Star clusters are good tracers for formation and evolution of galaxies. We compared different fitting methods by using spectra (or by combining photometry) to determine the physical parameters. We choose a sample of 17 star clusters in M33, which previously lacked spectroscopic observations. The low-resolution spectra were taken with the Xinglong 2.16 m reflector of NAOC. The photometry used in the fitting includes u_SC and v_SAGE bands from the SAGE survey, as well as the published UBVRI and ugriz photometry. We first derived ages and metallicities with the ULySS (Vazdekis et al. and pegase-hr) simple stellar population model and the Bruzual & Charlot stellar population synthesis models for the full-spectrum fitting. The fitting results of both the BC03 and ULySS models seem consistent with those of previous works as well. Then, we add the SAGE u_SC and v_SAGE photometry in the spectroscopic fitting with the BC03 models. It seems that the results become much better, especially for the Padova 2000+Chabrier initial mass function set. Finally, we add more photometry data, UBVRI and ugriz, in the fitting, and we found that the results do not improve significantly. Therefore, we conclude that the photometry is useful for improving the fitting results, especially for the blue bands (λ<4000 Å), e.g., u_SC and v_SAGE band. At last, we discuss the “UV excess” for the star clusters, and we find that five star clusters have UV excess, based on the GALEX far-UV and near-UV photometry.

星团是星系形成和演化的良好示踪剂。我们通过使用光谱（或结合测光法）比较了不同的拟合方法来确定物理参数。我们在M33中选择了17个星团的样本，这些星团以前没有光谱观测。低分辨率光谱是用NAOC的兴隆2.16 m反射镜拍摄的。在装配中使用的测光包括ù _SC和v _SAGE从SAGE调查带，以及已公布UBVRI和ugriz测光。我们首先使用UL y SS（Vazdekis等人和pegase-hr）简单的恒星种群模型以及用于全光谱拟合的Bruzual＆Charlot恒星种群综合模型。BC03和UL y SS模型的拟合结果似乎也与以前的作品一致。然后，我们在BC03模型的光谱拟合中添加SAGE u _SC和v _SAGE光度法。似乎结果变得更好了，尤其是对于Padova 2000 + Chabrier初始质量函数集。最后，我们添加更多的测光数据，UBVRI和ugriz，在装修，而且我们发现，结果并不显著提高。因此，我们得出结论，光度法可用于改善拟合结果，特别是对于蓝带（λ<4000Å），例如u _SC和v _SAGE频段。最后，我们讨论了星团的“紫外线过量”，基于GALEX远紫外和近紫外光度法，我们发现五个星团都有紫外线过量。