Dust in Starburst Galaxies
Dust in Starburst Galaxies
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星爆星系中的尘埃
DOI：
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发表时间：
1997
期刊：
影响因子：
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通讯作者：
A. Witt
中科院分区：
文献类型：
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作者：
K. Gordon;D. Calzetti;A. Witt
为了研究星暴尘埃的性质，我们构建了一个星暴星系中恒星和尘埃的模型，并将其应用于30个观测到的星暴光谱能量分布（SED）。星暴模型是将两个恒星演化合成模型与一个描述恒星光子通过尘埃辐射传输的模型相结合而建立的。利用恒星演化合成模型计算了年龄在1 × 106 ~ 15 × 109 yr之间的恒星群体的无尘SED。利用MonteCarlo辐射传输模型，计算了平均银河系（MW）和小麦哲伦云（SMC）尘埃、两种不同的星星/尘埃几何结构以及局部均匀或团状尘埃的辐射效应。使用颜色-颜色图，星爆模型被用来解释30星爆的行为与孔径匹配的紫外和光学SED（和IR的30）从以前的研究。从色-色图中可以明显看出，星爆中的尘埃有一个消光曲线，缺少2175 μ m的隆起，就像SMC曲线一样，还有一个陡峭的远紫外线上升，介于MW和SMC曲线之间。星星/尘埃几何学能够解释30个星爆在不同颜色图中的分布，它有一个内部的无尘恒星球，周围是一个外部的无星尘埃壳。当结合其他工作从猎户座地区和30多尔地区的大麦哲伦星云的文献，这项工作意味着一个趋势，尘埃性质与星星形成强度。
To investigate the nature of starburst dust, we constructed a model of the stars and dust in starburst galaxies and applied it to 30 observed starburst spectral energy distributions (SEDs). The starburst model was constructed by combining two stellar evolutionary synthesis models with a model describing the radiative transfer of stellar photons through dust. The stellar evolutionary synthesis models were used to compute the dust-free SEDs for stellar populations with ages between 1 × 106 and 15 × 109 yr. Using a Monte Carlo radiative transfer model, the effects of dust were computed for average Milky Way (MW) and Small Magellanic Cloud (SMC) dust, two different star/dust geometries, and locally homogeneous or clumpy dust. Using color-color plots, the starburst model was used to interpret the behavior of 30 starbursts with aperture-matched UV and optical SEDs (and IR for 19 of the 30) from previous studies. From the color-color plots, it was evident that the dust in starbursts has an extinction curve lacking a 2175 Å bump, like the SMC curve, and a steep far-UV rise, intermediate between the MW and SMC curves. The star/dust geometry that is able to explain the distribution of the 30 starbursts in various color-color plots has an inner dust-free sphere of stars surrounded by an outer star-free shell of clumpy dust. When combined with other work from the literature on the Orion region and the 30 Dor region of the Large Magellanic Cloud, this work implies a trend in dust properties with star formation intensity.