Connecting Galactic Outflows and Star Formation: Inferences from Hα Maps and Absorption-line Spectroscopy at 1 ≲ z ≲ 1.5This work is based in part on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.,The Astronomical Journal

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Connecting Galactic Outflows and Star Formation: Inferences from Hα Maps and Absorption-line Spectroscopy at 1 ≲ z ≲ 1.5This work is based in part on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
The Astronomical Journal ( IF 5.3 ) Pub Date : 2021-04-08 , DOI: 10.3847/1538-3881/abe85b
Nikolaus Z. Prusinski _{1,

2} , Dawn K. Erb ₁ , Crystal L. Martin ₃

Affiliation

We investigate the connection between galactic outflows and star formation using two independent data sets covering a sample of 22 galaxies between 1 ≲ z ≲ 1.5. The Hubble Space Telescope WFC3/G141 grism provides low spectral resolution, high spatial resolution spectroscopy yielding Hα emission-line maps from which we measure the spatial extent and strength of star formation. In the rest-frame near-UV, Keck/DEIMOS observes Fe ii and Mg ii interstellar absorption lines, which provide constraints on the intensity and velocity of the outflows. We compare outflow properties from individual and composite spectra with the star formation rate (SFR) and SFR surface density (Σ_SFR), as well as the stellar mass and specific SFR (sSFR). The Fe ii and Mg ii equivalent widths (EWs) increase with both SFR and Σ_SFR at ≳3σ significance, while the composite spectra show larger Fe ii EWs and outflow velocities in galaxies with higher SFR, Σ_SFR, and sSFR. Absorption-line profiles of the composite spectra further indicate that the differences between subsamples are driven by outflows rather than the interstellar medium. While these results are consistent with those of previous studies, the use of Hα images makes them the most direct test of the relationship between star formation and outflows at z > 1 to date. Future facilities such as the James Webb Space Telescope and the upcoming Extremely Large Telescopes will extend these direct, Hα-based studies to lower masses and SFRs, probing galactic feedback across orders of magnitude in galaxy properties and augmenting the correlations we find here.

中文翻译：

连接银河外流和恒星形成：从 Hα 图和 1 ≲ z ≲ 1.5 处的吸收线光谱推断这项工作部分基于 3D-HST 财政部计划（GO 12177 和 12328）与 NASA/ESA 哈勃望远镜的观测太空望远镜，由大学天文学研究协会运营，根据 NASA 合同 NAS5-26555。此处提供的一些数据是在 WM Keck 天文台获得的，该天文台是加州理工学院、加州大学和美国国家航空航天局之间的科学合作伙伴。WM Keck 基金会的慷慨资助使天文台成为可能。

我们使用覆盖 1 ≲ z ≲ 1.5之间的 22 个星系样本的两个独立数据集来研究星系流出和恒星形成之间的联系。哈勃太空望远镜 WFC3/G141 grism 提供低光谱分辨率、高空间分辨率光谱，产生 H α发射线图，我们可以从中测量恒星形成的空间范围和强度。在近紫外静止帧中，Keck/DEIMOS 观察到 Fe ii和 Mg ii星际吸收线，这对流出的强度和速度提供了限制。我们将单个和复合光谱的流出特性与恒星形成率 (SFR) 和 SFR 表面密度 (Σ _SFR)，以及恒星质量和比恒星形成率 (sSFR)。Fe ii和 Mg ii等效宽度 (EW) 随 SFR 和 Σ _SFR在 ≳3 σ显着性增加而增加，而复合光谱显示具有较高 SFR、Σ _SFR和 sSFR 的星系中更大的 Fe ii EW 和流出速度。复合光谱的吸收线剖面进一步表明子样本之间的差异是由外流而不是星际介质驱动的。虽然这些结果与之前的研究结果一致，但 H α图像的使用使它们成为对恒星形成与z 处外流之间关系的最直接测试> 1 至今。未来的设施，如詹姆斯韦伯太空望远镜和即将推出的超大望远镜，将把这些直接的、基于H α的研究扩展到较低的质量和恒星形成率，探测星系属性中跨数量级的星系反馈，并增强我们在这里找到的相关性。

更新日期：2021-04-08

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