脉泽向RLMi的辐射进行了观测。由于参考校准品的发射太弱，我们不得不开发一种特殊的方法来精确地关联两种跃迁的坐标。我们提出了相对天体测量对准v=1和v=2 J=1-0 SiO脉泽地图，在多个时代，并讨论天体物理结果。天文测量信息纳入SiO脉泽的地图挑战了目前的理论模型中的弱点，这将需要进一步的改进，以解决观测结果。
英文摘要：
Oxygen-rich Asymptotic Giant Branch (AGB) stars are intense emitters of SiO and H$_2$O maser lines at 43 (J=1-0, v=1 and 2) and 22 GHz, respectively. VLBI observations of the maser emission provides a unique tool to sample the innermost layers of the circumstellar envelopes in AGB stars. Nevertheless, the difficulties in achieving astrometrically aligned v=1 and v=2 SiO maser maps have traditionally prevented a unique interpretation of the observations in terms of physical underlying conditions, which depend on the nature of the SiO pumping mechanism. We have carried out observations of the SiO and H$_2$O maser emission towards RLMi, using the astrometric capabilities of VERA. Due to the too-weak emission of the reference calibrator we had to develop a special method to accurately relate the coordinates for both transitions. We present relative astrometrically aligned v=1 and v=2 J=1-0 SiO maser maps, at multiple epochs, and discuss the astrophysical results. The incorporation of astrometric information into the maps of SiO masers challenges the weak points in the current theoretical models, which will need further refinements to address the observations results.
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