DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. II. COMBINATIONS OF ULTRAVIOLET AND INFRARED TRACERS
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DOI：
10.1088/0004-637x/741/2/124
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发表时间：
2011-08
期刊：
影响因子：
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通讯作者：
C. Hao;R. Kennicutt;Benjamin D. Johnson;D. Calzetti;D. Dale;J. Moustakas
中科院分区：
文献类型：
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作者：
C. Hao;R. Kennicutt;Benjamin D. Johnson;D. Calzetti;D. Dale;J. Moustakas
我们提出了新的校准远紫外（FUV）衰减来自总红外FUV光度比（IRX）和FUV近紫外（NUV）的颜色。我们发现IRX校正的FUV光度与衰减校正的Hα光度（由Balmer衰减量测量）紧密线性相关，均方根散射为±0.09 dex。这些衰减校正的FUV与Hα光度的比值与演化合成模型的预测是一致的，假设星星形成速率超过1亿年，太阳金属丰度，以及Salpeter或Kroupa初始质量函数，质量下限和上限分别为0.1和100 M。IRX校正的FUV与Balmer校正的Hα光度比在我们的样本天体所覆盖的范围内没有显示出任何与其他星系性质相关的趋势。相比之下，FUV衰减来自FUV-NUV颜色（UV光谱斜率）显示更大的随机和系统的不确定性。当与Balmer校正的Hα光度或IRX校正的FUV光度相比时，颜色校正的FUV光度显示出2.5倍的均方根散射，以及作为光度和其他参数的函数的系统非线性偏差。25 μm和1.4GHz射电连续谱光度与观测到的FUV光度的线性组合也与Balmer校正的Hα光度有很好的相关。这些结果提供了有用的处方推导衰减校正星星形成率的基础上的线性组合的UV和IR或无线电光度，这是方便的表格形式。我们的校准与文献中的衰减校正和尘埃衰减规律的比较也。
We present new calibrations of far-ultraviolet (FUV) attenuation as derived from the total infrared to FUV luminosity ratio (IRX) and the FUV–near-UV(NUV) color. We find that the IRX-corrected FUV luminosities are tightly and linearly correlated with the attenuation-corrected Hα luminosities (as measured from the Balmer decrement), with an rms scatter of ±0.09 dex. The ratios of these attenuation-corrected FUV to Hα luminosities are consistent with evolutionary synthesis model predictions, assuming a constant star formation rate over 100 Myr, solar metallicity, and either a Salpeter or a Kroupa initial mass function with lower and upper mass limits of 0.1 and 100 M☉. The IRX-corrected FUV to Balmer-corrected Hα luminosity ratios do not show any trend with other galactic properties over the ranges covered by our sample objects. In contrast, FUV attenuation derived from the FUV–NUV color (UV spectral slope) show much larger random and systematic uncertainties. When compared to either Balmer-corrected Hα luminosities or IRX-corrected FUV luminosities the color-corrected FUV luminosities show ∼2.5 times larger rms scatter, and systematic nonlinear deviations as functions of luminosity and other parameters. Linear combinations of 25 μm and 1.4 GHz radio continuum luminosities with the observed FUV luminosities are also well correlated with the Balmer-corrected Hα luminosities. These results provide useful prescriptions for deriving attenuation-corrected star formation rates of galaxies based on linear combinations of UV and IR or radio luminosities, which are presented in convenient tabular form. Comparisons of our calibrations with attenuation corrections in the literature and with dust attenuation laws are also made.