Dataset for A Multi-Wavelength Study of the Symbiotic Mira HM Sge with SOFIA & HST

We have targeted the dusty symbiotic mira system HM Sge with four instruments from the IR to the UV. We have used these observations along with archival observations to study how the system has been evolving after its 1975 nova-like outburst. We have detected ro-vibrational water emission in a symbiotic system for the first time using new EXES high spectral resolution infrared spectroscopy. The features, detected in emission, have velocities consistent with the systemic velocity but do not show any clear evidence of high velocity outflows. Mid-infrared photometry and grism spectroscopy show that the oxygen-rich Asymptotic Giant Branch (AGB) dust and dust output has shown little to no change over the past 39 years. In the optical/UV, we detect three main NII nebular features that were detected 22 years ago, and they show little to no movement; several of the previously detected NII features are no longer visible. New UV spectroscopy has shown that the nebular environment continues to steadily relax after the system's 1975 outburst. The data suggest however, that the hot component has increased in temperature from 200,000 K in 1989 to now greater than 250,000 K. Our new and archival observations suggest that the evolution of the system after its outburst is swift with little to no major changes after a period of a couple years.

我们针对富尘共生米拉变星系统HM Sge，采用覆盖从红外到紫外波段的四台观测仪器。我们结合本次观测与存档观测数据，探究该系统在1975年类新星爆发后的演化历程。借助全新的EXES高分辨率红外光谱观测，我们首次在共生系统中探测到了水的振转发射谱线。本次探测到的发射谱线特征其速度与系统本征速度一致，未观测到明显的高速外流迹象。中红外测光与光栅光谱观测显示，富氧渐近巨星支（Asymptotic Giant Branch, AGB）尘埃及其尘埃产出量在过去39年间几乎无显著变化。在光学/紫外波段，我们探测到22年前曾被观测到的三个主要的[N II]星云特征，这些特征几乎未发生位移；此前观测到的部分[N II]特征现已消失。新的紫外光谱观测表明，该系统自1975年爆发后，星云环境仍在持续平稳地趋于松弛状态。不过观测数据显示，系统的热成分温度已从1989年的200,000 K升高至当前的250,000 K以上。我们结合新观测与存档数据的分析结果表明，该系统在爆发后的演化速度较快，仅在最初数年内发生显著变化，后续几乎无明显演化。