KBSS-InCLOSE I：z~2-3 类星体视线发射星系内CGM的设计与初步结果
KBSS-InCLOSE I: Design and First Results from the Inner CGM of QSO Line Of Sight Emitting Galaxies at z~2-3
AI总结：
本文介绍了KBSS-InCLOSE巡天的设计与初步结果，通过结合Keck/KCWI和MOSFIRE观测，将z~2-3星系性质与内CGM物理条件相联系，发现星系外流将金属和尘埃驱动至CGM的直接证据。
摘要：
我们介绍了KBSS-InCLOSE（z~2-3类星体视线发射星系内环星系际介质）的设计与初步结果。该巡天将星系性质（如恒星质量M_*、星际介质ISM金属丰度）与内CGM的物理条件（如运动学、金属丰度）联系起来，以直接观测星系尺度的重子循环。我们获取了凯克重子结构巡天（KBSS）类星体的深空Keck/KCWI光学IFU指向，以发现小投影距离b≲12"（98 kpc，z̄=2.3）处的新恒星形成星系，随后获取后续Keck/MOSFIRE近红外光谱以确认其红移。我们利用KBSS图像和Keck/HIRES类星体光谱来模拟恒星族群和内CGM吸收。本文分析了两个类星体场，利用KCWI发现了15个以上的新星系，随后对Q2343-G1（z=2.43；G1）和Q2233-N1（z=3.15；N1）这两个星系使用MOSFIRE观测，它们均与阻尼莱曼α吸收体相关。我们发现G1具有典型的M_*以及紫外/光学发射性质。N1的M_*较低且具有极强的星云发射。我们联合分析了中性相CGM和电离ISM的N/O（在此z值下尚属首次）、尘埃消光以及高电离CGM，发现：G1的CGM贫金属且演化程度低于其ISM，而N1的CGM和ISM丰度相当；它们的CGM显示的尘埃消光比ISM少约1 dex；G1的CGM有热的、富金属星系外流喷射物的直接证据。这些发现支持金属和尘埃由外流驱动进入CGM，但也可能是剥离的ISM气体或卫星星系富集。完整的KBSS-InCLOSE样本将探索这些情景。
英文摘要：
We present the design and first results of the Inner Circumgalactic Medium (CGM) of QSO Line of Sight Emitting galaxies at $z\sim 2-3$, KBSS-InCLOSE. The survey will connect galaxy properties (e.g., stellar mass $M_*$, interstellar medium ISM metallicity) with the physical conditions of the inner CGM (e.g., kinematics, metallicity) to directly observe the galaxy-scale baryon cycle. We obtain deep Keck/KCWI optical IFU pointings of Keck Baryonic Structure Survey (KBSS) QSOs to discover new star-forming galaxies at small projected distances $b\lesssim12"$ (98 kpc, $\overline{z}=2.3$), then obtain follow-up Keck/MOSFIRE NIR spectra to confirm their redshifts. We leverage KBSS images and Keck/HIRES QSO spectra to model stellar populations and inner CGM absorption. In this paper, we analyze two QSO fields and discover more than 15 new galaxies with KCWI, then use MOSFIRE for two galaxies Q2343-G1 ($z=2.43$; G1) and Q2233-N1 ($z=3.15$; N1), which are both associated with Damped Lyman Alpha absorbers. We find that G1 has typical $M_*$,UV/optical emission properties. N1 has lower $M_*$ with very strong nebular emission. We jointly analyze neutral phase CGM and ionized ISM in N/O (for the first time at this $z$), dust extinction, and high-ionization CGM finding that: G1's CGM is metal poor and less evolved than its ISM, while N1's CGM and ISM abundances are comparable; their CGM shows $\sim1$ dex less dust extinction than the ISM; and G1's CGM has direct evidence of hot, metal-rich galactic outflow ejecta. These findings support that metals and dust are driven into the CGM from outflows, but may also be e.g., stripped ISM gas or satellite enrichment. The full KBSS-InCLOSE sample will explore these scenarios.
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