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A comparison of the UV and HI properties of the extended UV (XUV) disk galaxies NGC 2541, NGC 5832 and ESO406-042
Journal of Astrophysics and Astronomy ( IF 1.1 ) Pub Date : 2021-07-24 , DOI: 10.1007/s12036-021-09749-9
M. Das 1 , J. Yadav 1 , J. Murthy 1 , N. Patra 2 , K. S. Dwarakanath 2 , S. S. McGaugh 3 , J. Schombert 4 , P. T. Rahna 5
Affiliation  

We present a UV study of 3 extended UV (XUV) galaxies that we have observed with the UVIT and the GMRT. XUV galaxies show filamentary or diffuse star formation well beyond their optical disks, in regions where the disk surface density lies below the threshold for star formation. GALEX observations found that surprisingly 30% of all the nearby spiral galaxies have XUV disks. The XUV galaxies can be broadly classified as Type 1 and Type 2 XUV disks. The Type 1 XUV disks have star formation that is linked to that in their main disk, and the UV emission appears as extended, filamentary spiral arms. The UV luminosity is associated with compact star forming regions along the extended spiral arms. The star formation is probably driven by slow gas accretion from nearby galaxies or the intergalactic medium (IGM). But the Type 2 XUV disks have star formation associated with an outer low luminosity stellar disk that is often truncated near the optical radius of the galaxy. The nature of the stellar disks in Type 2 XUV disks are similar to that of the diffuse stellar disks of low surface brightness galaxies. The star formation in Type 2 XUV disks is thought to be due to rapid gas accretion or gas infall from nearby high velocity clouds (HVCs), interacting galaxies or the IGM. In this paper, we investigate the star formation properties of the XUV regions of two Type 2 galaxies and one mixed XUV type galaxy and compare them with the neutral hydrogen (HI) emisison in their disks. We present preliminary results of our UVIT (FUV and NUV) observations of NGC 2541, NGC 5832 and ESO406-042, as well as GMRT observations of their HI emission. We describe the UV emission morphology, estimate the star formation rates and compare it with the HI distribution in these Type 2 and mixed XUV galaxies.



中文翻译:

扩展紫外线 (XUV) 盘状星系 NGC 2541、NGC 5832 和 ESO406-042 的 UV 和 HI 特性比较

我们展示了我们用 UVIT 和 GMRT 观测到的 3 个扩展紫外线 (XUV) 星系的紫外线研究。XUV 星系在盘面密度低于恒星形成阈值的区域显示出远远超出其光盘的丝状或漫射恒星形成。GALEX 观测发现,令人惊讶的是,附近所有螺旋星系中有 30% 具有 XUV 盘。XUV 星系可以大致分为 1 型和 2 型 XUV 盘。1 型 XUV 盘的恒星形成与其主盘中的恒星形成相关联,并且紫外线发射表现为延伸的丝状旋臂。紫外光度与沿延伸旋臂的致密恒星形成区域有关。恒星的形成可能是由附近星系或星系际介质(IGM)缓慢的气体吸积驱动的。但是 2 型 XUV 盘的恒星形成与外部低光度恒星盘有关,该盘通常在星系的光学半径附近被截断。2 型 XUV 盘中星盘的性质类似于低表面亮度星系的漫射星盘。2 型 XUV 盘中的恒星形成被认为是由于来自附近高速云 (HVC)、相互作用的星系或 IGM 的快速气体吸积或气体下降。在本文中,我们研究了两个 2 型星系和一个混合 XUV 型星系的 XUV 区域的恒星形成特性,并将它们与它们盘中的中性氢 (HI) 发射进行了比较。我们展示了我们对 NGC 2541、NGC 5832 和 ESO406-042 的 UVIT(FUV 和 NUV)观测的初步结果,以及它们的 HI 发射的 GMRT 观测。

更新日期:2021-07-24
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