Beta Decay and Electron Capture Stellar Rates of Heavy Nuclei.

<strong>QRPA rates: </strong>This dataset contains beta decay and electron capture rates which have been computed employing the fully microscopic proton-neutron QRPA (quasi-particle random-phase approximation) within a broad density, ρY_e = (10 - 10¹¹) [g cm^-3], and temperature, T = (1-30) [GK], grid relevant to the pre-collapse astrophysical environment (from now on referred to as stellar rates). <br> <strong>Class 1 nuclei (Global) rates: </strong>This dataset contains beta decay and electron capture (Global) stellar rates for class 1 nuclei. Class 1 contains nuclides with energy values of the first parent excitation states above 2 MeV calculated by our pn-QRPA model. Our class 1 nuclides belong to the global Brink Axcel (GBA) hypothesis category where the strength distributions of all initial excited states have been replicated only by the ground state GT distribution. <br> <strong>Class 2 nuclei (Local) rates: </strong>This dataset contains beta decay and electron capture (Local) stellar rates for class 2 nuclei. Class 2 contains nuclides, where our (pn-QRPA) model computes only one initial excited state above ground level around 1 MeV energy. In class 2 nuclides, combined GT strength distributions of the parent ground and first excited state have been replaced for all subsequent levels in the parent nucleus. We refer to class 2 as localized Brink Axcel (LBA) hypothesis. <br> <strong>Class 3 nuclei (Local) rates: </strong>This dataset contains beta decay and electron capture (Local) stellar rates for class 3 nuclei. Class 3 contains nuclides, where our (pn-QRPA) model computes several parent excited states with energies up to 1 MeV. In class 3 nuclides, combined GT strength distributions of the parent ground and multiple excited states have been replaced for all subsequent levels in the parent nucleus. We refer to class 3 as localized Brink Axcel (LBA) hypothesis. <br> <br> <br> <br>