1998年呂克華教授與李純良先生使用WIYN/Hydra多目標光纖光譜儀取得部份球狀星團NGC 288成員星及附近天區場星的光譜，這些光譜被用來分析徑向速度與判別光譜譜型。在分析過程中，天光平場光譜被用來檢驗本論文的色散校正精確度，經由IRAF/xcsao計算的結果得知本論文色散校正精確度可達5.5 km/s。我們求得NGC 288整體的徑向速度為-56.3±20.1 km/s，並將此徑向速度與 Guo (1995) 分析的自行運動量結合求得NGC 288相對於本地靜止標準的空間速度為(u,v,w)=(29.7±18.1, -258.6±18.3, 62.3±20.3)km/s,這樣的空間速度顯示NGC 288的軌道方向與銀河的旋轉方向相反。 Spectra of NGC~288 members and nearby field stars were obtained by Dr. Phillip K. Lu & John T. Lee with the WIYN/Hydra Multi-fiber positioner spectrograph in 1998 in order to get radial velocity and to classify the spectral types. A particular inspection through Solar spectra were carried out to investigate the precision of the radial velocity. Cross correlation analysis shows that our determination can achieve ~5.5 km/sec. The mean radial velocity of NGC 288 is -56.3±20.1 km/s, which was combined with the mean proper motion, obtained by Guo (1995) to derive the space velocity of NGC 288 with respect to Local Standard Rest and we get (u,v,w)=(29.7±18.1, -258.6±18.3, 62.3±20.3)km/s. We also compare the effective temperature, Teff, determined from spectral type as well as the result derived from the SED fitting by BATC data. The well agreement suggests that Teff resolved by multi-color fitting technique is more effective, and not less accurate, than traditional spectral observation.