标题： 用于确定星暴星系尘埃消光的流量比方法 显示英文标题

标题： The Flux Ratio Method for Determining the Dust Attenuation of Starburst Galaxies

摘要： 恒星爆发星系中尘埃的存在使研究它们的恒星群体变得复杂，因为尘埃的影响与星系恒星年龄和金属量变化所关联的影响相似。 如果结合紫外/光学/近红外观测与远红外观测，这种退化对于恒星爆发星系是可以克服的。 我们提出了计算特定波长尘埃消光的流量比方法的校准，即基于 F(IR)/F(\lambda ) 流量比的 Att(\lambda ) 计算。 我们的校准基于来自 PEGASE 恒星演化综合模型的谱能量分布（SED）以及从我们的蒙特卡洛辐射传输模型计算出的尘埃效应（吸收和散射）。 我们测试了这种方法预测的巴耳末发射线消光，与使用无线电观测计算出的消光进行了比较，发现一致性良好。 使用流量比方法计算了几颗恒星爆发星系的紫外消光曲线，这些结果与过去的工作相比令人满意。 Att(\lambda ) 和 F(IR)/F(\lambda ) 之间的关系几乎完全独立于假设的尘埃属性（颗粒类型、分布和团块性）。 对于紫外波段，该关系也独立于假设的恒星属性（年龄、金属量等），除了非常老的爆发群体的情况。 然而，在更长波长下，该关系依赖于假设的恒星属性。 显示英文摘要

摘要： The presence of dust in starburst galaxies complicates the study of their stellar populations as the dust's effects are similar to those associated with changes in the galaxies' stellar age and metallicity. This degeneracy can be overcome for starburst galaxies if UV/optical/near-infrared observations are combined with far-infrared observations. We present the calibration of the flux ratio method for calculating the dust attenuation at a particular wavelength, Att(\lambda), based on the measurement of F(IR)/F(\lambda) flux ratio. Our calibration is based on spectral energy distributions (SEDs) from the PEGASE stellar evolutionary synthesis model and the effects of dust (absorption and scattering) as calculated from our Monte Carlo radiative transfer model. We tested the attenuations predicted from this method for the Balmer emission lines of a sample starburst galaxies against those calculated using radio observations and found good agreement. The UV attenuation curves for a handful of starburst galaxies were calculated using the flux ratio method, and they compare favorably with past work. The relationship between Att(\lambda) and F(IR)/F(\lambda) is almost completely independent of the assumed dust properties (grain type, distribution, and clumpiness). For the UV, the relationship is also independent of the assumed stellar properties (age, metallicity, etc) accept for the case of very old burst populations. However at longer wavelengths, the relationship is dependent on the assumed stellar properties.