A ∼15 kpc outflow cone piercing through the halo of the blue compact metal-poor galaxy SBS 0335–052E
A ∼15 kpc outflow cone piercing through the halo of the blue compact metal-poor galaxy SBS 0335–052E
复制标题
～15 kpc 流出锥体穿过蓝色致密贫金属星系 SBS 0335～052E 的光环
DOI：
10.1051/0004-6361/202244930
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发表时间：
2023
影响因子：
6.5
通讯作者：
Bik, A.
中科院分区：
文献类型：
--
作者：
Herenz, E. C.;Inoue, J.;Salas, H.;Koenigs, B.;Moya-Sierralta, C.;Cannon, J. M.;Hayes, M.;Papaderos, P.;Östlin, G.;Bik, A.
低质量恒星形成星系的外流是星系演化和宇宙学模型的基本组成部分。尽管在致密的恒星爆发星系中形成外流的条件似乎很有利，但在这样的系统中，千秒差距尺度的外流的令人信服的观测证据是稀缺的。目的在贫金属致密矮星SBS 0335− 052 E的晕中，千秒差距尺度的电离丝的出现以前与外流无关。在本文中，我们调查这些细丝是否提供证据outflow.MethodsWe获得了新的VLT/MUSE WFM和深NRAO/VLA B-配置21厘米的星系数据。MUSE数据提供了低表面亮度灯丝的Hβ/Hα和[O III]λ5007/Hα的形态学、运动学和发射线比，而VLA数据提供了系统内部和周围中性气体的形态学和运动学。这两个数据集被用于在音乐会之间的比较电离和中性phase.ResultsWe报告的lacy certainary电离结构的延长到16 kpc的投影距离在SBHα= 1.5 × 10 - 18尔格·s·cm-2 arcsec-2。 灯丝显示出不寻常的低Hα/Hβ = 2.4和低[O III]/Hα = 0.4 − 0.6，这是弥漫电离气体的典型特征。 它们的光谱很窄（约20 km s−1），并且没有速度子结构。细丝从细长的H I晕向外延伸。在小尺度上，NHI峰值偏离了主要的恒星形成地点。H I和H II的形态学和运动学揭示了恒星形成驱动的反馈如何不同地与电离和中性phase.ConclusionsWe相互作用的原因，灯丝是一个大规模的表现恒星形成驱动的反馈，即一个巨大的外流锥，突出通过这个富含气体的系统的晕的边缘边缘变亮。一个简单的玩具模型，这样一个圆锥形结构被发现与观察。
ContextOutflows from low-mass star-forming galaxies are a fundamental ingredient for models of galaxy evolution and cosmology. Despite seemingly favourable conditions for outflow formation in compact starbursting galaxies, convincing observational evidence for kiloparsec-scale outflows in such systems is scarce.AimsThe onset of kiloparsec-scale ionised filaments in the halo of the metal-poor compact dwarf SBS 0335−052E was previously not linked to an outflow. In this paper we investigate whether these filaments provide evidence for an outflow.MethodsWe obtained new VLT/MUSE WFM and deep NRAO/VLA B-configuration 21 cm data of the galaxy. The MUSE data provide morphology, kinematics, and emission line ratios of Hβ/Hαand [O III]λ5007/Hαof the low surface-brightness filaments, while the VLA data deliver morphology and kinematics of the neutral gas in and around the system. Both datasets are used in concert for comparisons between the ionised and the neutral phase.ResultsWe report the prolongation of a lacy filamentary ionised structure up to a projected distance of 16 kpc at SBHα= 1.5 × 10−18erg s cm−2arcsec−2. The filaments exhibit unusual low Hα/Hβ≈ 2.4 and low [O III]/Hα∼ 0.4 − 0.6 typical of diffuse ionised gas. They are spectrally narrow (∼20 km s−1) and exhibit no velocity sub-structure. The filaments extend outwards from the elongated H I halo. On small scales, theNHIpeak is offset from the main star-forming sites. The morphology and kinematics of H I and H II reveal how star-formation-driven feedback interacts differently with the ionised and the neutral phase.ConclusionsWe reason that the filaments are a large-scale manifestation of star-formation- driven feedback, namely limb-brightened edges of a giant outflow cone that protrudes through the halo of this gas-rich system. A simple toy model of such a conical structure is found to be commensurable with the observations.