JWST预览：船底座西壁中H $_2$、Br- $γ$和K-连续体的自适应光学图像
A JWST Preview: Adaptive-Optics Images of H$_2$, Br-$γ$, and K-continuum in Carina's Western Wall
摘要：
我们提出了第一个宽视场近红外自适应光学图像船底座的西墙（G287.38-0.62），其中一个最明亮和最明确的辐射接口已知的大规模恒星形成的区域。新的窄带H $_2$ 2.12 $μ$ m、Br- $γ$和K-连续谱图像追踪了来自云的光蒸发流，并确定了来自周围大质量恒星的紫外辐射激发分子氢发出荧光的位置。随着$\sim$ 1.5“$\times$ 2.9”的视野和60 $-$ 110 mas之间的空间分辨率，新的图像显示了一个壮观的细节水平在一个大面积，并预示着什么JWST应该实现。壁是凸形的，在其顶点附近有一个大的三角形延伸。顶点附近的界面由3个$-$ 4规则间隔的脊组成，投影间距为$\sim$ 2000 AU，表明存在大规模的动态重要磁场。长城的北部边缘断裂成几个宽度为$\sim$ 1800 AU的后掠碎片，类似于开尔文-亥姆霍兹不稳定性，长城的南部也显示出复杂的形态，包括半波长为2500 AU的正弦曲线状变化。虽然解离锋必须增加沿着墙表面的密度，但它不会分解成指向电离源的柱子，如果锋触发新恒星形成，可能会发生这种情况。我们发现，MHO 1630是一个H型$_2$外流，在壁的北部没有明确的驱动源，它由一系列排列成一条线的弓形激波组成。
英文摘要：
We present the first wide-field near-infrared adaptive optics images of Carina's Western Wall (G287.38-0.62), one of the brightest and most well-defined irradiated interfaces known in a region of massive star formation. The new narrowband H$_2$ 2.12$μ$m, Br-$γ$ and K-continuum images trace the photoevaporative flow from the cloud and identify locations where UV-radiation from the surrounding massive stars excites molecular hydrogen to fluoresce. With a field of view of $\sim$ 1.5' $\times$ 2.9' and spatial resolution between 60 $-$ 110 mas, the new images show a spectacular level of detail over a large area, and presage what JWST should achieve. The Wall is convex in shape, with a large triangular-shaped extension near its apex. The interface near the apex consists of 3 $-$ 4 regularly-spaced ridges with projected spacings of $\sim$ 2000 AU, suggestive of a large-scale dynamically-important magnetic field. The northern edge of the Wall breaks into several swept-back fragments of width $\sim$ 1800 AU that resemble Kelvin-Helmholtz instabilities, and the southern part of the Wall also shows complex morphologies including a sinusoidal-like variation with a half-wavelength of 2500 AU. Though the dissociation front must increase the density along the surface of the Wall, it does not resolve into pillars that point back to the ionization sources, as could occur if the front triggered new stars to form. We discovered that MHO 1630, an H$_2$ outflow with no clear driving source in the northern portion of the Wall, consists of a series of bow shocks arrayed in a line.
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