Precision cosmology with voids in the final BOSS data. (arXiv:2007.07895v2 [astro-ph.CO] UPDATED)

<a href="http://arxiv.org/find/astro-ph/1/au:+Hamaus_N/0/1/0/all/0/1">Nico Hamaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pisani_A/0/1/0/all/0/1">Alice Pisani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_J/0/1/0/all/0/1">Jin-Ah Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lavaux_G/0/1/0/all/0/1">Guilhem Lavaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wandelt_B/0/1/0/all/0/1">Benjamin D. Wandelt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weller_J/0/1/0/all/0/1">Jochen Weller</a>

We report novel cosmological constraints obtained from cosmic voids in the

final BOSS DR12 dataset. They arise from the joint analysis of geometric and

dynamic distortions of average void shapes (i.e., the stacked void-galaxy

cross-correlation function) in redshift space. Our model uses tomographic

deprojection to infer real-space void profiles and self-consistently accounts

for the Alcock-Paczynski (AP) effect and redshift-space distortions (RSD)

without any prior assumptions on cosmology or structure formation. It is

derived from first physical principles and provides an extremely good

description of the data at linear perturbation order. We validate this model

with the help of mock catalogs and apply it to the final BOSS data to constrain

the RSD and AP parameters $f/b$ and $D_AH/c$, where $f$ is the linear growth

rate, $b$ the linear galaxy bias, $D_A$ the comoving angular diameter distance,

$H$ the Hubble rate, and $c$ the speed of light. In addition, we include two

nuisance parameters in our analysis to marginalize over potential systematics.

We obtain $f/b=0.540pm0.091$ and $D_AH/c=0.588pm0.004$ from the full void

sample at a mean redshift of $z=0.51$. In a flat $Lambda$CDM cosmology, this

implies $Omega_mathrm{m}=0.312pm0.020$ for the present-day matter density

parameter. When we use additional information from the survey mocks to

calibrate our model, these constraints improve to $f/b=0.347pm0.023$,

$D_AH/c=0.588pm0.003$, and $Omega_mathrm{m}=0.310pm0.017$. However, we

emphasize that the calibration depends on the specific model of cosmology and

structure formation assumed in the mocks, so the calibrated results should be

considered less robust. Nevertheless, our calibration-independent constraints

are among the tightest of their kind to date, demonstrating the immense

potential of using cosmic voids for cosmology in current and future data.

We report novel cosmological constraints obtained from cosmic voids in the

final BOSS DR12 dataset. They arise from the joint analysis of geometric and

dynamic distortions of average void shapes (i.e., the stacked void-galaxy

cross-correlation function) in redshift space. Our model uses tomographic

deprojection to infer real-space void profiles and self-consistently accounts

for the Alcock-Paczynski (AP) effect and redshift-space distortions (RSD)

without any prior assumptions on cosmology or structure formation. It is

derived from first physical principles and provides an extremely good

description of the data at linear perturbation order. We validate this model

with the help of mock catalogs and apply it to the final BOSS data to constrain

the RSD and AP parameters $f/b$ and $D_AH/c$, where $f$ is the linear growth

rate, $b$ the linear galaxy bias, $D_A$ the comoving angular diameter distance,

$H$ the Hubble rate, and $c$ the speed of light. In addition, we include two

nuisance parameters in our analysis to marginalize over potential systematics.

We obtain $f/b=0.540pm0.091$ and $D_AH/c=0.588pm0.004$ from the full void

sample at a mean redshift of $z=0.51$. In a flat $Lambda$CDM cosmology, this

implies $Omega_mathrm{m}=0.312pm0.020$ for the present-day matter density

parameter. When we use additional information from the survey mocks to

calibrate our model, these constraints improve to $f/b=0.347pm0.023$,

$D_AH/c=0.588pm0.003$, and $Omega_mathrm{m}=0.310pm0.017$. However, we

emphasize that the calibration depends on the specific model of cosmology and

structure formation assumed in the mocks, so the calibrated results should be

considered less robust. Nevertheless, our calibration-independent constraints

are among the tightest of their kind to date, demonstrating the immense

potential of using cosmic voids for cosmology in current and future data.

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