Neutron star spins from our progenitors as a function of neutron star mass. We assume any remnant from our suite of models with a mass below 2.5 M_⊙ is a neutron star and consider only these remnants. With the Geneva models, we have studied the angular momentum coupling of different burning layers and their effect on the neutron star spin. The Geneva models with the original mild coupling produce spin periods shorter than 1 ms (not shown here, but very close to magenta triangles; see below). Some angular momentum loss in the supernova engine (e.g., magnetic coupling such as a magnetar engine) would be required to slow neutron stars down for such models to match the data. The spins are nearly the same if the coupling extends through the CO core (magenta triangles). Coupling through the helium layer (blue squares and empty red circles; different helium core definitions) and hydrogen layer (green solid circles) produces slower neutron stars. The helium-coupled models match the data (but realize that we are using rapidly rotating progenitors with no angular momentum loss during NS formation). The MESA models (not shown here) with the Tayler-Spruit dynamo produce ∼10 ms pulsars; generating spins that match fastest-spinning pulsars with rapidly spinning progenitor stars, an indication that the MESA models produce reasonable coupling results. The Fuller models (not shown here) do not produce rotating neutron stars, requiring spin-up mechanisms in the supernova engine to match the data. For comparison we also mark (with black lines) the range of two observational estimates. More details on models and observations are given in Appendix A.6.1.