草帽星系中恒星和尘埃的全色辐射转移模拟
Panchromatic radiative transfer modeling of stars and dust in the Sombrero galaxy
摘要：
本文详细研究了草帽星系M104的尘埃能量平衡。从完整的辐射转移分析，包括散射、吸收和热再发射，我们建立了模型，可以再现在光学/近红外波段的图像，观测到的恒星SED和短轴消光轮廓在V和R_C波段。一个标准模型，只包含一个旧的恒星星族加热尘埃，低估了观测到的尘埃辐射在红外波长的一个因素~ 3。补充这一基本模型与年轻的恒星组成部分低恒星形成活动的内盘（SFR ~ 0.21 Msun/yr）和尘埃环（SFR ~ 0.05 Msun/yr），我们能够解决的差异，在尘埃的能量预算的草帽星系在波长短向100 \mum。为了解释超过100 \mum的FIR/submm发射的增加，我们提出了一个额外的尘埃成分分布在静止的团块。这个具有团簇状尘埃结构的模型预测，总尘埃含量的四分之三（约2.8 x 10^7 Msun）存在于致密的尘埃云中，没有相关的嵌入源。虽然高分辨率光学数据支持草帽星系中的cluerous尘埃结构的假设，但我们不能排除具有较高尘埃发射率的尘埃颗粒占亚毫米波长能量预算差异的一部分的可能性。
英文摘要：
We present a detailed study of the dust energy balance in the Sombrero galaxy M104. From a full radiative transfer analysis, including scattering, absorption and thermal re-emission, we construct models that can reproduce images at optical/near-infrared wavelengths, the observed stellar SED and the minor axis extinction profiles in the V and R_C band. A standard model, that contains only an old stellar population to heat the dust, underestimates the observations of dust emission at infrared wavelengths by a factor of ~ 3. Supplementing this basic model with a young stellar component of low star formation activity in both the inner disk (SFR ~ 0.21 Msun/yr) and dust ring (SFR ~ 0.05 Msun/yr), we are capable of solving the discrepancy in the dust energy budget of the Sombrero galaxy at wavelengths shortwards of 100 \mum. To account for the increased FIR/submm emission beyond 100 \mum, we propose a additional dust component distributed in quiescent clumps. This model with a clumpy dust structure predicts three-quarters of the total dust content (~ 2.8 x 10^7 Msun) to reside in compact dust clouds with no associated embedded sources. Although the assumption of a clumpy dust structure in the Sombrero galaxy is supported by high-resolution optical data, we cannot rule out the possibility that dust grains with a higher dust emissivity account for part of the discrepancy in the energy budget at submm wavelengths.
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