Probing star formation and ISM properties using galaxy disk inclination
Probing star formation and ISM properties using galaxy disk inclination
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DOI：
10.1051/0004-6361/201732255
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发表时间：
2018-01
影响因子：
6.5
通讯作者：
S. Leslie;M. Sargent;E. Schinnerer;B. Groves;A. V. D. Wel;G. Zamorani;Y. Fudamoto;P. Lang;
中科院分区：
文献类型：
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作者：
S. Leslie;M. Sargent;E. Schinnerer;B. Groves;A. V. D. Wel;G. Zamorani;Y. Fudamoto;P. Lang;
在先前的工作中，已经发现中等红移（z ~ 0.7）的盘星系在静止坐标系B带表面亮度中比它们的本地对应物显示出更多的光学厚度行为，这表明在过去的~6 Gyr中尘埃性质的演化。我们比较了在不同波长（紫外线（UV），中红外线（MIR），远红外线（FIR），和无线电）的两个良好匹配的样本的盘占主导地位的星系：本地斯隆数字巡天（SDSS）选择的样本在z ~ 0.07和磁盘的样本在z ~ 0.7从宇宙演化调查（COSMOS）的正面和侧面的恒星形成星系的光度。我们已经推导出校正因子来解释用于样本选择的参数的倾斜依赖性。我们发现，典型的星系是透明的MIR波长在两个红移，和FIR和无线电发射也是透明的预期。然而，在这些波长下降低的灵敏度限制了我们的分析;我们不能排除FIR或无线电中的不透明性。紫外线衰减在z ~ 0和z ~ 0.7之间增加，其中z ~ 0.7样品是衰减的~3.4倍。在z ~ 0.7处较大的紫外线衰减可以解释为新生恒星形成区域周围有更多的尘埃。SFRUV与1 − cos（i）趋势的归一化拟合演化（解释为团块分数）与z < 1的星系的分子气体分数/尘埃分数演化之间有很好的一致性。
Disk galaxies at intermediate redshift (z ~ 0.7) have been found in previous work to display more optically thick behaviour than their local counterparts in the rest-frame B-band surface brightness, suggesting an evolution in dust properties over the past ~6 Gyr. We compare the measured luminosities of face-on and edge-on star-forming galaxies at different wavelengths (Ultraviolet (UV), mid-infrared (MIR), far-infrared (FIR), and radio) for two well-matched samples of disk-dominated galaxies: a local Sloan Digital Sky Survey (SDSS)-selected sample at z ~ 0.07 and a sample of disks at z ~ 0.7 drawn from Cosmic Evolution Survey (COSMOS). We have derived correction factors to account for the inclination dependence of the parameters used for sample selection. We find that typical galaxies are transparent at MIR wavelengths at both redshifts, and that the FIR and radio emission is also transparent as expected. However, reduced sensitivity at these wavelengths limits our analysis; we cannot rule out opacity in the FIR or radio. Ultra-violet attenuation has increased between z ~ 0 and z ~ 0.7, with the z ~ 0.7 sample being a factor of ~3.4 more attenuated. The larger UV attenuation at z ~ 0.7 can be explained by more clumpy dust around nascent star-forming regions. There is good agreement between the fitted evolution of the normalisation of the SFRUV versus 1 − cos(i) trend (interpreted as the clumpiness fraction) and the molecular gas fraction/dust fraction evolution of galaxies found out to z < 1.