Exploring the cosmological synergy between galaxy cluster and cosmic void number counts. (arXiv:2210.07248v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pelliciari_D/0/1/0/all/0/1">Davide Pelliciari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contarini_S/0/1/0/all/0/1">Sofia Contarini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marulli_F/0/1/0/all/0/1">Federico Marulli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moscardini_L/0/1/0/all/0/1">Lauro Moscardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giocoli_C/0/1/0/all/0/1">Carlo Giocoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lesci_G/0/1/0/all/0/1">Giorgio Francesco Lesci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolag_K/0/1/0/all/0/1">Klaus Dolag</a>
Galaxy clusters and cosmic voids are the most extreme objects of our Universe
in terms of mass and size, tracing two opposite sides of the large-scale matter
density field. By studying their abundance as a function of their mass and
radius, respectively, i.e. the halo mass function (HMF) and void size function
(VSF), it is possible to achieve fundamental constraints on the cosmological
model. While the HMF has already been extensively exploited providing robust
constraints on the main cosmological model parameters (e.g. $Omega_{rm m}$,
$sigma_8$ and $S_8$), the VSF is still emerging as a viable and effective
cosmological probe. Given the expected complementarity of these statistics, in
this work we aim at estimating the costraining power deriving from their
combination. To achieve this goal, we exploit realistic mock samples of galaxy
clusters and voids extracted from state-of-the-art large hydrodynamical
simulations, in the redshift range $0.2 leq z leq 1$. We perform an accurate
calibration of the free parameters of the HMF and VSF models, needed to take
into account the differences between the types of mass tracers used in this
work and those considered in previous literature analyses. Then, we obtain
constraints on $Omega_{rm m}$ and $sigma_8$ by performing a Bayesian Markov
Chain Monte Carlo analysis. We find that cluster and void counts represent
powerful independent and complementary probes to test the cosmological
framework. In particular, we found that the constraining power of the HMF on
$Omega_{rm m}$ and $sigma_8$ improves drastically with the VSF contribution,
increasing the $S_8$ constraint precision by a factor of about $60%$.
Galaxy clusters and cosmic voids are the most extreme objects of our Universe
in terms of mass and size, tracing two opposite sides of the large-scale matter
density field. By studying their abundance as a function of their mass and
radius, respectively, i.e. the halo mass function (HMF) and void size function
(VSF), it is possible to achieve fundamental constraints on the cosmological
model. While the HMF has already been extensively exploited providing robust
constraints on the main cosmological model parameters (e.g. $Omega_{rm m}$,
$sigma_8$ and $S_8$), the VSF is still emerging as a viable and effective
cosmological probe. Given the expected complementarity of these statistics, in
this work we aim at estimating the costraining power deriving from their
combination. To achieve this goal, we exploit realistic mock samples of galaxy
clusters and voids extracted from state-of-the-art large hydrodynamical
simulations, in the redshift range $0.2 leq z leq 1$. We perform an accurate
calibration of the free parameters of the HMF and VSF models, needed to take
into account the differences between the types of mass tracers used in this
work and those considered in previous literature analyses. Then, we obtain
constraints on $Omega_{rm m}$ and $sigma_8$ by performing a Bayesian Markov
Chain Monte Carlo analysis. We find that cluster and void counts represent
powerful independent and complementary probes to test the cosmological
framework. In particular, we found that the constraining power of the HMF on
$Omega_{rm m}$ and $sigma_8$ improves drastically with the VSF contribution,
increasing the $S_8$ constraint precision by a factor of about $60%$.
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