During 1997-2006 there are 40 solar energetic particle (SEP) events with the peak proton intensity Jpm> 1/cm2srs at proton energies of>60 MeV from GOES data. These events are archived in 39 folders. Each folder comprises the omnidirectional intensity (omn) and sectored count (sec) data of H(2.5-4 MeV), He2(2.5-5 MeV/n), He5(5-8 MeV/n), O(2.5-5 MeV/n), and Fe(2.5-5 MeV/n) ions with 1-hour time resolution as measured by the Wind/EPACT/LEMT sensor. Also, there is a solar wind + IMF data file (swd) taken from the NASA/SPDF/CDAWeb OMNI data. In addition, there are two value-added products included. (1) The ion first-order anisotropy (A1s) data calculated from the omn, sec, and swd files mentioned above. The calculation method is based on Tan et al. (ApJ, 661, 1297, 2007). (2) The first-order anisotropy plot of various ions from the deduced ion anisotropy data, which should help people making a preliminary study of the events without a lot of effort. It should be mentioned that in the calculation of the ion first-order anisotropy in the solar wind frame the index (gamma) of ion energy spectra is a necessary parameter. We use the gamma of protons as deduced from IMP-8 proton data. For the event in which the IMP-8 proton data are absent, the gamma of He2(2.5-5 MeV/n) ions is used instead. It is because that from 21 selected SEP events that have IMP-8 proton data (from 1997 Nov. 3 to 2001 Oct. 21) the ratio of gamma of H(2.5-4 MeV) to gamma of He2(2.5-5 MeV/n) is found to be 1.0+-0.2. Therefore, the gamma of He2 ions can be used to be the gamma of H ions, provided that the error (+-0.2) has been included into the final error estimation of proton anisotropy. Since the omni, sec, and swd files are self-explanatory, below we will only describe the format of the deduced A1s file. A1s_YYYYMMDD.txt File Description: Hourly output of the deduced bulk flow velocity and first-order anisotropy data of H, He, O, or Fe ions as measured by Wind/EPACT/LEMT. Data format is the text file with comma-separated values (CSV). The notation of the file name XXX_omn_YYYYMMDD.txt or XXX_sec_YYYYMMDD.txt: XXX= H 2.5-4 MeV H ions XXX=He2 2.5-5 MeV/n He ions XXX=He5 5-8 MeV/n He ions XXX= O 2.5-5 MeV/n O ions XXX= Fe 2.5-5 MeV/n Fe ions YYYY Year MM Month DD Day The Day is usually one day before the launch time of the primary coronal mass ejection (CME) that causes the solar energetic particle (SEP) event. Variable Notes: iyear Year (I4) imonth month(I2) iday day(I2) ihour hour(I2) The above integer time is the starting time of the sampled 1-hour interval doy Day of Year day Day of Month The above floating time is the center time of the sampled 1-hour interval Solar Wind& IMF variables and their RMS deviations B, dB 1AU IP Magnitude of average field vector (nT) thetaB, dthetaB 1AU IP Latitude/Theta of average B vector (deg) phiB, dphiB 1AU IP Longitude/Phi of average B vector (deg) phiBA, dphiBA When phiB> 180, phiBA = phiB-360 (deg) N, dN 1AU IP Ion number density (per cc) Vsw, dVsw 1AU IP plasma flow speed (1000 km/s) phisw, dphisw 1AU IP plasma flow longitude (deg) Va Alfven speed (1000 km/s) Ion spectra variables gamma dgamma Power-law index of ion energy spectra Tm Mean energy of ions in the sampled energy range (MeV/n) logJm Logarithmic ion intensity at Tm (1/(cm2 s sr MeV/n)) Normalized Anisotropies calculated in the spacecraft frame A1/A0 dA1/A0 First-order anisotropy A2/A0 dA2/A0 Second-order anisotropy A3/A0 dA3/A0 Third-order anisotropy Bulk flow velocities and their RMS deviations Vf dVf Ion bulk flow speed (1000 km/s) phif dphif Longitudinal angle of ion bulk flow velocity (deg) phif-phiB dphif-phiB Difference between phif and PhiB (deg) First anisotropies in the solar wind frame and their RMS deviations A1s dA1s Magnitude of ion first-order anisotropy in the solar wind frame phiA1s dphiA1s Longitudinal angle of ion first-order anisotropy in the solar wind frame (deg) A1speB dA1speB A1s component perpendicular to the mean magnetic field A1spaB dA1spaB A1s component parallel to the mean magnetic field