On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
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DOI：
10.3847/1538-4357/ac7b88
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发表时间：
2022-08
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影响因子：
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通讯作者：
K. Rubin;Christian Juarez;K. Cooksey;J. Werk;J. Prochaska;J. O’Meara;J. Burchett;Ryan J. Rickards Vaught;V. Kulkarni;L. Straka
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作者：
K. Rubin;Christian Juarez;K. Cooksey;J. Werk;J. Prochaska;J. O’Meara;J. Burchett;Ryan J. Rickards Vaught;V. Kulkarni;L. Straka
我们利用中等分辨率的Keck/Echellette光谱仪和成像光谱仪对明亮类星体的冷气体进行了研究，其中Ca i λλ3934，3969和Na i λλ5891被追踪，5897在21个前景恒星形成星系的星际/环星系介质中，红移为0.03 1012.5 cm−2（N（Na i）> 1012.0 cm−2）的吸收发生在入射f C（Ca ii）= 0.63+0.10 −0.11（f C（Na i）= 0.57+0.10 −0.11）。我们发现没有证据表明f C或静止框架等效宽度Wr（Ca i K）或Wr（Na i 5891）对R或M * 的依赖性。相反，W r（Ca ii K）与局部SFR在>3σ显著性相关，表明Ca ii追踪星星形成驱动的外流。虽然大多数吸收体的速度在宿主红移的±50 km s−1以内，但它们的速度宽度（用Δv 90表示）普遍比星际物质的倾斜环速度模型所暗示的大30-177 km s−1。这些运动学必须追踪银河喷泉流，并证明它们在R> 5 kpc时持续存在。最后，我们评估了尘埃变红与W r（Ca ii K）（W r（Na i 5891））之间的关系，发现33%（24%）的吸收体与最佳拟合的银河系E（B−V）-W r关系在>3σ显著性上不一致。
We use medium-resolution Keck/Echellette Spectrograph and Imager spectroscopy of bright quasars to study cool gas traced by Ca ii λλ3934, 3969 and Na i λλ5891, 5897 absorption in the interstellar/circumgalactic media of 21 foreground star-forming galaxies at redshifts 0.03 1012.5 cm−2 (N(Na i) > 1012.0 cm−2) occur with an incidence f C(Ca ii) = 0.63+0.10 −0.11 (f C(Na i) = 0.57+0.10 −0.11). We find no evidence for a dependence of f C or the rest-frame equivalent widths W r (Ca ii K) or W r (Na i 5891) on R ⊥ or M *. Instead, W r (Ca ii K) is correlated with local SFR at >3σ significance, suggesting that Ca ii traces star formation-driven outflows. While most of the absorbers have velocities within ±50 km s−1 of the host redshift, their velocity widths (characterized by Δv 90) are universally 30–177 km s−1 larger than that implied by tilted-ring modeling of the velocities of interstellar material. These kinematics must trace galactic fountain flows and demonstrate that they persist at R ⊥ > 5 kpc. Finally, we assess the relationship between dust reddening and W r (Ca ii K) (W r (Na i 5891)), finding that 33% (24%) of the absorbers are inconsistent with the best-fit Milky Way E(B−V)-W r relations at >3σ significance.