高分辨率三维辐射转移建模III。DustPedia棒星系
High-resolution, 3D radiative transfer modelling III. The DustPedia barred galaxies
摘要：
背景：本机宇宙中晚型星系中的尘埃负责吸收恒星发射的大约三分之一的能量。通常认为，尘埃加热主要是由于吸收了最年轻（<= 1亿年）恒星发射的紫外线和可见光子。因此，尘埃在远红外波段的热再发射通常与星系的恒星形成活动有关。然而，一些研究认为，年龄更大的恒星对尘埃加热的贡献可能更重要。辐射传输（RT）模拟的进展终于使我们能够实际量化恒星辐射场对弥漫尘埃的加热机制。目标：作为DustPedia项目的主要目标之一，我们已经为附近的星系构建了详细的3D恒星和尘埃RT模型。我们分析了四个正面棒星系：NGC 1365，M83，M95和M100中不同恒星星族对尘埃加热的贡献。我们的目标是量化的分数直接相关的年轻恒星，在全球范围内和局部尺度上，并评估酒吧的加热分数的影响。结果如下：我们推导出每个星系的全球衰减规律，并确认高sSFR的星系有较浅的衰减曲线和较弱的UV颠簸。平均而言，36.5%的辐射热光度被尘埃吸收。我们报告了一个明确的效果的酒吧结构上的尘埃加热部分的径向配置文件的年轻恒星，和尘埃温度。我们发现，年轻的恒星是尘埃加热的主要贡献者，在整个星系中，平均约59%的光度用于此目的。尘埃加热的比例在棒区下降到~53%，在鼓包区下降到~38%，在鼓包区，老恒星是尘埃加热的主要贡献者。我们还发现了一个很强的联系之间的加热分数的年轻恒星和sSFR。
英文摘要：
Context: Dust in late-type galaxies in the local Universe is responsible for absorbing approximately one third of the energy emitted by stars. It is often assumed that dust heating is mainly attributable to the absorption of UV and optical photons emitted by the youngest (<= 100 Myr) stars. Consequently, thermal re-emission by dust at FIR wavelengths is often linked to the star-formation activity of a galaxy. However, several studies argue that the contribution to dust heating by much older stars might be more significant. Advances in radiation transfer (RT) simulations finally allow us to actually quantify the heating mechanisms of diffuse dust by the stellar radiation field. Aims: As one of the main goals in the DustPedia project, we have constructed detailed 3D stellar and dust RT models for nearby galaxies. We analyse the contribution of the different stellar populations to the dust heating in four face-on barred galaxies: NGC1365, M83, M95, and M100. We aim to quantify the fraction directly related to young stars, both globally and on local scales, and to assess the influence of the bar on the heating fraction. Results: We derive global attenuation laws for each galaxy and confirm that galaxies of high sSFR have shallower attenuation curves and weaker UV bumps. On average, 36.5% of the bolometric luminosity is absorbed by dust. We report a clear effect of the bar structure on the radial profiles of the dust-heating fraction by the young stars, and the dust temperature. We find that the young stars are the main contributors to the dust heating, donating, on average ~59% of their luminosity to this purpose throughout the galaxy. This dust-heating fraction drops to ~53% in the bar region and ~38% in the bulge region where the old stars are the dominant contributors to the dust heating. We also find a strong link between the heating fraction by the young stars and the sSFR.
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