论文标题
使用成对的类星体光谱中C IV吸收器的横向自相关功能来限制伴生培养基的大小
Constraining the Size of the Circumgalactic Medium Using the Transverse Autocorrelation Function of C IV Absorbers in Paired Quasar Spectra
论文作者
论文摘要
环乳介质（CGM）在星系的形成和演化中起着至关重要的作用，它是星系与周围的播层培养基（IGM）之间的生命线。在这项研究中，我们利用了独特的类星体对样本来研究CGM的特性，并使用吸收线断层扫描。我们提供了一个中等分辨率的新样本Keck/Esi，Magellan/Mage和VLT/Xshooter Spectra的29 Quasar Pairs，Redshift $ 2 <Z <3 $。我们从文献中用32对的其他光谱补充样品，创建了一个61个类星体对的目录，具有1.7“和132.9”之间的角度分离，并在14 kpc和887 kpc之间进行了预测的物理分离（$ r_ \ perp $）。我们构建了906个金属线吸收双重C IV（$ λλ1548，1550 $）的目录，其等效宽度从6mÅ$ \ $ \ leq w_ {r，1550} \ leq 2053 $mÅ。样品的最佳拟合线性模型（$ \ log f（w_r）= m \ log（w_r）= m \ log（w_ {r}） + b $）的样品产生的系数为$ m = -1.44 \ pm0.16 $和$ b = -0.43 \ pm0.43 \ pm0.16 $。为了限制C IV的投影范围，我们计算横向自相关函数。在低$ r_ \ perp $下的自相关功能的扁平功能为金属富集的CGM的相干长度提供了下限 - 按200 $ h^{ - 1} $ commoving kpc的顺序。这种物理尺寸的约束使我们能够完善对CGM中金属的理解，在CGM中，CGM中的C IV范围取决于气流，反馈，金属注入和混合的时间表以及宿主星系的质量。
The circumgalactic medium (CGM) plays a vital role in the formation and evolution of galaxies, acting as a lifeline between galaxies and the surrounding intergalactic medium (IGM). In this study we leverage a unique sample of quasar pairs to investigate the properties of the CGM with absorption line tomography. We present a new sample of medium resolution Keck/ESI, Magellan/MagE, and VLT/XSHOOTER spectra of 29 quasar pairs at redshift $2 < z < 3$. We supplement the sample with additional spectra of 32 pairs from the literature, creating a catalog of 61 quasar pairs with angular separations between 1.7" and 132.9" and projected physical separations ($r_\perp$) between 14 kpc and 887 kpc. We construct a catalog of 906 metal-line absorption doublets of C IV ($λλ1548, 1550$) with equivalent widths ranging from 6 mÅ $\leq W_{r, 1550} \leq 2053$ mÅ. The best fit linear model to the log-space equivalent width frequency distribution ($\log f(W_r) = m\log(W_{r}) + b$) of the sample yields coefficients of $m=-1.44\pm0.16$ and $b=-0.43\pm0.16$. To constrain the projected extent of C IV, we calculate the transverse autocorrelation function. The flattening of the autocorrelation function at low $r_\perp$ provides a lower limit for the coherence length of the metal enriched CGM - on the order of 200 $h^{-1}$ comoving kpc. This physical size constraint allows us to refine our understanding of the metals in the CGM, where the extent of C IV in the CGM depends on gas flows, feedback, timescale of metal injection and mixing, and the mass of the host galaxies.
