M83环核星团的紫外光谱
Ultraviolet Spectroscopy of Circumnuclear Star Clusters in M83
摘要：
我们分析档案HST/STIS/FUV-MAMA成像和光谱的13个紧凑的星团内的环核星爆区域的M83，最近的这样的例子。我们比较观察到的光谱与半经验模型，这是基于银河系O和B星与IUE观察到的经验库，并与理论模型，这是基于一个新的理论UV库的热大质量恒星计算与WM基本。模型是用Starburst 99生成的，金属丰度为Z=0.020和Z=0.040，恒星IMF的质量上限为10，30，50和100 M_sol。我们估计的年龄和质量的集群从最佳拟合的模型光谱，并发现，来自半经验和理论模型的年龄同意平均在1.2倍。光谱年龄估计值来自HST/WFC 3/UVIS多波段测光的比较显示出类似的协议，但一个集群的水平。这些星团的年龄范围从300万年到2000万年不等，并且似乎没有沿着M83星暴的年龄梯度。具有强天鹅座P型轮廓的星团质量是10^4 M_sol的几倍，似乎已经形成了质量超过30 M_sol的恒星，并且与0.1-100 M_sol的Kroupa IMF一致。星爆中的场区缺乏P-Cygni剖面，主要由B星组成。
英文摘要：
We analyze archival HST/STIS/FUV-MAMA imaging and spectroscopy of 13 compact star clusters within the circumnuclear starburst region of M83, the closest such example. We compare the observed spectra with semi-empirical models, which are based on an empirical library of Galactic O and B stars observed with IUE, and with theoretical models, which are based on a new theoretical UV library of hot massive stars computed with WM-Basic. The models were generated with Starburst99 for metallicities of Z=0.020 and Z=0.040, and for stellar IMFs with upper mass limits of 10, 30, 50, and 100 M_sol. We estimate the ages and masses of the clusters from the best fit model spectra, and find that the ages derived from the semi-empirical and theoretical models agree within a factor of 1.2 on average. A comparison of the spectroscopic age estimates with values derived from HST/WFC3/UVIS multi-band photometry shows a similar level of agreement for all but one cluster. The clusters have a range of ages from about 3 to 20 Myr, and do not appear to have an age gradient along M83's starburst. Clusters with strong P-Cygni profiles have masses of a few times 10^4 M_sol, seem to have formed stars more massive than 30 M_sol, and are consistent with a Kroupa IMF from 0.1-100 M_sol. Field regions in the starburst lack P-Cygni profiles and are dominated by B stars.
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