We use the Point Process MAPping (PPMAP) algorithm to reanalyse the Herschel and SCUBA-2 observations of the L1688 and L1689 subregions of the Ophiuchus molecular cloud. PPMAP delivers maps with high resolution (here 14 arcsec, corresponding to ${\sim}0.01\, {\rm pc}$ at ${\sim}140\, {\rm pc}$), by using the observations at their native resolutions. PPMAP also delivers more accurate dust optical depths, by distinguishing dust of different types and at different temperatures. The filaments and pre-stellar cores almost all lie in regions with $N_{\rm H_2}\gtrsim 7\times 10^{21}\, {\rm cm}^{-2}$ (corresponding to AV ≳ 7). The dust temperature, T, tends to be correlated with the dust opacity index, β, with low T and low β concentrated in the interiors of filaments. The one exception to this tendency is a section of filament in L1688 that falls – in projection – between the two B stars: S1 and HD147889; here T and β are relatively high, and there is compelling evidence that feedback from these two stars has heated and compressed the filament. Filament fwhms are typically in the range $0.10$ to $0.15\, {\rm pc}$. Most filaments have line-densities in the range $25$ to $65\, {\rm M_{\odot }\, pc^{-1}}$. If their only support is thermal gas pressure, and the gas is at the canonical temperature of $10\, {\rm K}$, the filaments are highly supercritical. However, there is some evidence from ammonia observations that the gas is significantly warmer than this, and we cannot rule out the possibility of additional support from turbulence and/or magnetic fields. On the basis of their spatial distribution, we argue that most of the starless cores are likely to disperse (rather than evolving to become pre-stellar).

中文翻译：

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蛇夫座 L1688 和 L1689 丝状结构的 PPMAP 分析

我们使用点过程映射 (PPMAP) 算法重新分析蛇夫座分子云的 L1688 和 L1689 子区域的 Herschel 和 SCUBA-2 观测值。PPMAP 提供高分辨率的地图（这里 14 arcsec，对应于 ${\sim}0.01\，{\rm pc}$ at ${\sim}140\，{\rm pc}$），通过使用他们在本机分辨率。PPMAP 还通过区分不同类型和不同温度下的灰尘，提供更准确的灰尘光学深度。灯丝和前星核几乎都位于 $N_{\rm H_2}\gtrsim 7\times 10^{21}\, {\rm cm}^{-2}$ 的区域（对应于 AV ≳ 7） . 粉尘温度 T 倾向于与粉尘不透明度指数 β 相关，低 T 和低 β 集中在细丝内部。这种趋势的一个例外是 L1688 中的一段灯丝，在投影中位于两颗 B 星之间：S1 和 HD147889；这里 T 和 β 相对较高，有令人信服的证据表明来自这两颗恒星的反馈加热并压缩了灯丝。灯丝 fwhms 通常在 $0.10$ 到 $0.15\, {\rm pc}$ 的范围内。大多数灯丝的线密度在 $25$ 到 $65\, {\rm M_{\odot }\, pc^{-1}}$ 之间。如果它们的唯一支持是热气体压力，并且气体处于标准温度 $10\, {\rm K}$，则细丝是高度超临界的。然而，从氨的观测中有一些证据表明气体比这要暖得多，我们不能排除湍流和/或磁场提供额外支持的可能性。根据它们的空间分布，