来自CALIFA巡天的九个被动旋涡星系的恒星星族：它们是S0s的祖先吗？
Stellar populations of nine passive spiral galaxies from the CALIFA survey: are they progenitors of S0s?
摘要：
我们研究了CALIFA巡天中被动旋涡星系的恒星星族性质。选取了9个NUV-r > 5且光谱中无或弱星云发射线的旋涡星系作为被动旋涡星系。我们的被动螺旋位于红移范围为0.001 < z < 0.021，恒星质量范围为10.2 < log（M_{\star} / M_{\odot}）< 10.8。在WISE IR色色图中，它们显然属于早期星系。我们分析了恒星星族的两个有效半径，使用最佳拟合模型的Lick/IDS系统中测量的吸收线强度指数。我们发现被动螺旋的恒星星族分布范围很广，甚至在它们的中心也是如此，而且它们之间几乎没有任何共同的趋势。我们比较了被动螺旋与在相同质量范围内选择的S 0。S 0在年龄、金属丰度和[a/Fe]方面覆盖了很宽的范围，被动螺旋的恒星星族包含在S 0属性的传播中。然而，被动螺旋的分布偏向于较高的金属丰度值，较低的[a/Fe]，和年轻的年龄在所有半径。这些结果表明，被动螺线可能与它们的恒星星族中的S 0有关。我们推测，S 0的恒星星族的多样性可能是由于S 0形成的不同演化途径造成的，被动螺旋可能是其中一个可能的途径。
英文摘要：
We investigate the stellar population properties of passive spiral galaxies in the CALIFA survey. Nine spiral galaxies that have NUV-r > 5 and no/weak nebular emission lines in their spectra are selected as passive spirals. Our passive spirals lie in the redshift range of 0.001 < z < 0.021 and have stellar mass range of 10.2 < log(M_{\star}/M_{\odot}) < 10.8. They clearly lie in the domain of early-type galaxies in the WISE IR color-color diagram. We analyze the stellar populations out to two effective radius, using the best-fitting model to the measured absorption line-strength indices in the Lick/IDS system. We find that stellar populations of the passive spirals span a wide range, even in their centers, and hardly show any common trend amongst themselves either. We compare the passive spirals with S0s selected in the same mass range. S0s cover a wide range in age, metallicity, and [a/Fe], and stellar populations of the passive spirals are encompassed in the spread of the S0 properties. However, the distribution of passive spirals are skewed toward higher values of metallicity, lower [a/Fe], and younger ages at all radii. These results show that passive spirals are possibly related to S0s in their stellar populations. We infer that the diversity in the stellar populations of S0s may result from different evolutionary pathways of S0 formation, and passive spirals may be one of the possible channels.
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