论文标题
$ 3 <z <5 $：同时研究AGN和星系的总休息时间UV光度函数，$ -28 <m _ {\ rm UV} <-16 $
The total rest-frame UV luminosity function from $3 < z < 5$: A simultaneous study of AGN and galaxies from $-28<M_{\rm UV}<-16$
论文作者
论文摘要
我们介绍了RedShifts $ z = 3 $，$ z = 4 $和$ z = 5 $的静电帧紫外线光度功能的测量值，分别使用96894、38655和7571来源来映射AGN和Galaxy-Palaxy-Paraxy-Paraxy-Araxy-Araky-Paraxy-Araky-procted Ultraviolet在Reiver of Repoch epoch epoch epoch epoch epoch epoch epoch epoch之后的过渡。使用全面的光度红移方法选择来源，使用HSC和Vista涵盖的$ 10 $ deg $^2 $的深层遗传遗产领域。模板拟合的使用涵盖了$ 0.3 \ text { - }2.4μ$ M的波长范围$ 80 \ text { - } 90 $的完整性，比古典颜色彩色切割方法高得多。测得的LF包括$ -26 <m _ {\ rm UV} <-19.25 $。使用其他研究的互补结果，将其进一步扩展到$ -28.5 <m _ {\ rm UV} <-16 $，从而同时拟合了合并的AGN和Galaxy LF。 We find that there are fewer UV luminous galaxies ($M_{\rm UV}<-22$) at $z\sim3$ than $z\sim4$, indicative of an onset of widespread quenching alongside dust obscuration, and that the evolution of the AGN LF is very rapid, with their number density rising by around 2 orders of magnitude from $3<z<6$.仍然很难确定是否比Schechter函数优选双重功率定律（DPL）功能形式来描述Galaxy UV LF。从我们的UV LFS估算氢电离光子预算，我们发现AGN可以为但不能仅维持宇宙的电离为$ z = 3-5 $。但是，迅速发展的AGN LF在EOR内部强烈不利。
We present measurements of the rest-frame ultraviolet luminosity function at redshifts $z=3$, $z=4$ and $z=5$, using 96894, 38655 and 7571 sources respectively to map the transition between AGN and galaxy-dominated ultraviolet emission shortly after the epoch of reionization. Sources are selected using a comprehensive photometric redshift approach, using $10$deg$^2$ of deep extragalactic legacy fields covered by both HSC and VISTA. The use of template fitting spanning a wavelength range of $0.3\text{--}2.4μ$m achieves $80\text{--}90$ per cent completeness, much higher than classical colour-colour cut methodology. The measured LF encompasses $-26<M_{\rm UV}<-19.25$. This is further extended to $-28.5<M_{\rm UV}<-16$ using complementary results from other studies, allowing for the simultaneous fitting of the combined AGN and galaxy LF. We find that there are fewer UV luminous galaxies ($M_{\rm UV}<-22$) at $z\sim3$ than $z\sim4$, indicative of an onset of widespread quenching alongside dust obscuration, and that the evolution of the AGN LF is very rapid, with their number density rising by around 2 orders of magnitude from $3<z<6$. It remains difficult to determine if a double power law (DPL) functional form is preferred over the Schechter function to describe the galaxy UV LF. Estimating the Hydrogen ionizing photon budget from our UV LFs, we find that AGN can contribute to, but cannot solely maintain, the reionization of the Universe at $z=3-5$. However, the rapidly evolving AGN LF strongly disfavours a significant contribution within the EoR.
