This simulation shows the predicted gamma-ray flux from WIMP dark matter annihilation in your galaxy's halo, compared with Fermi-LAT observational limits.
Your early-type (Sa) galaxy contains 1.10 × 10¹² M☉ total mass, with dark matter comprising 90.9% of this mass. This dark matter fraction is higher than most spiral galaxies.
At 10 kpc from the galactic center, we predict a gamma-ray flux of 8.50e-22 photons/cm²/s. This flux is below the detection threshold by the Fermi-LAT telescope.
The purple line shows how the gamma-ray flux from dark matter annihilation varies with distance. Your galaxy's profile shows a steep decline, indicating a concentrated dark matter halo. This is characteristic of older, more evolved galaxies.
The red dashed line represents Fermi-LAT's detection limit. Regions where the purple line exceeds this limit (not seen in your galaxy) are potential targets for dark matter indirect detection experiments.
This analysis provides crucial constraints on dark matter particle properties. Your galaxy'sweak gamma-ray signal might indicate a less concentrated halo or different dark matter properties. These predictions can be tested against actual gamma-ray observations to validate dark matter models.