It is unlikely that rapid spin played a significant role in delaying the collapse of the merging neutron stars ``GW170817'' into a black hole. The timescales for the merger and collapse of the neutron stars are determined by their masses, radii, and orbital characteristics, rather than their spin.

In the case of ``GW170817'', observations and models suggest that the primary neutron star had a mass of about 1.3 times that of the Sun, while the secondary neutron star had a mass of about 1.4 times that of the Sun. The radii of neutron stars are typically around 10 kilometers, and they orbit each other at a distance of a few hundred kilometers.

The merger and collapse of the neutron stars occurred in a matter of seconds, driven by the gravitational interactions between the two massive objects. The rapid spin of the neutron stars may have affected the details of the merger process, such as the ejection of matter and the formation of jets, but it is not expected to have significantly delayed the collapse into a black hole.

After the merger, the resulting object was a hot and dense remnant known as a ``merger remnant.'' This remnant was observed across the electromagnetic spectrum, including in the form of gamma-rays, X-rays, and visible light. The remnant eventually collapsed into a black hole due to its own gravitational pull, but this process occurred on a timescale of several seconds to minutes.

Therefore, while the rapid spin of the neutron stars may have had some influence on the merger and collapse process, it is not considered to be the main factor that delayed the collapse into a black hole in the case of ``GW170817.''