ABRIDGED: NGC5253 was previously studied by our group with the aim to elucidate in detail the starburst interaction processes. Some open issues regarding the 2D structure of the main properties of the ionized gas remain to be addressed. Using IFS data obtained with FLAMES, we derived 2D maps for different tracers of electron density (n_e), electron temperature (T_e) and ionization degree. The maps for n_e as traced by several line ratios are compatible with a 3D stratified view of the nebula with the highest n_e in the innermost layers and a decrease of n_e outwards. To our knowledge, this is the first time that a T_e map based on [SII] lines for an extragalactic object is presented. The joint interpretation of our two T_e maps is consistent with a T_e structure in 3D with higher temperatures close to the main ionizing source surrounded by a colder and more diffuse component. The highest ionization degree is found at the peak of emission for the gas with relatively high ionization in the main GHIIR and lower ionization degree delineating the more extended diffuse component. Abundances for O, Ne and Ar are constant over the mapped area within <0.1 dex. The mean 12+log(O/H) is 8.26 while the relative abundances of log(N/O), log(Ne/O) and log(Ar/O) were \sim-1.32, -0.65 and -2.33, respectively. There are two locations with enhanced N/O. The first (log(N/O)\sim-0.95) is associated to two super star clusters. The second (log(N/O)\sim-1.17), reported here for the first time, is associated to two moderately massive (2-4x10^4 M_sun) and relatively old (\sim10 Myr) clusters. A comparison of the N/O map with those produced by strong line methods supports the use of N2O2 over N2S2 in the search for chemical inhomogeneities within a galaxy. The results on the localized nitrogen enhancement were used to compile and discuss the factors that affect the complex relationship between Wolf-Rayet stars and N/O excess.
A study of the interplay between ionized gas and star clusters in the central region of NGC 5253 with 2D spectroscopy
简要：本文对NGC 5253中心区进行了详细的二维研究，以描述其中心区~ 210 pc × 130 pc的恒星和电离气体结构以及电离气体的消光分布、物理性质和运动学特征。我们利用光学积分场光谱（IFS）与火焰获得的数据。NGC 5253中电离气体的详细消光图显示，最大的消光与突出的巨HII区域有关。在光学连续谱的峰和消光峰之间存在约0.5”的偏移，这与红外中的发现一致。我们发现恒星的消光比气体少0.33倍。[SII] l 6717/[SII] l 6731图显示电子密度（N_e）梯度从Ha（790 cm ^-3）的发射峰值向外下降，而Ar线比跟踪$N_e~4200 - 6200 cm ^（-3）的区域。根据过量[NII]/Ha推断，被额外氮污染的区域延伸到距离最大污染3.3”（~ 60 pc）的距离，该距离与连续排放峰值偏移~1.5”。沃尔夫-拉叶特徴以不规则的模式分布在较大的区域（~ 100 pc x 100 pc），与年轻的星团有关。我们测量了大部分视场中的He^+丰度，在局部区域中，He^+/H^+的值<~0.0005，这些区域通常与W-R发射或额外氮的区域不一致。线路轮廓很复杂。最多需要三个发射分量来再现它们。其中一个与巨大的HII区有关，呈现超音速宽度，[NII]和[SII]发射线相对于Ha移动了40 km/s。类似地，其中一个窄分量在[NII]线上呈现<~ 20 km/…
A deep, multi-epoch Chandra HETG study of the ionized outflow from NGC 4051
主动吸积的超大质量黑洞显著影响其宿主星系的演化，通过以广角流出排出大部分气体来截断进一步的恒星形成。X射线波段是理解这些黑洞风如何影响其环境的关键，因为流出物具有高温（$\sim$ 10 $^{5-8}$ K）。我们已经开发了一个贝叶斯框架，用于表征活动星系核（AGN）的外流，具有更好的探索参数空间和进行鲁棒模型选择的能力。我们将这个框架应用到一个新的700 ks和档案315 ks钱德拉高能透射光栅观测的塞弗特星系NGC 4051。我们已经检测到NGC 4051的六个固有吸收体。这些风分量的速度跨度从400 km s $^{-1}$到30，000 km s $^{-1}$。我们已经确定，统计上最重要的风分量是纯粹的碰撞电离，这是第一次检测到这样的吸收体。这种风具有$T\approx10^7$ K和$v\approx880$ km s $^{-1}$，并且在两个时期之间保持非常稳定。其他慢分量也随时间保持稳定。快速外流成分在2008年至2016年之间改变了它们的性质，这表明要么是物理变化，要么是云在视线范围内移动。对于其中一个快速分量，我们获得了迄今为止最严格的风密度测量值之一，log $n/$ [cm $^{-3}$ ]=13.0 $^{+0.01}_{-0.02}$，并确定它位于$\sim$ 240引力半径处。估计总流出功率超过5%的热光度（尽管有很大的不确定性），使其在星系-黑…
