Dietz, M.Lederer-Woods, C.Aberle, O.Andrzejewski, J.Audouin, L.Bacak, M.Balibrea, J.Barbagallo, M.Bečvář, F.Berthoumieux, E.Billowes, J.Bosnar, D.Brown, A.Caamaño, M.Calviño, F.Calviani, M.Cano-Ott, D.Cardella, R.Casanovas, A.Cerutti, F.Chen, Y. H.Chiaveri, E.Colonna, N.Cortés, G.Cortés-Giraldo, M. A.Cosentino, L.Damone, L. A.Diakaki, M.Domingo-Pardo, C.Dressler, R.Dupont, E.Durán, I.Fernández-Domínguez, B.Ferrari, A.Ferreira, P.Finocchiaro, P.Furman, V.Göbel, K.García, A. R.Garg, R.Gawlik, A.Gilardoni, S.Glodariu, T.Gonçalves, I. F.González-Romero, E.Griesmayer, E.Guerrero, C.Gunsing, F.Harada, H.Heinitz, S.Heyse, J.Jenkins, D. G.Jericha, E.Käppeler, F.Kadi, Y.Kahl, D.Kalamara, A.Kavrigin, P.Kimura, A.Kivel, N.Kokkoris, M.Krtička, M.Kurtulgil, D.Leal-Cidoncha, E.Leeb, H.Lerendegui-Marco, J.Lo Meo, S.Lonsdale, S. J.Macina, D.Marganiec, J.Martínez, T.Masi, A.Massimi, C.Mastinu, P.Mastromarco, M.Maugeri, E. A.Mazzone, A.Mendoza, E.Mengoni, A.Milazzo, P. M.Mingrone, F.Musumarra, A.Negret, A.Nolte, R.Oprea, A.Patronis, N.Pavlik, A.Perkowski, J.Porras, I.Praena, J.Quesada, J. M.Radeck, D.Rauscher, T.Reifarth, R.Rubbia, C.Ryan, J. A.Sabaté-Gilarte, M.Saxena, A.Schillebeeckx, P.Schumann, D.Sedyshev, P.Smith, A. G.Sosnin, N. V.Stamatopoulos, A.Tagliente, G.Tain, J. L.Tarifeño-Saldivia, A.Tassan-Got, L.Valenta, S.Vannini, G.Variale, V.Vaz, P.Ventura, A.Vlachoudis, V.Vlastou, R.Wallner, A.Warren, S.Weiss, C.Woods, P. J.Wright, T.Žugec, P.2025-12-312025-12-312101-6275https://hdl.handle.net/1885/733797628The slow neutron capture process (s-process) is responsible for producing about half of the elemental abundances heavier than iron in the universe. Neutron capture cross sections on stable isotopes are a key nuclear physics input for s-process studies. The 72Ge(n, γ) cross section has an important influence on production of isotopes between Ge and Zr during s-process in massive stars and therefore experimental data are urgently required. 72Ge(n, γ) was measured at the neutron time-of-flight facility n-TOF (CERN) for the first time at stellar energies. The measurement was performed using an enriched 72GeO2 sample at a flight path of 185m with a set of liquid scintillation detectors (C6D6). The motivation, experiment and current status of the data analysis are reported.This work was supported by the Adolf Messer Foundation, by the Austrian Science Fund FWF (J 3503), the Science and Technology Facilities Council UK (ST/M006085/1), and the European Reseach Council ERC-2015-STG Nr. 677497.enPublisher Copyright: © The Authors, published by EDP Sciences, 2018.2018-06-2910.1051/epjconf/20171840200585051043923