论文标题
JWST预览：H $ _2 $，BR- $γ$和Carina's Western Wall的K-Continuum的自适应 - 播放图像
A JWST Preview: Adaptive-Optics Images of H$_2$, Br-$γ$, and K-continuum in Carina's Western Wall
论文作者
论文摘要
我们介绍了Carina's Western Wall（G287.38-0.62）的第一个宽场近红外自适应光学图像，这是在大型恒星形成区域中已知的最亮，定义最明确的辐照界面之一。新的窄带h $ _2 $ 2.12 $ $ m，br- $γ$和k-continuum图像从云中追踪光蒸发流，并确定来自周围巨大恒星的紫外线辐射激发分子氢的位置。凭借$ \ sim $ 1.5' $ \ times $ 2.9'的视野和60 $ - $ 110 MAS之间的空间分辨率，新图像在大面积上显示出壮观的细节，并预示JWST应该实现的目标。墙的形状为凸，其顶端附近有一个大三角形延伸。顶点附近的界面由3 $ -4 $ 4定期间隔的脊组成，预计的间距为$ \ sim $ 2000 au，暗示着一个大规模的动态磁场。墙壁的北边缘分解成宽度$ \ sim $ 1800 au的几个横扫后背碎片，类似于开尔文 - 赫尔姆霍尔茨的不稳定，墙壁的南部还显示了复杂的形态，包括正弦状的变化，半波长为2500 au。尽管解离界必须增加沿壁表面的密度，但它不能分解为柱子，将其指向电离源，如果前面触发新恒星形成，可能会发生这种情况。我们发现，MHO 1630是墙壁北部没有清晰的驾驶源的H $ _2 $流出，由一系列的弓形冲击组成。
We present the first wide-field near-infrared adaptive optics images of Carina's Western Wall (G287.38-0.62), one of the brightest and most well-defined irradiated interfaces known in a region of massive star formation. The new narrowband H$_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.
