Detection of a universal core-halo transition in dwarf galaxies as predicted by Bose-Einstein dark matter. (arXiv:2010.10337v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Pozo_A/0/1/0/all/0/1">Alvaro Pozo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Broadhurst_T/0/1/0/all/0/1">Tom Broadhurst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martino_I/0/1/0/all/0/1">Ivan de Martino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiueh_T/0/1/0/all/0/1">Tzihong Chiueh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smoot_G/0/1/0/all/0/1">George F. Smoot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonoli_S/0/1/0/all/0/1">Silvia Bonoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angulo_R/0/1/0/all/0/1">Raul Angulo</a>
Most nearby classical dwarf galaxies are now known to be surrounded by large
halos of stars extending to over $2~{rm kpc}$, adding to the puzzling
properties of these dark matter dominated galaxies. Simulations of dark matter
as a Bose Einstein condensate, $psi$DM, predict large halos surrounding a
soliton core with a marked density transition at the core radius, set by the de
Broglie wavelength. This transition is a prominent hallmark of $psi$DM because
the ground state forms a standing wave soliton that is much denser than the
halo of excited states. Here we identify this predicted transition at a radius
of $simeq 1.0~{rm kpc}$ in the stellar profiles of dwarfs lying beyond the
Milky Way, corresponding to a boson mass of $m_psi simeq
1.1^{+0.2}_{-0.1}times 10^{-22}{rm eV}$, assuming stars trace the mass. Clear
transitions are also evident for most classical dwarfs that orbit the Milky
Way, with pronounced amplitudes indicating significant tidal stripping as
anticipated in $psi$DM simulations of orbiting dwarfs (Schive, Chieuh &
Broadhurst 2020), where the halo is more easily stripped than the stable
soliton core. Furthermore, the shallow slope of the observed halos accurately
matches the tidal stripping simulation. We conclude that $psi$DM accounts well
for the observed family of classical dwarf profiles with tidal stripping
included, in contrast to heavy particle, cold dark matter, CDM, where low mass
galaxies should be concentrated and core-less, quite unlike the extensive
core-halo structure observed.
Most nearby classical dwarf galaxies are now known to be surrounded by large
halos of stars extending to over $2~{rm kpc}$, adding to the puzzling
properties of these dark matter dominated galaxies. Simulations of dark matter
as a Bose Einstein condensate, $psi$DM, predict large halos surrounding a
soliton core with a marked density transition at the core radius, set by the de
Broglie wavelength. This transition is a prominent hallmark of $psi$DM because
the ground state forms a standing wave soliton that is much denser than the
halo of excited states. Here we identify this predicted transition at a radius
of $simeq 1.0~{rm kpc}$ in the stellar profiles of dwarfs lying beyond the
Milky Way, corresponding to a boson mass of $m_psi simeq
1.1^{+0.2}_{-0.1}times 10^{-22}{rm eV}$, assuming stars trace the mass. Clear
transitions are also evident for most classical dwarfs that orbit the Milky
Way, with pronounced amplitudes indicating significant tidal stripping as
anticipated in $psi$DM simulations of orbiting dwarfs (Schive, Chieuh &
Broadhurst 2020), where the halo is more easily stripped than the stable
soliton core. Furthermore, the shallow slope of the observed halos accurately
matches the tidal stripping simulation. We conclude that $psi$DM accounts well
for the observed family of classical dwarf profiles with tidal stripping
included, in contrast to heavy particle, cold dark matter, CDM, where low mass
galaxies should be concentrated and core-less, quite unlike the extensive
core-halo structure observed.
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