氮过剩蓝致密矮星系的积分场谱学
Integral field spectroscopy of nitrogen overabundant blue compact dwarf galaxies
摘要：
我们研究了三个蓝致密矮星系的物理性质和氧、氮丰度的空间分布（HS 0128+2832、HS 0837+4717和Mrk 930），其中报告了过量的N/O，以研究这种过量的性质，特别是，如果它与Wolf-Rayet（WR）星有关，我们用PMAS积分场光谱在可见光谱范围内观测到了这些BCD（3700 - 6900 ℃），使用直接法和适当的强线法绘制其物理化学性质。我们做一个统计分析的结果分布，我们比较它们与星系的综合属性。我们的结果表明，三个星系的外部位于[NII]/Hα vs. [OIII]/Hβ诊断图的“活动星系核区”，这很可能是由于这些区域的高N/O和激发结构的结合。从统计分析，它是假设，某一属性可以被认为是空间均匀（或均匀），如果一个正常的高斯函数适合其分布在几个地区的星系。此外，当高斯分布不符合相应的分布时，通常会出现积分性质与分布均值之间的不一致。我们发现，对于Mrk 930，除了电子密度和红化之外，所有参数都是均匀的。旋转曲线与Hα图和UV图像一起揭示了扰动的形态和可能的相互作用过程。在几个kpc量级的空间尺度上，N/O在三个研究对象中是恒定的，因此我们得出结论，从光谱学估计的WR星的数量不足以污染ISM并在这些对象中产生观测到的N/O过量
英文摘要：
We study the spatial distribution of the physical properties and of oxygen and nitrogen abundances in three Blue Compact Dwarf Galaxiess (HS 0128+2832, HS 0837+4717 and Mrk 930) with a reported excess of N/O in order to investigate the nature of this excess and, particularly, if it is associated with Wolf-Rayet (WR) stars We have observed these BCDs by using PMAS integral field spectroscopy in the optical spectral range (3700 - 6900 Å), mapping their physical-chemical properties, using both the direct method and appropriate strong-line methods. We make a statistical analysis of the resulting distributions and we compare them with the integrated properties of the galaxies. Our results indicate that outer parts of the three galaxies are placed on the "AGN-zone" of the [NII]/Hα vs. [OIII]/Hβ diagnostic diagram most likely due to a high N/O combined with the excitation structure in these regions. From the statistical analysis, it is assumed that a certain property can be considered as spatially homogeneous (or uniform) if a normal gaussian function fits its distribution in several regions of the galaxy. Moreover, a disagreement between the integrated properties and the mean values of the distribution usually appears when a gaussian does not fit the corresponding distribution. We find that for Mrk 930, the uniformity is found for all parameters, except for electron density and reddening. The rotation curve together with the Hα map and UV images, reveal a perturbed morphology and possible interacting processes. The N/O is found to be constant in the three studied objects at spatial scales of the order of several kpc so we conclude that the number of WR stars estimated from spectroscopy is not sufficient to pollute the ISM and to produce the observed N/O excess in these objects
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