Power spectrum of density fluctuations, halo abundances and clustering with primordial black holes. (arXiv:2010.06470v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_N/0/1/0/all/0/1">Nelson Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magana_J/0/1/0/all/0/1">Juan Magana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sureda_J/0/1/0/all/0/1">Joaquin Sureda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araya_I/0/1/0/all/0/1">Ignacio Araya</a>
We study the effect of dark matter (DM) being encapsulated in primordial
black holes (PBHs) on the power spectrum of density fluctuations $P(k)$; we
also look at its effect on the abundance of haloes and their clustering. We
allow the growth of Poisson fluctuations since matter and radiation equality
and study both monochromatic and extended PBH mass distributions. We present
updated monochromatic black hole mass constraints by demanding $<10%$
deviations from the $Lambda$ cold dark matter power spectrum at a scale of
$k=1$hMpc$^{-1}$. Our results show that PBHs with masses $>10^4$h$^{-1}M_odot$
are excluded from conforming all of the dark matter in the Universe. We also
apply this condition to our extended Press-Schechter (PS) mass functions, and
find that the Poisson power is scale dependent even before applying evolution,
due to the change of the mass density in PBHs with redshift, and therefore with
scale, as they start affecting the gravitational potential at different times.
We find that characteristic masses $M^*leq10^2 $h$^{-1}M_odot$ are allowed,
{leaving only two characteristic PBH mass windows of PS mass functions when
combining with previous constraints, at $M^*sim10^2$h$^{-1}M_odot$ and
$sim10^{-8}$h$^{-1}M_odot$ where all of the DM can be in PBHs. The resulting
dark matter halo mass functions within these windows are similar} to those
resulting from cold dark matter made of fundamental particles, but as soon as
the parameters produce unrealistic $P(k)$, the resulting halo mass functions
and their bias as a function of halo mass deviate strongly from the behaviour
measured in the real Universe.
We study the effect of dark matter (DM) being encapsulated in primordial
black holes (PBHs) on the power spectrum of density fluctuations $P(k)$; we
also look at its effect on the abundance of haloes and their clustering. We
allow the growth of Poisson fluctuations since matter and radiation equality
and study both monochromatic and extended PBH mass distributions. We present
updated monochromatic black hole mass constraints by demanding $<10%$
deviations from the $Lambda$ cold dark matter power spectrum at a scale of
$k=1$hMpc$^{-1}$. Our results show that PBHs with masses $>10^4$h$^{-1}M_odot$
are excluded from conforming all of the dark matter in the Universe. We also
apply this condition to our extended Press-Schechter (PS) mass functions, and
find that the Poisson power is scale dependent even before applying evolution,
due to the change of the mass density in PBHs with redshift, and therefore with
scale, as they start affecting the gravitational potential at different times.
We find that characteristic masses $M^*leq10^2 $h$^{-1}M_odot$ are allowed,
{leaving only two characteristic PBH mass windows of PS mass functions when
combining with previous constraints, at $M^*sim10^2$h$^{-1}M_odot$ and
$sim10^{-8}$h$^{-1}M_odot$ where all of the DM can be in PBHs. The resulting
dark matter halo mass functions within these windows are similar} to those
resulting from cold dark matter made of fundamental particles, but as soon as
the parameters produce unrealistic $P(k)$, the resulting halo mass functions
and their bias as a function of halo mass deviate strongly from the behaviour
measured in the real Universe.
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