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Modern models of s-process nucleosynthesis in stars require stellar reactionrates with high precision. Most of the neutron capture cross sections in thes-process have been measured and for an increasing number of reactions therequired precision is achieved. This does not necessarily mean, however, thatthe stellar rates are constrained equally well because only capture on theground state of a target is measured in the laboratory. Captures on excitedstates can considerably contribute to stellar rates already at typicals-process temperatures. We show that the ground state contribution X to astellar rate is the relevant measure to identify reactions which are or couldbe well constrained by experiments and apply it to (n,gamma) reactions in thes-process. It is further shown that the maximally possible reduction inuncertainty of a rate through determination of the g.s. cross section isdirectly given by X. An error analysis of X is presented and it is found that Xis a robust measure with overall small uncertainties. Several specific examples(neutron capture on 79Se, 95Zr, 121Sn, 187Os, and 193Pt) are discussed indetail. The ground state contributions for a set of 411 neutron capturereactions around the s-process path are presented in a table. This allows toidentify reactions which may be better constrained by experiments and suchwhich cannot be constrained by only measuring ground state cross sections (andthus require supplementary studies). General trends and implications arediscussed.

Opportunities to constrain astrophysical reaction rates for the s-process through determination of the ground state cross sections