| Autor: |
Burger JD; University of Iceland, Dunhagi 5, 107 Reykjavík, Reykjavíkurborg, Iceland; Department of Physics and Astronomy, University of California, Riverside, California 92521, USA; and Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Bayern, Germany., Zavala J; University of Iceland, Dunhagi 5, 107 Reykjavík, Reykjavíkurborg, Iceland., Sales LV; Department of Physics and Astronomy, University of California, Riverside, California 92521, USA., Vogelsberger M; MIT Kavli Institute for Astrophysics and Space Research, Ronald McNair Building, 37-611, Cambridge, Massachusetts 02139, USA and The NSF AI Institute for Artificial Intelligence and Fundamental Interactions, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, Massachusetts 02139, USA., Marinacci F; Department of Physics and Astronomy 'Augusto Righi', University of Bologna, Bologna, I-40129, Italy., Torrey P; Department of Astronomy, University of Florida, 211 Bryant Space Sciences Center, Gainesville, Florida 32611, USA. |
| Abstrakt: |
Impulsive supernova feedback and nonstandard dark matter models, such as self-interacting dark matter (SIDM), are the two main contenders for the role of the dominant core formation mechanism at the dwarf galaxy scale. Here we show that the impulsive supernova cycles that follow episodes of bursty star formation leave distinct features in the distribution function of stars: groups of stars with similar ages and metallicities develop overdense shells in phase space. If cores are formed through supernova feedback, we predict the presence of such features in star-forming dwarf galaxies with cored host halos. Their systematic absence would favor alternative dark matter models, such as SIDM, as the dominant core formation mechanism. |
