论文标题
红外光度功能的明亮末端和丰富的红外星系的丰度
The bright end of the infrared luminosity functions and the abundance of hyperluminous infrared galaxies
论文作者
论文摘要
我们提供了红外（IR）光度函数（LFS）光亮末端的最准确估计，并且由于高灵敏度，角度分辨率，较大的lum lum comport and probers and probist and probist and probist and probers contercition therects therects comports y IR亮度> 10^13 l_solties> 10^13 l_ solarties的丰度（Hlirgs）。我们在靴子（8.63 deg^2），洛克曼孔（10.28 ver^2）和Elais-N1（6.74 ver^2）的靴子中交叉匹配Herschel源和Lofar源，分别为RMS敏感性约为32、22和20 MJY。我们将匹配的样本分为独特的和多个类别。对于多个比赛，我们使用Lofar位置和150 MHz通量密度作为先验来融合了Herschel通量。我们执行光谱能分布（SED）拟合，并结合多波长对应物的识别和光度红移估计值，以得出IR亮度。 LOFAR数据的深度使我们能够根据250微米通量密度（分别为45、40和35 MJY，Lockman Hole和Elais-N1中的250微米通量密度（分别为45、40和35 MJY）识别明亮的赫歇尔源样品的高度完整（约92％的完整性）样本。大多数明亮的Herschel资源都属于独特的类别（即单个Lofar对应物）。对于多次匹配，无线电发射与FAR-IR发射之间存在出色的对应关系。我们在IR LFS中发现了一个很好的协议，以前的研究对Z大约6左右，该研究使用了De-herschel数据。迄今为止，我们的样本给出了最强，最清洁的迹象，即Hlirgs的人口的表面密度约为5至18 / deg^2（由于应用的通量极限和宇宙差异的组合而变化），不确定性的不确定性为2。在比较中，Galform半无分析模型在hlirgs的繁殖范围内显着差。
We provide the most accurate estimate yet of the bright end of the infrared (IR) luminosity functions (LFs) and the abundance of hyperluminous IR galaxies (HLIRGs) with IR luminosities > 10^13 L_solar, thanks to the combination of the high sensitivity, angular resolution, and large area of the LOFAR Deep Fields, which probes an unprecedented dynamic range of luminosity and volume. We cross-match Herschel sources and LOFAR sources in Bootes (8.63 deg^2), Lockman Hole (10.28 deg^2), and ELAIS-N1 (6.74 deg^2) with rms sensitivities of around 32, 22, and 20 mJy per beam, respectively. We divide the matched samples into unique and multiple categories. For the multiple matches, we de-blend the Herschel fluxes using the LOFAR positions and the 150-MHz flux densities as priors. We perform spectral energy distribution (SED) fitting, combined with multi-wavelength counterpart identifications and photometric redshift estimates, to derive IR luminosities. The depth of the LOFAR data allows us to identify highly complete (around 92% completeness) samples of bright Herschel sources with a simple selection based on the 250 micron flux density (45, 40, and 35 mJy in Bootes, Lockman Hole, and ELAIS-N1, respectively). Most of the bright Herschel sources fall into the unique category (i.e. a single LOFAR counterpart). For the multiple matches, there is excellent correspondence between the radio emission and the far-IR emission. We find a good agreement in the IR LFs with a previous study out to z around 6 which used de-blended Herschel data. Our sample gives the strongest and cleanest indication to date that the population of HLIRGs has surface densities of around 5 to 18 / deg^2 (with variations due to a combination of the applied flux limit and cosmic variance) and an uncertainty of a factor of 2. In comparison, the GALFORM semi-analytic model significantly under-predicts the abundance of HLIRGs.
