模拟发现我们对尘埃遮蔽恒星形成的核算可能是不完整的
Simulations Find Our Accounting of Dust-Obscured Star Formation May Be Incomplete
摘要：
在宇宙正午，恒星形成率密度峰值的大部分被尘埃所掩盖。我们评估尘埃遮蔽恒星形成作用的准确程度受到我们经验方法中固有偏差的影响--无论是那些依赖于直接尘埃发射的方法还是那些依赖于星光推断尘埃衰减的方法。我们使用流体动力学模拟库与辐射转移，以探讨这些偏见。我们发现，对于红外发光的星系，在快速淬火系统（如合并后）的标准光度SFR的关系可以强烈高估真正的SFR。我们建议使用$L_{IR}/L_{1.6}$颜色来帮助识别此类系统并提供更准确的SFR。相反，我们发现诊断UVJ图错误地识别了一个尘埃恒星形成星系的子集。这是由于有效衰减曲线的可变性，包括在光学到近红外区域比卡尔泽蒂星爆定律更灰色。这与最近在宇宙正午观测到的红外选择星系相一致。我们的研究结果支持这样的观点，即我们需要一个全色的方法，从休息帧紫外线通过红外和SED建模，包括现实的SFH，并允许可变衰减曲线，如果我们想充分考虑到尘埃遮蔽恒星形成的最大星系建设的时代。
英文摘要：
The bulk of the star-formation rate density peak at cosmic noon was obscured by dust. How accurately we can assess the role of dust obscured star-formation is affected by inherent biases in our empirical methods -- both those that rely on direct dust emission and those that rely on the inferred dust attenuation of starlight. We use a library of hydrodynamic simulations with radiative transfer to explore these biases. We find that for IR luminous galaxies that are in rapidly quenching systems (e.g. post-coalescence) standard luminosity-to-SFR relations can strongly overestimate the true SFRs. We propose using the $L_{IR}/L_{1.6}$ color to both help identify such systems and provide more accurate SFRs. Conversely, we find that the diagnostic UVJ plot misidentifies a subset of dusty star-forming galaxies. This is due to variability in the effective attenuation curves including being much grayer in the optical-to-near-IR regime than the Calzetti starburst law. This is in agreement with recent observations of IR-selected galaxies at cosmic noon. Our results support the view that we need a panchromatic approach from the rest-frame UV through the IR and SED modeling that includes realistic SFHs and allows for variable attenuation curves if we want to fully account for dust obscured star-formation across the epochs of greatest galaxy build-up.
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