by A. Arinc Table 1. Experimental half-life values of 106 Rh. Reference Half-life (seconds) Comments UWM 30.1 (3) WM (23) reduced-χ 2 = 10.

Transcription

1 Comments on evaluation of decay data by A. Arinc Evaluation completed: March 2013 Literature cut-off date: December 2012 Evaluation procedure Weighted mean analyses were applied to determine recommended values throughout the evaluation when the data were in statistical agreement. When the data were not in statistical agreement, the Limitation of Relative Statistical Weights (LRSW) was used. Uncertainties were expanded to match the minimum input uncertainty where appropriate. Decay scheme is the daughter of 106 Ru and disintegrates by beta minus emission to various excited levels and the ground state of 106 Pd. The spins, parities, multipolarities, mixing ratios and level energies of 106 Pd are based on the mass-chain evaluation of De Frenne and Negret (2008De09). The Q(β - ) value of 3546 (5) kev is taken from the evaluation of Wang et al. (2012Wa38). Half-life The experimental half-life values used for calculating the recommended value are given in Table 1. The half-life values from 1946Se30 and 1950Gl05 were omitted from the analysis as no uncertainty was given. The data set is discrepant with a reduced-χ 2 of 10.9 on the Weighted Mean (WM) which is larger than the critical reduced-χ 2 of The recommended value of 30.1 (3) seconds is the Unweighted Mean (UWM) of 1966Mi10 and 1969KoZW. Table 1. Experimental half-life values of. Reference Half-life (seconds) Comments 1946Se30 40 no uncertainty 1950Gl05 30 no uncertainty 1966Mi (15) 1969KoZW (8) UWM 30.1 (3) WM (23) reduced-χ 2 = 10.9 Recommended value 30.1 (3) In the majority of circumstances will be encountered in equilibrium with 106 Ru therefore an accurate knowledge of the half-life is not required; however for applications where the is unsupported by 106 Ru (for example decay heats), new measurements of the half-life would be beneficial as the available data are inconsistent and in excess of 40 years old.

2 Gamma rays When more than one publication was available per laboratory only the latest published data were used (e.g. 1972Ma71 and 1973Ma35; 1960Ro12 and 1965Ro09). Published data with no reported uncertainty were not used for averaging process (i.e. 1971Az02, 1957Fi50). Energies The recommended values were derived from the differences in level energies as adopted from the mass-chain evaluation of 2008De09, and were compared to the experimental values calculated from the weighted mean (calculated with LWEIGHT4 code) of 1982Ka10, 1977Ok02, 1969St03, 1973Ma35, 1975Hs02, 1965Ro09, 1967Fo09, 1967Vr05 and 1968Ha35. When there was a disagreement between the calculated and evaluated gamma-ray emission energies, the latter were used. Although a few recent publications were available (1976Sh25, 1983Ku03 and 1993Ch32) on the precise measurement of the kev gamma-ray emission energy, the recommended value of (23) kev was taken from Helmer and van der Leun (2000He14). The data set from Rao and Fink (1967Ra11) was not taken into account as many of the values in this publication were excluded by Chauvenet s criterion as outliers. In the publication of Forest et al. (1967Fo09) only the values up to 2614 kev were used as this was the last energy calibration point available to the user based upon the information given, and any energies above this point will have been based upon extrapolation. In the publication of Hsue et al. (1975Hs02), only the use of a standard gamma calibration source was mentioned, which usually does not cover gamma-ray emissions as high as 3.3 MeV. The values from 1975Hs02 above 2000 kev are generally lower and with smaller associated uncertainties compared with the rest of the values reported by other authors, which may imply that an extrapolation of the energies was performed rather than a more precise interpolation. Therefore, the evaluator has decided to increase the uncertainties of 1975Hs02 above 2000 kev to a minimum of 0.3 kev to be in line with other reported uncertainties. Adopted nuclear levels of 106 Pd can be seen in Table 2. The experimental results and recommended values can be seen in Table 1 of Appendix 1.

3 Nuclear level number 0 1 Table 2. Adopted nuclear levels of 106 Pd. Nuclear level energy (kev) (23) a 2 + Spin and parity (3) (4) (4) (4) (3) (5) (16) (1 +, 2 +) (5) (5) (9) (5) (7) (20) (1 -) (8) (5) (8) (1 +) (21) (21) (9) (9) (7) (10) (8) (21) (17) (9) (18) (3) (25) (5) (4) (7) (7) (3) (9) (6) , (1, 2+) , 2 a) Derived from Helmer and van der Leun (2000He14) gamma-ray emission energy of (23) kev. Probabilities The gamma-ray emission probabilities were calculated as weighted means (calculated with LWEIGHT4 code) of the measurements of 1982Ka10, 1977Ok02, 1975Hs02, 1975De17, 1973Ma35, 1969Od01, 1696St03, 1968Ha35, 1967Vr05, 1967Ra11, 1967Fo09, 1966Ov01, 1962Am03, 1960Se07 and 1960Ro12. In some of the earlier papers (1960Ro12, 1960Se07, 1962Am03 and 1966Ov01) the high energy gamma-ray emission probabilities were impossible to place due to large differences between the energies measured by the authors and the adopted energies. In the publication of Hsue et al. (1975Hs02), the reported annihilation contribution of 0 +

4 5.1 % on the most intense peak at kev was disputed by Kaur et al. (1982Ka10) as being almost negligible. The annihilation contribution is dependent on the specifications of the gammaray spectrometry system and cannot be verified without precise details on the equipment and shielding used. Therefore the evaluator has decided to increase the reported uncertainties of 1975Hs02 by 5.1 %. Values were initially normalised to an intensity for the kev gamma-ray emission of The experimental results and recommended values can be seen in Table 2 of Appendix 1. Internal conversion coefficients and E0 transition probability Theoretical internal conversion coefficients (ICCs) were calculated using the BrIcc code (Kibédi et al., 2008Ki07) with the frozen orbital approximation, which uses interpolated values of Band et al. (2002Ba85). The transition at kev is pure E0 and absolute measurements for this transition were not available; the transition probability cannot be calculated using the balance of the decay scheme because the beta probabilities are not well known for the levels concerned. Using the ratio of the K- conversion electron intensity of the E0 transition to that of the E2 transition at kev, q 2 K(E0/E2) = (7) from Kibédi and Spear (2005Ki02) and the following data for the kev line: Relative gamma-ray emission probability (Pγ): 481 (5) ICC for K shell (α K ): (40) The calculated relative K-conversion intensity for the kev gamma ray is: = Pγ (621) α K (621) q 2 K(E0/E2 of 1133 to 621) = 481 (5) (40) (7) = 0.22 (3) Using the electronic factors for E0 calculated by BrIcc and assuming proportionality between the electronic factors and the conversion on each subshell, this gives a total relative conversion intensity for the kev transition of 0.25 (3). Normalisation factor Five absolute experimental values reported for the strongest gamma ray line at kev are given in Table 3. The AveTools computer code was used to calculate the average using three statistical methods: Limitation of Relative Statistical Weights (LRSW), Normalised Residual Methods (NRM) and the Rajeval Technique (RT).

5 Table 3. Absolute experimental values for the gamma ray line at kev. Reference Absolute Pγ 1,0 (%) Used Comments 1953Ka no No uncertainty 1966Ov (20) no Later publication 1975Ge06 available 1969Od (6) yes 1975De (23) yes 1975Ge (11) yes Uncertainty 95 % confidence UWM 21.0 (5) WM 20.7 (4) LRSW (5) NRM (21) RT (21) Recommended value (23) Minimum input uncertainty used The recommended value was taken from the Rajeval Technique and the minimum input uncertainty from 1975De17 was used. Using the absolute Pγ 1,0 value calculated above we can derive a normalisation factor of (23). The theoretical value obtained from the balance of the decay scheme to the ground state, taking the beta emission efficiency β 0,0 from 1992Gr21 of 79.1 (16) %, is (16) which is in good agreement with the value calculated from the experimental data. Beta particles Energies The values of the maximum beta-particle energies were derived from the Q(β - ) = 3546 (5) kev value from Wang et al. (2012Wa38) and the adopted nuclear level energies given in Table 2. The experimental data for the maximum beta-particle emission energies to the ground state (β 0,0 max ) is in good agreement with the calculated data and can be found in Table 4. The mean beta-particle energies and log ft values were calculated with the LOGFT code. Table 4. Experimental values for the maximum beta-particle emission energies to the ground state and first excited state of 106 Pd. Reference β 0,0 max (MeV) β 0,1 max (MeV) 1947Pe (10) 1958Gr (1) 1966JoZZ 3.55 (100) 3.04 (7) 1963Ke Be (12) Recommended value (5) (5)

6 Emission probabilities The theoretical beta-particle probabilities were calculated from the P(γ+ce) balance using the GTOL software and are given in Table 5. Table 5. Beta-particle emission energies, probabilities, transition type and log ft values of. Transition E βmax (kev) P β (%) Transition type log ft β 0, (5) (24) Allowed 5.18 β 0, (5) 8.2 (3) Allowed 5.87 β 0, (5) (21) Allowed 6.58 β 0, (5) 9.82 (15) Allowed 5.37 β 0, (5) (5) Unique 2 nd Forbidden 11.0 β 0, (5) 1.67 (3) Allowed 5.79 β 0, (5) (10) Allowed 7.06 β 0, (5) (21) (Allowed) 8.24 β 0, (5) (9) Allowed 5.93 β 0, (5) (8) Allowed 6.72 β 0, (5) (5) Allowed 6.62 β 0, (5) (7) Allowed 6.57 β 0, (5) (5) Allowed 6.71 β 0, (5) (15) (1 st Forbidden) 7.99 β 0, (5) (6) 1 st Forbidden 6.48 β 0, (5) (3) Allowed 5.78 β 0, (5) (4) (Allowed) 6.56 β 0, (5) (12) - - β 0, (5) (8) Allowed 7.36 β 0, (5) (3) Allowed 6.40 β 0, (5) (19) Allowed 6.47 β 0, (5) (9) Allowed 5.81 β 0, (5) (18) Allowed 6.29 β 0, (5) (7) Allowed 5.87 β 0, (5) (4) Unique 1 st Forbidden 7.82 β 0, (5) (3) - - β 0, (5) (5) Allowed 5.76 β 0, (5) (13) - - β 0, (5) (5) (Allowed) 6.55 β 0, (5) (13) Allowed 5.56 β 0, (5) (16) Allowed 7.09 β 0, (5) (4) Allowed 6.70 β 0, (5) (14) - - β 0, (5) (21) - - β 0, (5) (8) Allowed 5.71 β 0, (5) (9) - - β 0, (5) (19) - -

7 Table 6. Published values for the beta-particle emission probability to the ground state of 106 Pd. Reference β 0,0 (%) 1947Pe07 82 (2) 1958Gr Se Am Ke JoZZ Gr (16) Recommended value (24) The most recent and most precise measurement of the beta-particle emission probability to the ground state of 106 Pd reported by Greenwood et al. (1992Gr21) using total absorption gamma-ray spectrometry (TAGS) and the value derived theoretically from the singles gamma studies agree within the stated uncertainties. Atomic data The values of ω K, L, n KL and relative probabilities of the X-ray and Auger emissions were derived from Schönfeld and Janßen (1996Sc06). The energies and relative emission probabilities of the X-ray and Auger electrons have been calculated using the computer code EMISSION. A summary of the results is given in Tables 7 and 8. There are no known publications of measured data with which these values can be compared. Table 7. Calculated L X-ray emission energies and probabilities. L Xray Energy, /kev Calculated value Ll (5) Lα (11) Lη (17) Lβ (8) Lγ (6) LX total (14) Table 8. Calculated K X-ray emission energies and probabilities. K Xray Energy, /kev Calculated value Kα (5) Kα (9) Kβ (29) Kβ (10) KX total (17)

8 References 1946Se30 W. Seelmann-Eggebert, Naturwiss. 33 (1946) 279. [Half-life] 1947Pe07 W.C. Peacock, Phys. Rev. 72 (1947) [E β, P β ] 1950Gl05 L.E. Glendenin, E.P. Steinberg, National Nuclear Energy Series NNES 9 (1950) 793. [Half-life] 1953Ka47 B. Kahn, W.S. Lyon, Phys. Rev. 92 (1953) Fi50 E.I. Firsov, A.A. Bashilov, Izvest. Akad. Nauk SSSR, Ser. Fiz. 21 (1957) 1633; Columbia Tech. Transl. 21 (1958) ] 1958Gr07 E.P. Grigorev, A.V. Zolotavin, I.I. Kuzmin, E.D. Pavlitskaia, Izvest. Akad. Nauk SSSR, Ser. Fiz. 22 (1958) 194; Columbia Tech. Transl. 22 (1959) 191. [E β, P β ] 1960Ro12 R.L. Robinson, F.K. McGowan, W.G. Smith, Phys. Rev. 119 (1960) Se07 O.J. Segaert, J.L. Demuynck, Nucl. Phys. 16 (1960) Am03 S.Y. Ambiye, R.P. Sharma, Nucl. Phys. 29 (1962) 657. [E γ, P γ, P β ] 1963Ke13 T.J. Kennett, G.L. Keech, Nucl. Instrum. Methods 24 (1963) 142. [E β, P β ] 1965Ro09 R.L. Robinson, P.H. Stelson, F.K. McGowan, J.L.C. Ford, Jr., W.T. Milner, Nucl. Phys. 74 (1965) 281. [E γ ] 1966JoZZ A.S. Johnston, G.M. Julian, Bull. Am. Phys. Soc. 11 (1966) No.3, 409. [E β, P β ] 1966Mi10 V. Middelboe, Nature 211 (1966) 283. [Half-life] 1966Ov01 V.V. Ovechkin, T.K. Ragimov, D.F. Rau, Yadern. Fiz. 4 (1966) 683; Soviet J. Nucl. Phys. 4 (1967) Fo09 H. Forest, M. Huguet, C. Ythier, C. R. Acad. Sci., Paris 264B (1967) Ra11 P.V. Rao, R.W. Fink, Nucl. Phys. A103 (1967) Vr05 J. Vrzal, E.P. Grigorev, A.V. Zolotavin, J. Liptak, V.O. Sergeev, J. Urbanets, Izvest. Akad. Nauk SSSR, Ser. Fiz. 21 (1967) 696; Bull. Acad. Sci. USSR, Phys. Ser. 31 (1968) Ha35 J. Hattula, E. Liukkonen, Ann. Acad. Sci. Fennicae, Ser. A VI, No.274 (1968). 1969Be74 E. Beck, Nucl. Instrum. Methods 76 (1969) 77. [E β ] 1969KoZW Y. Kobayashi, Japan Atomic Energy Research Institute report JAERI-1178 (1969) 21. [Half-life] 1969Od01 P. Odru, Radiochim. Acta 12 (1969) 64. [P γ ]

9 1969St03 Kl.-D. Strutz, H.-J. Strutz, A. Flammersfeld, Z. Phys. 221 (1969) Az02 T. Azuma, Y. Sato, Annual Rep. Radiat. Center Osaka Prefect. 12 (1971) Ma71 C. Marsol, O. Rahmouni, G. Ardisson, C. R. Acad. Sci., Paris 275B (1972) Ma35 C. Marsol, G. Ardisson, Rev. Roum. Phys. 18 (1973) De17 K. Debertin, U. Schotzig, K.F. Walz, H.M. Weiss, Ann. Nucl. Energy 2 (1975) 37. [P γ ] 1975Ge06 A.M. Geidelman, V.V. Ovechkin, D.F. Rau, P.I. Fedotov, Y.V. Kholnov, Izvest. Akad. Nauk SSSR, Ser. Fiz. 39 (1975) 555; Bull. Acad. Sci. USSR, Phys. Ser. 39 (1975) No.3, 76. [P γ ] 1975Hs02 S.T. Hsue, H.H. Hsu, F.K. Wohn, W.R. Western, S.A. Williams, Phys. Rev. C12 (1975) Sh25 K. Shizuma, H. Inoue, Y. Yoshizawa, Nucl. Instrum. Methods 137 (1976) 599. [E γ ] 1977Ok02 K. Okano, Y. Kawase, S. Yamada, J. Phys. Soc. Japan 43 (1977) Ka10 R. Kaur, A.K. Sharma, S.S. Sooch, N. Singh, P.N. Trehan, J. Phys. Soc. Japan 51 (1982) Ku03 H. Kumahora, H. Inoue, Y. Yoshizawa, Nucl. Instrum. Methods 206 (1983) 489. [E γ ] 1992Gr21 R.C. Greenwood, D.A. Struttmann, K.D.Watts, Nucl. Instrum. Methods Phys. Res. A317 (1992) 175. [P β ] 1993Ch32 T. Chang, S. Wang, H. Wang, B. Meng, Nucl. Instrum. Methods Phys. Res. A325 (1993) 196. [E γ ] 1996Sc06 E. Schönfeld, H. Janßen, Nucl. Instrum. Methods Phys. Res. A369 (1996) 527. [X K, X L, Auger electrons] 2000He14 R.G. Helmer, C. van der Leun, Nucl. Instrum. Methods Phys. Res. A450 (2000) 35. [Eγ] 2002Ba85 I.M. Band, M.B. Trzhaskovskaya, C.W. Nestor Jr., P.O. Tikkanen, S. Raman, At. Data Nucl. Data Tables 81 (2002) 1. [ICC] 2005Ki02 T. Kibédi, R.H. Spear, At. Data Nucl. Data Tables 89 (2005) 77. [E0 transition] 2008De09 D. De Frenne, A. Negret, Nucl. Data Sheets 109 (2008) 943. [Spin, parity, energy level, multipolarity] 2008Ki07 T. Kibédi, T.W. Burrows, M.B. Trzhaskovskaya, P.M. Davidson, C.W. Nestor Jr., Nucl. Instrum. Methods Phys. Res. A589 (2008) 202. [Theoretical ICC] 2012Wa38 M. Wang, G. Audi, A.H. Wapstra, F.G. Kondev, M. MacCormick, X. Xu, B. Pfeiffer, Chinese Physics C36 (2012) [Q value]

10 Appendix 1: Experimental and recommended gamma-ray emission energies and probabilities. Table 1. Experimental and recommended gamma-ray emission energies (kev). 1982Ka Ok Hs02 a 1973Ma St Ha Fo09 b 1967Ra11 c 1967Vr Ro09 Evaluated Recommended γ 6, (20) (2) (22) (3) (5) (10) (20) (5) γ 6, (21) (3) (5) (5) (15) (21) (4) γ 9, (27) (5) (10) (3) (6) γ 1, (8) (10) (15) (8) (2) (3) (5) (5) (2) (5) (23) d γ 7, (2) (2) (9) (3) (4) (15) (20) (6) γ 2, (9) (3) (17) (2) (3) (6) (7) (5) (9) (9) (3) γ 3, (6) (10) (3) (2) (3) (3) (5) (5) (2) (5) (6) (4) γ 10, (14) (2) (4) (3) (6) (14) (6) γ 10, (2) (2) (8) (4) (8) (20) (6) γ 17, (10) (10) (10) γ 11, (2) (2) (5) (3) (3) (20) (9) γ 4, (2) (2) (5) (5) (3) (10) (5) (20) (4) γ 12, (2) (6) (8) (10) (15) 749 (2) (20) (20) γ 9, (5) (1) (9) (2) (3) (4) (6) (5) (7) (5) (6) γ 15, (4) (20) (10) (3) (4) (9) γ 5, (6) (15) (6) (4) γ 6, (6) (1) (7) (3) (3) (4) (6) (5) (7) (6) (3) γ 16, (5) (1) (8) (3) (5) (10) (8) (7) (5) (6) γ 10, (1) (5) (19) (3) (3) (10) (6) γ 10, (5) (3) (10) (3) (3) 1114 (2) (9) (5) (6)

11 1982Ka Ok Hs02 a 1973Ma St Ha Fo09 b 1967Ra11 c 1967Vr Ro09 Evaluated Recommended γ 2, (5) (2) (6) (2) (3) (4) (6) (5) (7) (5) (3) γ 3, (4) γ 11, (2) (2) (24) (5) (15) 1148 (2) (20) (9) γ 18, (2) (20) (20) (21) γ 12, (8) (2) (9) (3) (3) 1180 (2) (5) (8) (6) γ 7, (5) (1) (6) (3) (3) (6) (8) (5) (5) (5) γ 13, (2) (3) (7) (10) (20) (8) γ 20, (2) (3) (10) (20) (20) (9) γ 21, (2) (3) (7) (5) (15) (20) (9) γ 13, (2) (3) (8) (5) (10) (20) (8) γ 22, (2) (3) (24) (5) (15) (10) (20) (8) γ 24, (3) (3) (5) (6) (3) (9) γ 24, (3) (3) (4) (3) (6) (3) (9) γ 15, (3) (3) (3) (4) (4) (3) (9) γ 8, (2) (3) (15) (3) (4) 1396 (2) (15) (16) γ 9, (6) (6) (18) (5) (6) (15) (18) (5) γ 16, (13) (2) (8) (3) (3) (6) (12) (5) 1497 (1) (8) (6) γ 27, (2) (16) (8) (16) (16) γ 6, (6) (1) (6) (2) (3) (6) (10) (5) (11) (6) (3) γ 17, (2) (6) (3) (5) (9) (20) (20)

12 1982Ka Ok Hs02 a 1973Ma St Ha Fo09 b 1967Ra11 c 1967Vr05 Evaluated Recommended γ 17, (2) (8) (5) (7) (10) (20) (9) γ 20, (3) (10) (10) (20) (3) (10) γ 20, (3) (4) (8) (3) ~ (3) (3) γ 10, (2) (3) (3) (3) (15) - ~ (20) (20) γ 11, (5) (2) (7) (2) (3) (15) (20) (5) 1765 (1) (5) (9) γ 23, (3) (7) (8) (5) (15) (3) (10) γ 24, (3) (7) (10) (20) (3) (9) γ 12, (9) (1) (7) (2) (3) (15) (20) (5) 1796 (1) (7) (5) γ 28, (2) (10) (5) (4) (20) (20) γ 26, (2) (2) (5) (5) (8) - ~ (20) (17) γ 13, (9) (2) (8) (3) (3) (15) (15) (5) (8) (7) γ 28, (4) (8) (10) (20) (4) (4) γ 14, (10) (8) (8) (8) γ 15, (8) (1) (7) (3) (3) (15) (15) (5) (23) (8) γ 30, (4) (4) (12) (10) (15) (4) (25) γ 16, (6) (2) (3) a (3) (2) (10) (20) (5) (6) (5) γ 35, (5) (5) (5) γ 17, (1) (2) (3) a (3) (6) 2194 (2) (22) (5) (10) (10) γ 10, (1) (2) (3) a (5) (8) 2243 (2) (20) (10) (10) (5) γ 19, (2) (3) (3) (5) (5) 2278 (3) (30) (20) (21)

13 1982Ka Ok Hs02 a 1973Ma St Ha Fo09 b 1967Ra11 c Evaluated Recommended γ 20, (1) (2) (3) a (8) (4) 2310 (2) (20) (9) (10) (9) γ 21, (1) (2) (3) a (3) (5) 2317 (2) (30) (9) (10) (9) γ 22, (7) (2) (3) a (3) (3) (15) (20) (5) (7) (7) γ 23, (1) (2) (3) a (3) (3) 2389 (3) (20) (5) (10) (10) γ 24, (9) (2) (3) a (3) (3) 2406 (2) (20) (5) (9) (8) γ 13, (1) (2) (3) a (3) (3) 2439 (3) (20) (5) (10) (7) γ 25, (2) (15) (10) (20) (21) γ 14, (2) (3) (3) (5) (10) (20) (20) (20) γ 26, (6) (10) (10) (10) (20) (6) (17) γ 27, (1) (3) (3) a (3) (3) 2544 (2) (20) (6) (10) (10) γ 28, (2) (3) (3) (3) (3) 2573 (5) (30) (6) (20) (20) γ 29, (2) (3) (4) (5) (7) 2650 (5) (30) b (6) (20) (20) γ 17, (3) (3) (3) (5) (3) (3) (8) γ 30, (3) (3) (3) a (5) (3) 2708 (3) (15) b (5) (3) (25) γ 32, (4) (4) (10) (6) (4) (4) γ 34, (7) (5) (10) (5) (5) γ 35, (3) (3) (5) (5) (6) (18) b (8) (3) (3) γ 20, (3) (3) (3) (5) (4) 2825 (5) (18) b (8) (3) (3) γ 36, (10) (10) (10) γ 23, (8) (5) (10) (15) - ~ b (5) (5)

14 1982Ka Ok Hs02 a 1973Ma St Ha Fo09 b 1967Ra11 c Evaluated Recommended γ 24, (3) (3) (3) (5) (8) 2920 (5) (18) b (8) (3) (3) γ 26, (3) (3) (3) (5) (6) 3038 (2) (20) b (8) (3) (3) γ 27, (4) (3) (9) (5) (10) (30) b (10) (3) (3) γ 29, (10) (13) (25) (20) (10) (10) γ 31, (5) (5) (15) - - ~3252 b (5) (5) γ 33, (7) (5) (15) (5) (7) γ 36, (14) (14) (14) γ 37, (9) (9) (9) a) For data above 2000 kev, the uncertainty was increased to a minimum of 0.3 kev. b) Only data up to the last energy calibration point of 2614 kev were taken into account in evaluation. c) Data set not used as majority of values were rejected as outliers by Chauvenet s criterion. d) Data taken from Helmer and van der Leun (2000He14).

15 Table 2. Experimental and recommended relative gamma-ray emission probabilities. E γ (kev) 1982Ka Ok Hs02 a 1975De Ma St Od Ha Vr Ra Fo Ov Am Ro Se07 Recommended (5) 3.46 (11) 3.6 (4) 3.12 (24) (20) 4.5 (5) (5) (11) (4) 0.99 (10) 0.9 (2) 1.18 (8) (8) 2.3 (6) (21) (6) 0.62 (10) 0.46 (20) (8) b (8) (23) (65) (50) 1000 (40) (6) 0.41 (4) 0.46 (3) 0.4 (3) (4) 0.41 (4) (2) (3) (3) 37.2 (33) 35.9 (72) 43 (6) 35.9 (7) 38 (2) 33.7 (27) 32 (2) 35 (7) 34 (4) 35 (3) 50 (10) (13) (7) (4) (60) 474 (24) 515 (38) 487 (6) 476 (23) 476 (15) 477 (5) 480 (10) 485 (10) 485 (10) 473 (6) (50) 470 (30) 530 (20) 481 (5) (6) 0.54 (3) 0.45 (6) 0.44 (8) (5) 0.36 (6) (3) (6) 0.27 (1) 0.24 (4) 0.31 (22) (3) 0.12 (3) (10) (10) (9) (9) (9) 0.49 (2) 0.48 (8) 0.34 (15) (6) (20) 0.75 (7) c 0.69 (20) c 0.80 (10) c <0.9 c (4) 0.32 (2) 0.33 (7) 0.34 (15) (6) (20) (20) (11) (15) 0.06 (4) (4) 0.09 (9) (3) (11) (6) 21.5 (3) 20.9 (13) 23.7 (17) 20.9 (4) 25.0 (12) 20.2 (8) 23 (1) 19.0 (12) 20 (1) 21 (1) 18.0 (25) (20) 18 (2) 35 (5) 21.2 (3) (9) (7) (10) d - - ~ (4) (9) (4) 0.65 (8) (18) (8) (3) 76.4 (15) 72.7 (44) 84 (6) 71.1 (9) 73.5 (40) 70.6 (28) 73.5 (30) 72 (4) 80 (5) 75 (4) 63 (10) (4) 90 (10) 72.6 (9) (6) 1.57 (2) 1.43 (4) 1.67 (14) (10) 1.20 (9) 1.7 (6) 1.2 (2) 1.1 (2) 1.3 (1) 2.0 (3) (9) (6) 0.29 (1) 0.24 (7) 0.26 (4) (2) 0.25 (3) (14) (6) 0.58 (1) 0.51 (9) 0.55 (5) (5) 0.40 (6) 0.62 (25) 0.45 (10) (4) (13)

16 E γ (kev) 1982Ka Ok Hs02 a 1975De Ma St Od Ha Vr Ra Fo Ov Ro12 Recommended (3) 19.8 (3) 19.2 (4) 22.0 (16) 18.6 (4) 19.3 (9) 18.7 (8) 21.5 (10) 19 (2) (1) 16.0 (25) - 24 (3) 19.4 (3) (4) e (9) 0.15 (1) (8) 0.17 (3) (2) < (10) (8) (21) (6) (1) (6) (6) 0.71 (1) 0.68 (4) 0.76 (6) (4) 0.68 (7) 1.1 (3) 0.60 (5) (1) (10) (5) 2.81 (2) 2.64 (10) 3.11 (23) (13) 2.56 (13) 2.7 (2) 2.6 (2) (2) 2.3 (3) (24) (8) (5) (4) (14) (4) (4) (9) (4) (7) (8) (24) (4) (9) (5) (8) 0.06 (3) (10) (16) (5) (8) (7) (6) (23) (8) 0.14 (6) (6) (8) 0.17 (1) (12) 0.16 (3) (1) 0.18 (6) 0.25 (10) 0.13 (10) (6) (23) (9) (7) (6) (10) (15) (12) (9) (6) (6) (24) (2) (10) (19) (9) (9) (7) (22) (2) (10) (7) (16) 0.13 (1) (10) (23) (2) 0.15 (2) (10) (10) (5) 0.06 (3) (14) (13) (4) 0.08 (2) (1) (13) (6) 1.09 (3) 1.30 (8) 1.19 (9) (8) 1.25 (6) 1.6 (1) 1.5 (5) (15) 0.99 (10) (8) (16) 0.33 (2) (4) (6) (20) (3) 8.0 (1) 7.66 (38) 8.9 (7) 7.26 (10) 7.4 (4) 7.1 (3) 7.8 (4) 8.6 (10) (5) 7.2 (8) 8.1 (3) 6.3 (5) 7.6 (4) (20) 0.09 (1) (9) (23) (2) (9)

17 E γ (kev) 1982Ka Ok Hs02 a 1973Ma St Od Ha Vr Ra Fo Ov Ro Se07 Recommended (9) (9) (8) (24) 0.06 (1) 0.08 (3) (8) (10) (6) (8) (1) 0.05 (2) (8) (3) (6) (10) (17) (5) 0.06 (3) (17) (7) (20) (6) (9) (17) 0.12 (1) 0.07 (2) 0.10 (5) (15) (6) (9) 1.68 (3) 1.34 (12) 1.62 (13) 1.20 (6) 1.13 (6) 1.3 (1) 1.4 (2) (1) 1.1 (2) 2.6 (6) 1.9 (3) 2.0 (7) 1.46 (22) (10) (11) (4) (22) (18) (15) (4) (9) (6) (15) (1) (15) f (6) g (5) 1.36 (2) 1.22 (7) 1.48 (11) 1.27 (6) 1.23 (7) 1.35 (10) 1.1 (2) (1) 0.99 (20) (22) (20) (4) (23) 0.12 (3) 0.04 (2) (5) (17) (5) (5) (22) (4) (8) < (12) (7) 0.75 (2) 0.66 (4) 0.80 (6) 0.71 (11) 0.64 (5) 0.63 (6) 0.70 (15) (6) 0.74 (8) (20) (4) (6) (2) (5) (20) (8) (5) (2) (20) (8) 1.28 (2) 1.18 (7) 1.41 (11) 1.23 (6) 1.07 (7) 1.0 (2) 1.3 (2) (1) 1.25 (20) 1.4 (6) 1.0 (2) (21) (25) (4) (3) (16) (3) 0.03 (3) (3) (5) 1.71 (3) 1.69 (9) 1.95 (16) 1.75 (15) 1.56 (11) 1.7 (2) 1.7 (2) (1) 1.8 (3) 1.5 (3) 1.3 (2) 3 (1) 1.71 (3) (5) (3) (3) (10) 0.24 (1) (13) 0.26 (3) 0.25 (2) 0.27 (3) 0.5 (2) 0.24 (6) (3) 0.26 (4) (10) (5) (3) (6) (12) 0.09 (1) (15) (10) 0.13 (2) - < (12) (4) (21) (4) (4) (11) (5) (14) (10) 0.08 (3) (10) (4)

18 E γ (kev) 1982Ka Ok Hs02 a 1973Ma St Od Ha Vr Ra Fo Ro Se07 Recommended (9) (7) (13) (26) 0.28 (2) 0.29 (2) 0.35 (5) 0.30 (6) (4) (4) (7) (9) (7) (15) (27) 0.29 (3) 0.28 (2) 0.31 (5) 0.30 (6) (4) 0.28 (3) (7) (7) 1.14 (3) 1.08 (6) 1.25 (9) 1.12 (10) 1.04 (8) 1.1 (1) 1.4 (3) (1) 1.35 (15) 1.7 (2) (3) (10) (7) 0.30 (2) (27) 0.30 (3) 0.32 (3) 0.39 (4) 0.34 (8) (4) 0.38 (4) (7) (8) 0.71 (2) 0.68 (4) 0.81 (6) 0.60 (6) 0.60 (5) 0.78 (5) 0.72 (15) (7) 0.85 (9) (20) (7) (6) (11) (25) 0.25 (2) 0.19 (2) 0.22 (5) 0.25 (8) (3) 0.29 (3) (1) (6) (21) (2) (2) (3) (21) (20) (3) (4) 0.05 (1) (3) (6) (15) (15) (7) (17) (2) (14) (8) (2) (4) (15) (10) (4) (8) (14) 0.14 (1) 0.12 (1) 0.10 (2) 0.15 (5) (2) 0.17 (3) (4) (20) (3) (4) (12) (5) (7) (10) 0.07 (3) (15) (13) (3) (20) (2) (4) (7) (5) (6) - ~ (8) (15) (20) (8) (5) (20) (22) 0.10 (1) 0.15 (2) (6) 0.31 (9) h 0.35 (4) h 0.39 (5) h 0.3 (1) h 0.3 (1) h (25) (5) (20) (24) 0.18 (2) 0.17 (2) 0.19 (5) (5) (4) (2) (2) (2) (3) (20) (5) (20) (10) (1) (10) (3) (2) (2) (8) (3) (4) (1) (16) (20) (3) (2) (4) (12) (6) (6) 0.12 (5) 0.05 (3) (2) (14) (20) (10) (4) (4) (5) (10) (10) (1) (2) < (10)

19 E γ (kev) 1982Ka Ok Hs02 a 1973Ma St Ha Vr Ra Fo09 Recommended (3) (2) (5) (7) (5) (5) 0.05 (2) (2) (13) (20) (3) (2) (6) (9) (6) (5) 0.06 (2) (2) (11) (20) (3) (2) (2) (9) (3) (7) (6) (7) (20) (10) (7) (13) - ~ (2) (6) g (5) (13) (8) (1) < (8) (5) (11) (7) (1) (7) (14) (10) (10) (9) (9) (9) a) Uncertainty of 5.1 % added in quadrature to published data. b) Sum of kev and kev gamma-ray emission probabilities. c) Sum of kev and kev gamma-ray emission probabilities. d) Gamma ray only observed in coincidence spectra. e) E0 transition, no gamma ray observed. f) Sum of kev and kev gamma-ray emission probabilities. g) Recommended data was calculated using Rajeval Technique as the two most precise data are not in agreement. h) Sum of kev and kev gamma-ray emission probabilities.