TABLE XVI: Maxwellian averaged cross sections 〈 σ 〉$_{kT}$ (in mbarn) and stellar enhancement factors (f $^{∗}$) [17, 44] at p - process temperatures. TABLE XV: Comparison of Maxwellian averaged cross sections (in mbarn) at kT =30 keV. Reference $^{102}$Pd $^{120}$Te $^{130}$Ba $^{132}$Ba $^{156}$Dy Bao norm. 367 ± 17 539 ± 26 745 ± 29 394 ± 15 1653 ± 118 ENDF/B-VII.0 371 ± 17 535 ± 26 756 ± 29 398 ± 15 1616 ± 115 JEFF-3.0A 365 ± 16 – 728 ± 29 397 ± 15 1651 ± 118 JEFF-3.1 365 ± 16 540 ± 26 754 ± 29 397 ± 15 – JENDL-3.3 370 ± 17 535 ± 26 754 ± 29 397 ± 15 – Experimental data Bradley et al. [41] – – 761 ± 62 – – Beer [47] – – – – 1589 ± 145 Recommended data in compilations Bao et al. [45] 375 ± 118 a 420 ± 103 a 760 ± 110 379 ± 137 a 1567 ± 145 Allen [46] 320 400 2000 650 870 Theoretical predictions Holmes et al. [48] 247 275 397 250 1840 Harris [49] 363 776 1012 442 1637 Zhao et al. [50] 137 ± 45 293 ± 96 – 280 ± 92 850 ± 280 NON-SMOKER [17] 323 506 605 374 1190 MOST [19] b 665 307 490 227 2126 a Semi-empirical estimates. b Includes unspecified stellar enhancement factors. kT [keV] 170 215 260 $^{102}$Pd ENDF/B-VII.0 191 ± 9 177 ± 8 168 ± 8 JEFF-3.0A/3.1 164 ± 7 151 ± 7 141 ± 6 JENDL-3.3 192 ± 9 182 ± 8 173 ± 8 f ∗ [17] 1.11 1.19 1.27 $^{120}$Te ENDF/B-VII.0 / JENDL-3.3 311 ± 15 296 ± 14 284 ± 14 JEFF-3.1 304 ± 15 291 ± 14 281 ± 14 f ∗ [17] 1.10 1.18 1.25 $^{130}$Ba ENDF/B-VII.0 505 ± 20 500 ± 20 503 ± 20 JEFF-3.0A 323 ± 20 280 ± 20 248 ± 20 JEFF-3.1/JENDL-3.3 504 ± 20 499 ± 20 501 ± 20 f ∗ [17] 1.23 1.35 1.42 $^{132}$Ba Evaluations 258 ± 10 254 ± 10 253 ± 10 f ∗ [17] 1.16 1.23 1.28 $^{156}$Dy ENDF/B-VII.0 819 ± 58 772 ± 55 738 ± 53 JEFF-3.0A 895 ± 64 841 ± 60 802 ± 57 f ∗ [17] 1.50 1.55 1.56 dictions which are implicitly contained in the databases (see the discussion in Sec. VI B) and this way entering our extrapolation. Therefore, Fig. 4 also illustrates the necessity for cross section measurements with the time-of-flight method over a wider energy range from the resonance region up to about 1 MeV, in particular for nuclei involved in the p -process network. Unfortunately, this will be hard to achieve, mostly because isotopically pure samples of the rare p -isotopes are difficult to obtain. The (n, γ ) cross sections of the p -isotopes $^{102}$Pd, $^{120}$Te, 130 , $^{132}$Ba, and $^{156}$Dy have been measured in a quasi- stellar neutron spectrum corresponding to a thermal en- ergy of kT = 25 keV by means of the activation tech- nique. The results for $^{102}$Pd, $^{120}$Te, and $^{132}$Ba repre- sent the first experimental data, thus replacing rather uncertain theoretical predictions. For $^{130}$Ba and $^{156}$Dy the previously available experimental information could be significantly extended and improved. The measured cross sections were converted into Maxwellian averaged cross sections for a range of thermal energies between kT = 5 and 100 keV, and further extrapolated to the temperature region of the p -process. The extrapolation still relies on theory and this underscores the necessity for future measurements covering a wider energy range. VII. SUMMARY AND OUTLOOK 12