用CALIFA探索了质量-金属丰度关系：I.是否存在对恒星形成率的依赖性？
The Mass-Metallicity relation explored with CALIFA: I. Is there a dependence on the star formation rate?
摘要：
本文根据CALIFA巡天（150个星系）的第一批观测数据，给出了星系整体和局部M-Z关系的研究结果。这次巡天提供了每个星系完整光学范围的积分场光谱（最多2-3个有效半径），具有足够的分辨率来分离单个HII区域和/或聚集体。已检测到近$\sim$ 3000个单独的HII区域。光谱覆盖了[OII]3727和[SII]6731之间的波长范围，具有足够的信噪比来推导与每个区域相关的氧丰度和恒星形成率。此外，我们已经计算了综合和空间分辨恒星质量（和表面密度），SDSS光度数据的基础上。利用这些数据，我们探讨了恒星质量、氧丰度和恒星形成速率之间的关系。我们得到的积分恒星质量和气相丰度之间的紧密关系，与分散小于一个已经在文献中报道（$σ_{Δ{\rm log(O/H)}}=$ 0.07德克斯）。事实上，这个分散度只比我们的氧丰度得出的典型误差稍大。然而，我们没有发现任何次要的关系与恒星形成率，除了一个诱导由于这个量与恒星质量的主要关系。我们使用$\sim$ 3000个单独的HII区域来确认相应的局部关系的结果。我们的研究结果同意的情况下，在星系中的气体回收，无论是本地和全球范围内，是远远快于其他典型的时间尺度，如气体吸积流入和/或金属损失，由于流出。从本质上讲，晚型/盘主导的星系似乎是在一个准稳定的情况下，从一个瞬时回收/闭盒模型的预期类似的行为。
英文摘要：
We present the results on the study of the global and local M-Z relation based on the first data available from the CALIFA survey (150 galaxies). This survey provides integral field spectroscopy of the complete optical extent of each galaxy (up to 2-3 effective radii), with enough resolution to separate individual HII regions and/or aggregations. Nearly $\sim$3000 individual HII regions have been detected. The spectra cover the wavelength range between [OII]3727 and [SII]6731, with a sufficient signal-to-noise to derive the oxygen abundance and star-formation rate associated with each region. In addition, we have computed the integrated and spatially resolved stellar masses (and surface densities), based on SDSS photometric data. We explore the relations between the stellar mass, oxygen abundance and star-formation rate using this dataset. We derive a tight relation between the integrated stellar mass and the gas-phase abundance, with a dispersion smaller than the one already reported in the literature ($σ_{Δ{\rm log(O/H)}}=$0.07 dex). Indeed, this dispersion is only slightly larger than the typical error derived for our oxygen abundances. However, we do not find any secondary relation with the star-formation rate, other than the one induced due to the primary relation of this quantity with the stellar mass. We confirm the result using the $\sim$3000 individual HII regions, for the corresponding local relations. Our results agree with the scenario in which gas recycling in galaxies, both locally and globally, is much faster than other typical timescales, like that of gas accretion by inflow and/or metal loss due to outflows. In essence, late-type/disk dominated galaxies seem to be in a quasi-steady situation, with a behavior similar to the one expected from an instantaneous recycling/closed-box model.
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