论文标题
扩展的H $α$超过紧凑型远红外连续的尘土飞扬的金属 - 对灰尘分布和恒星形成率的见解
Extended H$α$ over compact far-infrared continuum in dusty submillimeter galaxies -- Insights into dust distributions and star-formation rates at $z\sim2$
论文作者
论文摘要
我们使用VLT上的ALMA和近红外（NIR）积分磁场光谱仪，包括Sinfoni和KMO，我们研究了H $α$和REST-FRAME FARFRAED（FIR）连续体的二维分布，在$ z \ sim2 $的六个亚略列表中。以类似的空间分辨率（$ \ sim $ 0.5“ fwhm; $ \ sim $ 4.5 kpc $ z = 2 $），我们发现，H $α$的半光度半径明显大于一半样品中的Fir连续性，而h $α$的平均值是中间因素，是$ 2.0 \ pm0的中间因素。 attenuation-corrected H$α$-based SFRs are systematically lower than the IR-based SFRs by at least a median factor of $3\pm1$, which cannot be explained by the difference in half-light radius alone. In addition, we find that in 40% of cases the total $V$-band attenuation ($A_V$) derived from energy balance modeling of the full ultraviolet(UV)-to-FIR spectral energy distributions (SEDs) is significantly higher than that derived from SED modeling using only the UV-to-NIR part of the SEDs, and the discrepancy appears to increase with increasing total infrared luminosity. Finally, considering all our findings along with the studies in the literature, we postulate that the dust distributions in SMGs, and possibly also in less IR luminous $z\sim2$ massive star-forming galaxies, can be decomposed into three main components;较老的恒星种群加热的弥漫性尘埃，更遮挡和延伸的年轻恒星形成的HII区域以及较低的填充因子较低但占主导地位的较重的中央区域，在这种红外发光度中，大多数衰减无法通过UV-to-to-to-to-nir发射来探测。
Using data from ALMA and near-infrared (NIR) integral field spectrographs including both SINFONI and KMOS on the VLT, we investigate the two-dimensional distributions of H$α$ and rest-frame far-infrared (FIR) continuum in six submillimeter galaxies at $z\sim2$. At a similar spatial resolution ($\sim$0.5" FWHM; $\sim$4.5 kpc at $z=2$), we find that the half-light radius of H$α$ is significantly larger than that of the FIR continuum in half of the sample, and on average H$α$ is a median factor of $2.0\pm0.4$ larger. Having explored various ways to correct for the attenuation, we find that the attenuation-corrected H$α$-based SFRs are systematically lower than the IR-based SFRs by at least a median factor of $3\pm1$, which cannot be explained by the difference in half-light radius alone. In addition, we find that in 40% of cases the total $V$-band attenuation ($A_V$) derived from energy balance modeling of the full ultraviolet(UV)-to-FIR spectral energy distributions (SEDs) is significantly higher than that derived from SED modeling using only the UV-to-NIR part of the SEDs, and the discrepancy appears to increase with increasing total infrared luminosity. Finally, considering all our findings along with the studies in the literature, we postulate that the dust distributions in SMGs, and possibly also in less IR luminous $z\sim2$ massive star-forming galaxies, can be decomposed into three main components; the diffuse dust heated by older stellar populations, the more obscured and extended young star-forming HII regions, and the heavily obscured central regions that have a low filling factor but dominate the infrared luminosity in which the majority of attenuation cannot be probed via UV-to-NIR emissions.
