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We provide a set of stellar evolution and nucleosynthesis calculations that applies established physics assumptions simultaneously to low-and intermediate-mass and massive star models. Our goal is to provide an internally consistent and comprehensive nuclear production and yield database for applications in areas such as presolar grain studies. Our non-rotating models assume convective boundary mixing (CBM) where it has been adopted before. We include 8 (12) initial masses for Z = 0.01 (0.02). Models are followed either until the end of the asymptotic giant branch phase or the end of Si burning, complemented by simple analytic core-collapse supernova (SN) models with two options for fallback and shock velocities. The explosions show which pre-SN yields will most strongly be effected by the explosive nucleosynthesis. We discuss how these two explosion parameters impact the light elements and the s and p process. For low-and intermediate-mass models, our stellar yields from H to Bi include the effect of CBM at the He-intershell boundaries and the stellar evolution feedback of the mixing process that produces the C 13 pocket. All post-processing nucleosynthesis calculations use the same nuclear reaction rate network and nuclear physics input. We provide a discussion of the nuclear production across the entire mass range organized by element group. The entirety of our stellar nucleosynthesis profile and time evolution output are available electronically, and tools to explore the data on the NuGrid VOspace hosted by the Canadian Astronomical Data Centre are introduced.

We revisit the evidence for the contribution of the long-lived radioactive nuclides 44 Ti, 55 Fe, 56 Co, 57 Co, and 60 Co to the UVOIR light curve of SN 1987A. We show that the V-band luminosity constitutes a roughly constant fraction of the bolometric luminosity between 900 and 1900 days, and we obtain an approximate bolometric light curve out to 4334 days by scaling the late time V-band data by a constant factor where no bolometric light curve data is available. Considering the five most relevant decay chains starting at 44 Ti, 55 Co, 56 Ni, 57 Ni, and 60 Co, we perform a least squares fit to the constructed composite bolometric light curve. For the nickel isotopes, we obtain best fit values of M( 56 Ni) = (7.1 ± 0.3) × 10 −2 M ⊙ and M( 57 Ni) = (4.1 ± 1.8) × 10 −3 M ⊙ . Our best fit 44 Ti mass is M( 44 Ti) = (0.55 ± 0.17)× 10 −4 M ⊙ , which is in disagreement with the much higher (3.1 ± 0.8) × 10 −4 M ⊙ recently derived from INTEGRAL observations. The associated uncertainties far exceed the best fit values for 55 Co and 60 Co and, as a result, we only give upper limits on the production masses of M( 55 Co) < 7.2 × 10 −3 M ⊙ and M( 60 Co) < 1.7 × 10 −4 M ⊙ . Furthermore, we find that the leptonic channels in the decay of 57 Co (internal conversion and Auger electrons) are a significant contribution and constitute up to 15.5% of the total luminosity. Consideration of the kinetic energy of these electrons is essential in lowering our best fit nickel isotope production ratio to [ 57 Ni/ 56 Ni] = 2.5 ± 1.1, which is still somewhat high but is in agreement with gamma-ray observations and model predictions.