从通量到尘埃质量：颗粒温度分布对超新星遗迹中冷尘埃质量的估计有影响吗？
From flux to dust mass: Does the grain-temperature distribution matter for estimates of cold dust masses in supernova remnants?
摘要：
从红外到亚毫米观测估计的尘埃量在很大程度上取决于对不同颗粒大小、成分和光学性质的假设。在这里，我们使用一个简单的模型的热辐射从冷硅酸盐/碳尘埃在一个范围内的尘埃颗粒的温度和适合的光谱能量分布（SED）的蟹状星云作为一个测试。与最近公布的数值相比，这可以将蟹状星云的尘埃质量降低约50%，将天文硅酸盐和无定形碳颗粒的尘埃质量降低30- 40（分别为0.25 M_sun-> 0.12 M_sun和0.12 M_sun-> 0.072 M_sun），但是根据对最冷颗粒的大小/温度的假设，隐含的尘埃质量也可以增加几乎六倍（0.25M_sun -> 1.14M_sun和0.12M_sun -> 0.71M_sun）。然而，由于预期的金属预算，后一个值显然是不现实的。此外，我们通过一个简单的数值实验表明，如果一个冷尘埃成分确实有一个颗粒温度分布，这几乎是不可避免的，两个温度的配合将产生一个不正确的尘埃质量估计。但我们得出结论，晶粒温度并不比通常约束不良的发射率（即，物质性质），尽管显然需要改进尘埃排放模型。与推导尘埃质量有关的最大的复杂性仍然来自尘埃成分的不确定性。
英文摘要：
The amount of dust estimated from infrared to sub-millimetre (submm) observations strongly depends on assumptions of different grain sizes, compositions and optical properties. Here we use a simple model of thermal emission from cold silicate/carbon dust at a range of dust grain temperatures and fit the spectral energy distribution (SED) of the Crab Nebula as a test. This can lower the derived dust mass for the Crab by ~50% and 30-40% for astronomical silicates and amorphous carbon grains compared to recently published values (0.25M_sun -> 0.12M_sun and 0.12M_sun -> 0.072M_sun, respectively), but the implied dust mass can also increase by as much as almost a factor of six (0.25M_sun -> 1.14M_sun and 0.12M_sun -> 0.71M_sun) depending on assumptions regarding the sizes/temperatures of the coldest grains. The latter values are clearly unrealistic due to the expected metal budget, though. Furthermore, we show by a simple numerical experiment that if a cold-dust component does have a grain-temperature distribution, it is almost unavoidable that a two-temperature fit will yield an incorrect dust mass estimate. But we conclude that grain temperatures is not a greater uncertainty than the often poorly constrained emissivities (i.e., material properties) of cosmic dust, although there is clearly a need for improved dust emission models. The greatest complication associated with deriving dust masses still arises in the uncertainty in the dust composition.
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