行星状星云NGC 5128中轻元素的绝对分布
The Light Element Abundance Distribution in NGC 5128 from Planetary Nebulae
摘要：
用ESO VLT FORS 1多缝观测了覆盖[O III]光度函数上4等的许多行星状星云（PNe）的轻元素丰度分布。在3500-7500埃波长范围内的51个PNe的光谱是在4、8和17千秒差距的三个场中获得的，距离为3.8兆秒差距。发射线比率是完全典型的PN，如在银河系。在10个PNe中检测到弱温敏的[O III] 4363 A谱线，在30个PNe中检测到[O II]和[O III]谱线，在7个PNe中仅检测到亮的[O III] 5007 A谱线。云光电离模型运行，以匹配光谱的球形，恒定密度星云电离的黑体中心恒星。他，N，O和Ne丰度相对于H进行了测定，并为更明亮的PNE，S和Ar;中心恒星的光度和温度也来自。对于40个有云模式的PNe，从光度函数的上2个马格，最可靠的估计元素，氧，平均12+log（O/H）为8.52。O/H在2-20 kpc范围内没有明显的径向梯度。根据多缝积分星光光谱和光度学研究，PN丰度与恒星星族的比较表明[Fe/H]=-0.4和[O/Fe]=0.25。NGC 5128中PN中心恒星的质量来自模型轨道，这意味着形成的时代比少数年轻人口的颜色星等研究更近。PNE的祖先可能属于最近的，较小的，恒星形成插曲的年轻尾巴，或来自其他进化渠道。[摘要]
英文摘要：
The light element abundance pattern from many planetary nebulae (PNe) covering the upper 4 mag. of the [O III] luminosity function was observed with ESO VLT FORS1 multi-slit. Spectra of 51 PNe over the wavelength range 3500-7500 Angstrom were obtained in three fields at 4, 8 and 17 kpc, for a distance of 3.8 Mpc. Emission line ratios are entirely typical of PN such as in the Milky Way. The temperature sensitive [O III]4363A line was weakly detected in 10 PNe, both [O II] and [O III] lines were detected in 30 PNe, and only the bright [O III]5007A line in 7 PN. Cloudy photoionization models were run to match the spectra by a spherical, constant density nebula ionized by a black body central star. He, N, O and Ne abundances with respect to H were determined and, for brighter PNe, S and Ar; central star luminosities and temperatures are also derived. For 40 PNe with Cloudy models, from the upper 2 mag. of the luminosity function, the most reliably estimated element, oxygen, has a mean 12+log(O/H) of 8.52. No obvious radial gradient is apparent in O/H over a range 2-20 kpc. Comparison of the PN abundances with the stellar population, from the spectra of the integrated starlight on the multi-slits and photometric studies, suggests [Fe/H]=-0.4 and [O/Fe]=0.25. The masses of the PN central stars in NGC 5128 from model tracks imply an epoch of formation more recent than for the minority young population from colour-magnitude studies. The PNe progenitors may belong to the young tail of a recent, minor, star formation episode or derive from other evolutionary channels.[Abridged]
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