Log-Normal Distribution of Cosmic Voids in Simulations and Mocks

Russell, Esra; Pycke, Jean-Renaud

doi:10.3847/1538-4357/835/1/69

Cited by 6 publications

(5 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Estimates of void sizes range between 10-50 Mpc/h [40,41]. A more recent study based on the Cosmic Void Catalog discovered similar results, with most void sizes falling between 10-30 Mpc/h [42]. While the vast majority of the voids have sizes near the middle of the mentioned range, there are examples of extremely large/small voids.…”

Section: Cosmic Voidsmentioning

confidence: 65%

Chameleon Screening in Cosmic Voids

Tamošiūnas¹,

Briddon²,

Burrage³

et al. 2022

Preprint

View full text Add to dashboard Cite

A key goal in cosmology in the upcoming decade will be to form a better understanding of the accelerated expansion of the Universe. Upcoming surveys, such as the Vera C. Rubin Observatory's 10-year Legacy Survey of Space and Time (LSST), Euclid and the Square Killometer Array (SKA) will deliver key datasets required to tackle this and other puzzles in contemporary cosmology. With this data, constraints of unprecedented power will be put on different models of dark energy and modified gravity. In this context it is crucial to understand how screening mechanisms, which hide the deviations of these theories from the predictions of general relativity in local experiments, affect structure formation. In this work we approach this problem by using a combination of analytic and numerical methods to describe chameleon screening in the context of cosmic voids. We apply a finite element method code, SELCIE, to solve the chameleon equation of motion for a number of void profiles derived from observational data and simulations. The obtained results indicate a complex relationship between the properties of cosmic voids and the size of the chameleon acceleration of a test particle. We find that the fifth force on a test particle in a void is primarily related to the depth and the inner density gradient of the void. For realistic void profiles, the obtained chameleon-to-Newtonian acceleration ratios range between a φ /a Newt ≈ 10 −6 − 10 −5 . However, it should be noted that in unusually deep voids with large inner density gradients, the acceleration ratios can be significantly higher. We also discuss the optimal density profiles for detecting the fifth force in the upcoming observational surveys.

show abstract

Section: Cosmic Voidsmentioning

confidence: 65%

Chameleon Screening in Cosmic Voids

Tamošiūnas¹,

Briddon²,

Burrage³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Estimates of void sizes range between 10-50 Mpc/h [42,43]. A more recent study based on the Cosmic Void Catalog discovered similar results, with most void sizes falling between 10-30 Mpc/h [44]. While the vast majority of the voids have sizes near the middle of the mentioned range, there are examples of extremely large/small voids.…”

Section: Cosmic Voidsmentioning

confidence: 65%

Chameleon screening in cosmic voids

Tamosiunas

Briddon

Burrage

et al. 2022

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

A key goal in cosmology in the upcoming decade will be to form a better understanding of the accelerated expansion of the Universe. Upcoming surveys, such as the Vera C. Rubin Observatory's 10-year Legacy Survey of Space and Time (LSST), Euclid and the Square Killometer Array (SKA) will deliver key datasets required to tackle this and other puzzles in contemporary cosmology. With this data, constraints of unprecedented power will be put on different models of dark energy and modified gravity. In this context it is crucial to understand how screening mechanisms, which hide the deviations of these theories from the predictions of general relativity in local experiments, affect structure formation. In this work we approach this problem by using a combination of analytic and numerical methods to describe chameleon screening in the context of cosmic voids. We apply a finite element method (FEM) code, SELCIE, to solve the chameleon equation of motion for a number of void profiles derived from observational data and simulations. The obtained results indicate a complex relationship between the properties of cosmic voids and the size of the chameleon acceleration of a test particle. We find that the fifth force on a test particle in a void is primarily related to the depth and the inner density gradient of the void. For realistic void profiles, the obtained chameleon-to-Newtonian acceleration ratios range between aϕ /aNewt ≈ 10-6– 10-5. However, it should be noted that in unusually deep voids with large inner density gradients, the acceleration ratios can be significantly higher. Similarly, other chameleon models, such as f(R) Hu-Sawicki theory allow for significantly higher acceleration ratios. Given these results, we also discuss the optimal density profiles for detecting the fifth force in the upcoming observational surveys.

show abstract

“…Through more or less seeming to be Gaussian bell curves, the size distribution (see left/middle panel of the Fig. 4) more likely to be log-normal distribution resembling the void size distributions obtained from the Cosmic Void Catalog (CVC) showed in Russell 2016 andPycke 2017. Since in this study we are not aiming at confirming the accurate distribution the DT voids obey, we postpone such a precision study for future work.…”

Section: The Number Function Of Dt Voidsmentioning

confidence: 80%

Baryon Acoustic Oscillation detections from the clustering of massive halos and different density region tracers in TianNu simulation

Liu¹,

Yu²,

Yu³

et al. 2017

Preprint

View full text Add to dashboard Cite

The Baryon Acoustic Oscillations (BAO) refer to the ripples of material density in the Universe. As the most direct density tracers in the universe, galaxies have been commonly used in studies of BAO peak detection. The spatial number density of galaxies, to a certain extent, reflects the distribution of the material density of our Universe. Using galaxies as matter tracers, we can construct more overlapping empty spheres (defined as DT voids in Zhao et al. 2016; DT is the abbreviation for "Delaunay Triangulation") than the matter tracers, via Delaunay Triangulation technique. We show that their radii excellently reflect the galaxy number density round them, and they can serve as reliable different density region tracers. Using the data from an unprecedented large-scale N-body simulation "TianNu", we conduct some fundamental statistical studies and clustering analysis of the DT voids. We discuss in detail the representative features of two-point correlation functions of different DT void populations. We show that the peak, the position of which corresponds to the average radius of data samples, is the most representative feature of the two-point correlation function of the DT voids. In addition, we also construct another voids, the disjoint voids, and investigate their some statistical properties and clustering properties. And we find that the occupied space of all disjoint voids accounts for about 45% of the volume of the simulation box, regardless of the number density of mock galaxies. We also investigate the BAO detections based on different tracers, i.e. mock galaxies, low-density region tracers (void tracers), and high-density region tracers respectively. Our results show that BAO intensities (the heights of BAO peaks) detected by low/high-density region tracers are enhanced significantly compared to the BAO detection by mock galaxies, for the mock galaxy catalogue with the number density of 7.52 × 10 −5 h 3 Mpc −3 .

show abstract

Log-Normal Distribution of Cosmic Voids in Simulations and Mocks

Cited by 6 publications

References 41 publications

Chameleon Screening in Cosmic Voids

Chameleon Screening in Cosmic Voids

Chameleon screening in cosmic voids

Baryon Acoustic Oscillation detections from the clustering of massive halos and different density region tracers in TianNu simulation

Contact Info

Product

Resources

About