Gas Heating from Spinning and Non-Spinning Evaporating Primordial Black
  Holes
  Primordial black holes (PBHs) from the early Universe constitute a viable
dark matter (DM) candidate and can span many orders of magnitude in mass. Light
PBHs with masses around $10^{15}$ g contribute to DM and will efficiently
evaporate through Hawking radiation at present time, leading to a slew of
observable signatures. The emission will deposit energy and heat in the
surrounding interstellar medium. We revisit the constraints from dwarf galaxy
heating by evaporating non-spinning PBHs and find that conservative constraints
from Leo T dwarf galaxy are significantly weaker than previously suggested.
Furthermore, we analyse gas heating from spinning evaporating PBHs. The
resulting limits on PBH DM abundance are found to be stronger for evaporating
spinning PBHs than for non-spinning PBHs.
