SPIDER II --grizYJHK中早型半导体的基本平面
SPIDER II - The Fundamental Plane of Early-type Galaxies in grizYJHK
摘要：
我们提出了一个完整的分析的基本面的早期型星系（ETGs）在附近的宇宙。如论文I中所定义的，样本包括位于覆盖整个区域局部密度（从田地到集群）的环境中的39，993个ETG。我们推导了grizYJHK波段ETG的FP，详细讨论了拟合过程、选择效应引起的偏差以及r_e和mue相关误差引起的偏差等影响FP系数的关键因素。通过对Kormendy关系的研究，我们发现它的斜率在g（3.44 ± 0.04）到K（3.80 ± 0.02）之间变化，这意味着较小尺寸的ETG比具有较大re的星系具有更大的光学/近红外半径比。我们还研究了Faber-Jackson关系，发现在不确定性范围内，它的斜率对所有波段都是相似的，平均值为0.198 ± 0.007。从g到K的幅值选择样本的FP系数的变化分别为11%、可忽略不计和10%。我们发现，FP的倾斜变得更大的Sersic指数和更大的轴比，独立的波段，我们测量的FP变量。这表明这些变化可能与银河系性质的结构和动力学差异有关。我们还表明，目前的半分析模型的星系形成再现非常好的年龄和金属丰度的变化的恒星星族存在于大规模ETG作为在这些系统中的恒星质量的函数。特别是，我们发现，大规模的ETG有同时代的恒星流行的年龄变化只有百分之几，每十年的质量，而金属丰度增加与恒星质量的23%，每质量十年。
英文摘要：
We present a complete analysis of the Fundamental Plane of early-type galaxies (ETGs) in the nearby universe. The sample, as defined in paper I, comprises 39,993 ETGs located in environments covering the entire domain in local density (from field to cluster). We derive the FP of ETGs in the grizYJHK wavebands with a detailed discussion on fitting procedure, bias due to selection effects and bias due to correlated errors on r_e and mue as key factors in obtaining meaningful FP coefficients. Studying the Kormendy relation we find that its slope varies from g (3.44+-0.04) to K (3.80+-0.02) implying that smaller size ETGs have a larger ratio of optical/NIR radii than galaxies with larger re. We also examine the Faber-Jackson relation and find that its slope is similar for all wavebands, within the uncertainties, with a mean value of 0.198+-0.007. The variation of the FP coefficients for the magnitude selected sample from g through K amounts to 11%, negligible, and 10%, respectively. We find that the tilt of the FP becomes larger for higher Sersic index and larger axis ratios, independent of the waveband we measured the FP variables. This suggests that these variations are likely related to structural and dynamical differences of galaxian properties. We also show that the current semi-analytical models of galaxy formation reproduce very well the variation of age and metallicity of the stellar populations present in massive ETGs as a function of the stellar mass in these systems. In particular, we find that massive ETGs have coeval stellar pops with age varying only by a few % per decade in mass, while metallicity increases with stellar mass by 23% per mass decade.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
