蛇夫座L1688和L1689的消化结构的PPMAP分析
A PPMAP analysis of the filamentary structures in Ophiuchus L1688 and L1689
摘要：
本文利用PPMAP（Point Process MAPping）算法对蛇夫座分子云L1688和L1689亚区的\textit{Herschel}和SCUBA-2观测资料进行了再分析。PPMAP通过使用原始分辨率下的观测值来提供高分辨率地图（此处为$14''$，对应于$\sim 140\,{\rm pc}$下的$\sim 0.01\,{\rm pc}$）。PPMAP还通过区分不同类型和不同温度的灰尘，提供更准确的灰尘光学深度。纤维和星前核几乎都位于具有$N_{\rm H_2}\gtrsim 7\times 10^{21}\,{\rm cm}^{-2}$的区域（对应于$A_{_{\rm V}}\gtrsim 7$）。尘埃温度，$T$，往往与尘埃不透明度指数，PDMATHAMT，与低$T$和低PDMATHAMT往往集中在内部的细丝。这种趋势的一个例外是L1688中的一段暗条，在投影中落在两颗B星S1和HD 147889之间;这里的$T$和$β$相对较高，并且有令人信服的证据表明来自这两颗恒星的反馈已经加热和压缩了暗条。灯丝{ \sc fwhm}通常在$0.10\,{\rm pc}$至$0.15\,{\rm pc}$的范围内。大多数长丝的线密度在$25\,{\rm M_{_\odot}\,pc^{-1}}$至$65\,{\rm M_{_\odot}\,pc^{-1}}$的范围内。如果它们唯一的支持是热气体压力，并且气体处于$10\,{\rm K}$的正则温度，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，气体比这要热得多，我们不能排除来自湍流和/或磁场的额外支持的可能性。根据它们的空间分布，我们认为大多数无星核心可能会分散（而不是演变成星前）。
英文摘要：
We use the PPMAP (Point Process MAPping) algorithm to re-analyse the \textit{Herschel} and SCUBA-2 observations of the L1688 and L1689 sub-regions of the Ophiuchus molecular cloud. PPMAP delivers maps with high resolution (here $14''$, 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 prestellar cores almost all lie in regions with $N_{\rm H_2}\gtrsim 7\times 10^{21}\,{\rm cm}^{-2}$ (corresponding to $A_{_{\rm V}}\gtrsim 7$). The dust temperature, $T$, tends to be correlated with the dust opacity index, $β$, with low $T$ and low $β$ tend 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 {\sc fwhm}s are typically in the range $0.10\,{\rm pc}$ to $0.15\,{\rm pc}$. Most filaments have line densities in the range $25\,{\rm M_{_\odot}\,pc^{-1}}$ 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 prestellar).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
