This is a very interesting discussion indeed. Studies done by D.A Howell in his paper: "The Type Ia Supernova Rate," Nature, 2001, which discusses the frequency of Type Ia supernovae in galaxies. I am not entirely conversant with the contents of this paper but on the other hand using a fairly simple calculation based on the rate of type 1a supernova in the milky way a fairly accurate estimate can be made of the frequency of type 1a supernovae events in the Universe:
Rate of Type Ia Supernovae in the Universe ≈ 500 years = 1 supernova per galaxy × 100 billion galaxies / 500 =200,000 supernovae per year. This seems to be extremely good news for the proponents of a Universe that is expanding at superluminal rates. While 200,000 Type Ia supernovae may occur annually in the observable Universe, not all of them will be detectable by human astronomers, and only a fraction will be observable with spectroscopic analysis.
Due to brightness and distance limitations: Supernovae in galaxies closer to us (within a few hundred million light-years) are much more likely to be detected spectroscopically than those at greater distances. For instance, supernovae in the Local Group of galaxies (including the Milky Way and nearby galaxies like Andromeda) are most likely to be observed in detail. As of recent surveys, about 50-100 Type Ia supernovae are detected spectroscopically per year in the observable Universe. This number is lower than the total number of supernovae detected (200,000) because spectroscopic follow-up requires significant resources, and not all detected supernovae are bright enough or close enough to be observed in detail.
Spectroscopic analysis is usually not the initial method used for detecting supernovae. Instead, it’s typically done after a supernova has been spotted using photometric methods (color filters). Once a transient event (like a supernova) is detected, telescopes with spectrographs follow up to obtain detailed spectra. Out of the 10-20 supernovae followed up spectroscopically, only those within a few hundred million light-years are likely to have high enough brightness and resolution for accurate validation and classification.
Typically, the number of supernovae validated spectroscopically will be lower than the initial follow-up count because many supernovae will be too faint or distant for a high-quality spectrum.
So how does this effect Dark Matter? If dark energy were not present, dark matter would represent approximately 84.4% of the total matter in the Universe.
Percentage of Dark Matter=Total Matter/Dark Matter×100 = 32/27 × 100 ≈ 84.4%
Note that using the AND Theory, the energy content would be significantly affected giving an estimate for Dark Matter as > 84.4 %