蓝色致密矮星系中的星暴。Mrk 1418的PMAS积分场谱
Mapping the starburst in Blue Compact Dwarf Galaxies. PMAS Integral Field Spectroscopy of Mrk 1418
摘要：
（节略）目的：通过光学积分场光谱（IFS）的观测，我们的目标是解开和描述的星暴成分在BCD Mrk 1418。特别是，我们建议研究恒星和电离气体的形态，研究电离机制（S）在星际介质，推导出的物理参数和电离气体的丰度。方法：在中国天文台3.5米望远镜上用PMAS对Mrk 1418进行IFS观测。中央16“x16”被映射。根据这些数据，我们绘制了最突出的发射谱线的地图，即[OII]，H-beta，[OIII]，H-alpha，[NII]和[SII]以及几个连续谱带，加上主线比率的地图：[OIII]/H-β、[NII]/H-α、[SII]/H-α和H-α/H-β，导出了视场中探测到的不同恒星形成区的物理参数和气态金属丰度。结果如下：Mrk 1418在连续谱和电离气体图中都显示出扭曲的形态;当前的恒星形成事件发生在五个节中，分布在星系核周围。这些结周围的星际介质被恒星光电离，没有其他激发机制的明确证据。该星系显示出不均匀的尘埃分布，中心区域的高H-α/H-β比率表明有大量的尘埃。各个恒星形成节点的氧丰度非常相似，这表明电离的星际介质在数百秒差距的空间尺度上是化学均匀的O/H。这个丰度（根据经验校准，Z~0.4 Z_solar）将Mrk 1418置于高金属丰度BCD组中。
英文摘要：
(Abridged) Aims: By means of optical Integral Field Spectroscopy (IFS) observations, we aim to disentangle and characterize the starburst component in the BCD Mrk 1418. In particular we propose to study the stellar and ionized gas morphology, to investigate the ionization mechanism(s) acting in the interstellar medium, to derive the physical parameters and abundances of the ionized gas. Methods: IFS observations of Mrk 1418 were carried out with PMAS at the 3.5 m telescope at CAHA. The central 16"x16" were mapped. From these data we built maps of the most prominent emission lines, namely [OII], H-beta, [OIII], H-alpha, [NII] and [SII] as well as of several continuum bands, plus maps of the main line ratios: [OIII]/H-beta, [NII]/H-alpha, [SII]/H-alpha, and H-alpha/H-beta, and derived the physical parameters and gaseous metal abundances of the different star-forming regions detected in the field of view. Results: Mrk 1418 shows a distorted morphology both in the continuum and in the ionized gas maps; the current star-formation episode is taking place in five knots, distributed around the nucleus of the galaxy. The interstellar medium surrounding these knots is photo-ionized by stars, with no clear evidence for other excitation mechanisms. The galaxy displays an inhomogeneous dust distribution, with the high H-alpha/H-beta ratio in the central areas indicating a large amount of dust. The oxygen abundances derived for the individual star-forming knots are very similar, suggesting that the ionized interstellar medium is chemically homogeneous in O/H over spatial scales of hundreds of parsecs. This abundance (Z~0.4 Z_solar from the empirical calibrations) places Mrk 1418 among the high metallicity BCD group.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
