The intensities of the coronal emission line at 5303 Angstrom (the green line) have been measured since 1951 at Norikura Coronagraph Station, National Astronomical Observatory of Japan. The measurements are made visually by using a prism spectrograph, at the height of 50 arcseconds above solar limb and at position angles 0, 5, 10, ,,, 355 degrees. The data from 1951 up to 1997 January are in the following format. (The data of 1997 January are included in the file for 1996.) One observation is written in six lines. YY MM DD hh mm 11 Id 1 I( 0) I( 5) ,,, I( 55) Obs YY MM DD hh mm 11 Id 2 I( 60) I( 65) ,,, I(115) Obs YY MM DD hh mm 11 Id 3 I(120) I(125) ,,, I(175) Obs YY MM DD hh mm 11 Id 4 I(180) I(185) ,,, I(235) Obs YY MM DD hh mm 11 Id 5 I(240) I(245) ,,, I(295) Obs YY MM DD hh mm 11 Id 6 I(300) I(305) ,,, I(355) Obs YY : year MM : month DD : day hh : hour mm : minute Id : diffuse light level I(PA): coronal intensity at position angle PA Id and I(PA) are in units of 10^(-6) of disk center brightness Obs : observer's ID 1 = M.Fukatsu 17 = M.Uchida 33 = T.Tsumita 2 = E.Hiei 18 = M.Ukai 34 = M.Ono 3 = H.Imai 19 = A.Yamaguchi 35 = T.Oe 4 = M.Irie 20 = Y.Yose 36 = S.Baba 5 = K.Kumagai 21 = H.Fukushima 37 = T.Hayashi 6 = M.Matsumoto 22 = I.Sano 38 = T.Natori 7 = M.Miyashita 23 = S.Ishikawa 39 = M.Notuki 8 = H.Miyazaki 24 = H.Miyazawa 40 = S.Nagasawa 9 = H.Morishita 25 = K.Mizugaki 41 = Y.Yamamoto 10 = Y.Nakagomi 26 = T.Kanda 42 = N.Tanaka 11 = Y.Ohki 27 = H.Sato 43 = Y.Nishino 12 = T.Okamoto 28 = S.Hamana 44 = K.Shinoda 13 = I.Shimizu 29 = S.Yajima 45 = M.Noguchi 14 = Y.Shimizu 30 = K.Higashi 46 = M.Saito 15 = T.Suzuki 31 = Y.Nojima 47 = Y.Suematsu 16 = A.Tokuya 32 = K.Nishi 48 = Y.Kato The data since 1997 October are represented in the format we use for the Quarterly Bulletin on Solar Activity.