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Most common formation channels of stellar mass black hole (BH) binaries likethe ones observed by LIGO, often assume they are assembled from the directcollapse of massive pre-supernova stars. However, it is still unclear whetherthe final mass and spin of the newly formed BH arises from the collapse of theentire stellar progenitor or just a fraction of it, given that coupling ofaccretion feedback released during BH formation to the surrounding infallingstar will inevitably lead to its ejection. If the BH is built up via diskaccretion, outflows from the center will result in residual gas ejection, thushalting the stellar collapse and reducing the amount of mass and spin that canbe accreted by the newly formed BH. Here we discuss the general properties ofBHs (mass and spin) associated with the collapse of rotating, helium starpre-supernova progenitors. When accretion feedback is included, the BH drivespowerful outflows that heat the surrounding envelope, effectively shutting downthe collapse. This gives rise to various outcomes ranging from very massive BHswith low spins, as inferred for GW150914, to lighter and faster-spinning BHs,as deduced for GW151226.

Accretion Feedback from newly-formed black holes and its implications for LIGO Sources