SCUSS u-BAND EMISSION AS A STAR-FORMATION-RATE INDICATOR
SCUSS u-BAND EMISSION AS A STAR-FORMATION-RATE INDICATOR
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讨论 u 波段发射作为恒星形成速率指标
DOI：
10.3847/1538-4357/835/1/70
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发表时间：
2017
影响因子：
4.9
通讯作者：
Zou Hu
中科院分区：
文献类型：
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作者：
Zhou Zhimin;Zhou Xu;Wu Hong;Fan Xiao-Hui;Fan Zhou;Jiang Zhao-Ji;Jing Yi-Peng;Li Cheng;Lesser Michael;Jiang Lin-Hua;Ma Jun;Nie Jun-Dan;Shen Shi-Yin;Wang Jia-Li;Wu Zhen-Yu;Zhang Tian-Meng;Zou Hu
我们根据南银河盖 u 波段巡天 (SCUSS) 的数据提出并分析了使用光学 u 波段光度来估计星系恒星形成率 (SFR) 的可能性，该数据提供了覆盖南银河盖约 5000 deg2 的深度 u 波段光度测量。基于 BPT 图选择的两个正常恒星形成星系样本，我们将 SCUSS 数据与斯隆数字巡天和广域红外巡天探测器 (WISE) 相结合，探索 u 波段、Hα 和红外光度之间的相关性。衰减校正的 u 波段光度与巴尔默衰减校正的 Hα 光度紧密相关，均方根散射约为 0.17 dex。 IR校正的u光度是根据u波段光度的衰减与WISE 12（或22）μm光度之间的相关性得出的，然后用巴尔默校正的Hα光度进行校准。这些校准的系统残差根据我们样本对象覆盖范围内的物理特性进行测试。我们发现最佳拟合的非线性关系比线性关系更好，建议应用于 SFR 的测量。系统偏差主要来自老恒星族的污染和尘埃消光的影响；因此，在未来的工作中需要进行更详细的分析。
We present and analyze the possibility of using optical u-band luminosities to estimate star-formation rates (SFRs) of galaxies based on the data from the South Galactic Cap u band Sky Survey (SCUSS), which provides a deep u-band photometric survey covering about 5000 deg2 of the South Galactic Cap. Based on two samples of normal star-forming galaxies selected by the BPT diagram, we explore the correlations between u-band, Hα, and IR luminosities by combing SCUSS data with the Sloan Digital Sky Survey and Wide-field Infrared Survey Explorer (WISE). The attenuation-corrected u-band luminosities are tightly correlated with the Balmer decrement-corrected Hα luminosities with an rms scatter of ∼0.17 dex. The IR-corrected u luminosities are derived based on the correlations between the attenuation of u-band luminosities and WISE 12 (or 22) μm luminosities, and then calibrated with the Balmer-corrected Hα luminosities. The systematic residuals of these calibrations are tested against the physical properties over the ranges covered by our sample objects. We find that the best-fitting nonlinear relations are better than the linear ones and recommended to be applied in the measurement of SFRs. The systematic deviations mainly come from the pollution of old stellar population and the effect of dust extinction; therefore, a more detailed analysis is needed in future work.