论文标题
NGC 3079中的60 kpc银河风锥
A 60-kpc Galactic Wind Cone in NGC 3079
论文作者
论文摘要
银河风与强烈的恒星形成和AGN有关。根据它们的形成机理和速度，它们可能会从宿主星系中去除大量的气体，从而抑制恒星的形成，富集了乳层间培养基并塑造圆形的气体。但是，这些风的长期演变仍然是未知的。我们报告了从Galaxy的NGC 3079到至少60 kpc的风的检测。我们在FUV线排放中检测到60 kpc的风（如Galex中的宽FUV滤波器推断），在X射线中至少30〜kpc。形态，亮度，温度和密度表明发射来自震惊的材料，O/Fe比率意味着X射线发射气体富含II型超新星。如果是这样，那么从简单的冲击模型推断出的速度约为500 km/s，足以逃脱银河系。但是，可见成分的风中的推断动能要比规范热的超级风模型小得多。
Galactic winds are associated with intense star formation and AGNs. Depending on their formation mechanism and velocity they may remove a significant fraction of gas from their host galaxies, thus suppressing star formation, enriching the intergalactic medium, and shaping the circumgalactic gas. However, the long-term evolution of these winds remains mostly unknown. We report the detection of a wind from NGC 3079 to at least 60 kpc from the galaxy. We detect the wind in FUV line emission to 60 kpc (as inferred from the broad FUV filter in GALEX) and in X-rays to at least 30~kpc. The morphology, luminosities, temperatures, and densities indicate that the emission comes from shocked material, and the O/Fe ratio implies that the X-ray emitting gas is enriched by Type II supernovae. If so, the speed inferred from simple shock models is about 500 km/s, which is sufficient to escape the galaxy. However, the inferred kinetic energy in the wind from visible components is substantially smaller than canonical hot superwind models.
