论文标题
空间解决的CIII] $λ$ 1909在Haro 11中排放11
Spatially resolved CIII]$λ$1909 emission in Haro 11
论文作者
论文摘要
CIII] 1909（以下称为CIIII]）线是Ly $α$后最强的紫外线发射线，因此，对恒星形成（SF）星系的高红移研究引起了人们的关注。据认为，在具有亚级金属性和低质量的星系中，C III]发射最强，但是，在高红移和低红移处对许多此类星系的光谱观察产生了不确定甚至矛盾的结果。我们介绍了有史以来的第一个C III]成像，该成像是通过HST/STI获得的，用于低频SF Galaxy Haro 11。群集参数，例如恒星质量，灰尘分数和灰尘衰减以及通过光谱能量分布拟合获得的电离参数，与CIIII型宽度（与eW）相关的（ew）的范围不相关，该组合的组合是不相关的（集群人口。 Comparing the ratio of C III] emission line flux from individual clusters to that of H$α$, [O III], and [O II] we find that the clusters with the highest EW(C III]) can be reconciled only with Cloudy models with an extremely high C/O ratio of $\ge$ 1.4(C/O)$_\odot$ for an ionizing population of single stars, binary stars, or a mixture of二元星和活性银核。鉴于强度C III]的点状性质，EW（C III）的整合总强度依赖于星系的形态，这将解释在具有相似SF特性的星系中观察到的EW（C III]）强度的较大散射，并且具有相似的SF特性，并且具有相似的低金属性和恒星质量。
The CIII]1909 (hereafter, C III]) line is the strongest ultraviolet emission line after Ly$α$ and is therefore of interest to high redshift studies of star-forming (SF) galaxies near the epoch of reionization. It is thought that C III] emission is strongest in galaxies with subsolar metallicity and low mass, however, spectral observations of numerous such galaxies at high and low redshift produce inconclusive or even contradictory results. We present the first ever C III ] imaging, obtained with HST/STIS for the low-redshift SF galaxy Haro 11. Cluster parameters like stellar mass, dust fraction and dust attenuation, and ionization parameter, obtained through spectral energy distribution fitting, show no correlation with the CIII] equivalent width (EW), which may be due to a combination of the limitation of the models and the age-homogeneity of the cluster population. Comparing the ratio of C III] emission line flux from individual clusters to that of H$α$, [O III], and [O II] we find that the clusters with the highest EW(C III]) can be reconciled only with Cloudy models with an extremely high C/O ratio of $\ge$ 1.4(C/O)$_\odot$ for an ionizing population of single stars, binary stars, or a mixture of binary stars and active galactic nuclei. Given the point-like nature of strong C III], the integrated total strength of EW(C III]) becomes dependent on the morphology of the galaxy, which would explain the large scatter in EW(C III]) strengths, observed in galaxies with otherwise similar SF properties, and of similarly low metallicity and stellar mass.
