Weak gravitational lensing is the primary method used to detect dark matter in dwarf spheroidal galaxies. It involves measuring the distortion of light from distant galaxies as it passes through the gravitational field of the dark matter halo.

Dark matter in dwarf spheroidal galaxies is expected to be distributed in an extended halo, with a density that decreases with distance from the center of the galaxy.

The mass of a dwarf spheroidal galaxy's dark matter halo is directly proportional to the mass of the galaxy itself.

All of the above factors contribute to the challenge of detecting dark matter in dwarf spheroidal galaxies.

The Sagittarius Dwarf Spheroidal Galaxy is the closest dwarf spheroidal galaxy to the Milky Way, located approximately 50 kiloparsecs away.

Dwarf spheroidal galaxies typically have masses in the range of 10^5 - 10^6 solar masses.

Dwarf spheroidal galaxies typically have sizes in the range of 100 - 1000 light years.

Dwarf spheroidal galaxies typically have luminosities in the range of 10^3 - 10^4 solar luminosities.

Dwarf spheroidal galaxies typically have metallicities in the range of 1/100 solar.

Dwarf spheroidal galaxies typically have star formation rates in the range of 0.01 solar masses per year.

Dwarf spheroidal galaxies typically have dark matter contents of around 95%.

Cold dark matter is the primary type of dark matter candidate that is thought to exist in dwarf spheroidal galaxies.

Dark matter in dwarf spheroidal galaxies is expected to have a cuspy density profile.

Dwarf spheroidal galaxies are expected to have flat rotation curves.