论文标题
Muse和Alma看到的BR1202-0725系统的电离和凉气含量
The Ionised- and Cool-Gas Content of The BR1202-0725 System as seen by MUSE and ALMA
论文作者
论文摘要
我们介绍了Z〜4.7的气体丰富的主要合并BR1202-0725的观察，该观察构成了早期宇宙中最受欢迎的田野之一。我们将这些数据与现有的ALMA观察结合使用来比较和对比该系统的空间解决的电离电离和酷气含量，该系统容纳了一个Quasar（QSO），一个QUASAR（QSO），一个子麦格尔银河系（SMG），一个次数的光学伴侣（“ lae1”，“ lae2”），以及其他伴侣，与其他伴侣一起发现了nord norciien are n pre n and arciien arciien are n of a n ree n ree n'' QSO。我们发现QSO BR1202-0725表现出大型$α$ halo，覆盖$ \ of55 $ pkpc onsky onsky on Surface Brightness sb $ \ geq $ \ geq $ 17 erg/s/s/cm $^2 $/cm $^2 $/arcsec $^2 $。相比之下，具有类似远红外光度和星形形成率（SFR）的SMG并未表现出如此$α$ halo。 QSO的光环表现出高速宽度（$ \ sim1000 $ km/s），但气体运动在某种程度上是在运动学上与先前观察到的[CII]桥之间的QSO和SMG之间的相结合。我们注意到，文献中称为LAE2的对象没有显示$α$排放的局部峰值，而是它的轮廓与成为QSO扩展的LY $α$ HALO的一部分更加一致。 LAE3的性质是高红移LAE的典型特性；我们测量f $ _ {\ rm {lyα}} $（lae3）= $ 0.24 \ $ 0.03e-16 erg/s/s/cm $ $^2 $，对应于sfr $ _ {\ rm {lyα}} \ y.5 $ 5.0 $ 5.5 $ \ $ 0.5 m $ \ $ 0.5 m $ 0.5 m $ $ {_ y/y/速度宽度为$ΔV$（LAE3）$ \约400 $ km/s，等效宽度ew $ _0 $（ly $ a $α_ {\，5σ}}^{\，lim}）\ geq 34.05 $ $ $ \\ a $ a $，与恒星形成$ $ $ em em em em em emsision a $一致。我们还注意到至少三个对象的光谱中的$ \ sim -400 $ km/s的连贯吸收功能； QSO，LAE1和“ LAE2”可能意味着存在至少$ 24 $ PKPC的中性气壳的存在。
We present MUSE observations of the gas-rich major-merger BR1202-0725 at z~4.7, which constitutes one of the most overdense fields known in the early Universe. We utilise these data in conjunction with existing ALMA observations to compare and contrast the spatially resolved ionised- and cool-gas content of this system which hosts a quasar (QSO), a sub-millimeter galaxy (SMG), the two known optical companions ("LAE1", "LAE2"), and an additional companion discovered in this work "LAE3" just 5 arcsec to the North of the QSO. We find that QSO BR1202-0725 exhibits a large Ly$α$ halo, covering $\approx55$ pkpc on-sky at surface brightness levels of SB$\geq$1E-17 erg/s/cm$^2$/arcsec$^2$. In contrast, the SMG, of similar far-infrared luminosity and star formation rate (SFR), does not exhibit such a Ly$α$ halo. The QSO's halo exhibits high velocity widths ($\sim1000$ km/s) but the gas motion is to some extent kinematically coupled with the previously observed [CII] bridge between the QSO and the SMG. We note that the object known in the literature as LAE2 shows no local peak of Ly$α$ emission, rather, its profile is more consistent with being part of the QSO's extended Ly$α$ halo. The properties of LAE3 are typical of high-redshift LAEs; we measure F$_{\rm{Lyα}}$(LAE3) = $0.24\pm$0.03E-16 erg/s/cm$^2$, corresponding to SFR$_{\rm{Lyα}}\approx\ $5.0$\pm$0.5 M${_\odot}$/yr. The velocity width is $Δv$(LAE3) $\approx 400$ km/s, and equivalent width EW$_0$(Ly$α_{\,5σ}^{\,lim})\geq 34.05$ $\\A$, consistent with star formation being the primary driver of Ly$α$ emission. We also note a coherent absorption feature at $\sim -400$km/s in spectra from at least three objects; the QSO, LAE1 and "LAE2" which could imply the presence of an expanding neutral gas shell with an extent of at least $24$ pkpc.
