标题： 早期类型星系基本平面的倾斜度：波长依赖性 显示英文标题

标题： The tilt of the Fundamental Plane of Early-type galaxies: wavelength dependence

摘要： 74个后发星系团中的早型（E+S0+S0a）星系的光度参数R_e和mu_e首次在近红外H波段中被推导出来。 这些数据结合文献中找到的中心速度弥散测量值，用于确定该星系团的H波段基本平面对关系。 同样的方法应用于B、V、r、I和K波段中之前可用的光度数据，以进行多波长的基本平面研究。 由于FP参数值中的系统不确定性既来自于拟合算法的选择，也来自于样本选择过程中存在的统计偏差，因此我们强调在六个光度波段中使用相同的拟合算法并进行适当的修正以消除样本不完整性的影响的重要性。 我们发现FP的mu_e系数随波长变化是稳定的，而sigma系数随着波长的增加显著增加，这与Pahre & Djorgovski之前的结果一致。 尽管FP关系的斜率随波长变化，但从未接近维里定理的预期。 我们还发现，斜率变化的幅度可以完全由早型星系中颜色与亮度之间的已知关系来解释。 我们得出结论，基本平面的倾斜是显著的，必须是由于早型星系中某种形式的同位性破坏所致，而其波长依赖性则来自产生这些星系颜色-亮度关系的任何机制（目前首选的是质量-金属含量序列的存在）。 显示英文摘要

摘要： The photometric parameters R_e and mu_e of 74 early-type (E+S0+S0a) galaxies in the Coma cluster are derived for the first time in the near IR H band. These are used, coupled with measurements of the central velocity dispersion found in the literature, to determine the H band Fundamental Plane (FP) relation of this cluster. The same procedure is applied to previously available photometric data in the B, V, r, I, and K bands, to perform a multi-wavelength study of the FP. Because systematic uncertainties in the value of the FP parameters are introduced both by the choice of the fitting algorithm, and by the presence of statistical biases connected with the sample selection procedure, we emphasize the importance of deriving the FP parameters in the six photometric bands using an identical fitting algorithm, and appropriate corrections to eliminate the effects of sample incompleteness. We find that the FP mu_e coefficient is stable with wavelength, while the sigma coefficient increases significantly with increasing wavelength, in agreement with an earlier result presented by Pahre & Djorgovski. The slope of the FP relation, although changing with wavelength, never approaches the virial theorem expectation. We also find that the magnitude of the slope change can be entirely explained by the presence of the well known relation between color and magnitude among early-type galaxies. We conclude that the tilt of the Fundamental Plane is significant, and must be due to some form of broken homology among early-type galaxies, while its wavelength dependence derives from whatever mechanism (currently the preferred one is the existence of a mass-metal content sequence) produces the color-magnitude relation in those galaxies.