Galaxy and halo angular clustering in LCDM and Modified Gravity cosmologies. (arXiv:2204.05305v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Drozda_P/0/1/0/all/0/1">Paweł Drozda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hellwing_W/0/1/0/all/0/1">Wojciech A. Hellwing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bilicki_M/0/1/0/all/0/1">Maciej Bilicki</a>
Using a suite of $N$-body simulations we study the angular clustering of
galaxies, halos, and dark matter in $mathrm{Lambda text{CDM}}$ and Modified
Gravity (MG) scenarios. We consider two general categories of such MG models,
one is the $f(R)$ gravity, and the other is the normal branch of the
Dvali-Gabadadze-Porrati brane world (nDGP). To measure angular clustering we
construct a set of observer-frame lightcones and resulting mock sky catalogs.
We focus on the area-averaged angular correlation functions, $W_J$, and the
associated reduced cumulants, $S_Jequiv W_J/W_2^{(J-1)}$, and robustly measure
them up to the 9th order using counts-in-cells (CIC). We find that $0.15 < z <
0.3$ is the optimal redshift range to maximize the MG signal in our lightcones.
Analyzing various scales for the two types of statistics, we identify up to
20% relative departures in MG measurements from general relativity (GR), with
varying signal significance. For the case of halos and galaxies, we find that
$3$rd order statistics offer the most sensitive probe of the different
structure formation scenarios, with both $W_3$ and the reduced skewness, $S_3$,
reaching from $2sigma$ to $4sigma$ significance at angular scales $theta
sim 0.13 ^circ$. The MG clustering of the smooth dark matter field is
characterized by even stronger deviations ($stackrel{>}{{}_sim} 5sigma$)
from GR, albeit at a bit smaller scales of $thetasim0.08^circ$, where
baryonic physics is already important. Finally, we stress out that our mock
halo and galaxy catalogs are characterized by rather low surface number
densities when compared to existing and forthcoming state-of-the-art
photometric surveys. This opens up exciting potential for testing GR and MG
using angular clustering in future applications, with even higher precision and
significance than reported here.
Using a suite of $N$-body simulations we study the angular clustering of
galaxies, halos, and dark matter in $mathrm{Lambda text{CDM}}$ and Modified
Gravity (MG) scenarios. We consider two general categories of such MG models,
one is the $f(R)$ gravity, and the other is the normal branch of the
Dvali-Gabadadze-Porrati brane world (nDGP). To measure angular clustering we
construct a set of observer-frame lightcones and resulting mock sky catalogs.
We focus on the area-averaged angular correlation functions, $W_J$, and the
associated reduced cumulants, $S_Jequiv W_J/W_2^{(J-1)}$, and robustly measure
them up to the 9th order using counts-in-cells (CIC). We find that $0.15 < z <
0.3$ is the optimal redshift range to maximize the MG signal in our lightcones.
Analyzing various scales for the two types of statistics, we identify up to
20% relative departures in MG measurements from general relativity (GR), with
varying signal significance. For the case of halos and galaxies, we find that
$3$rd order statistics offer the most sensitive probe of the different
structure formation scenarios, with both $W_3$ and the reduced skewness, $S_3$,
reaching from $2sigma$ to $4sigma$ significance at angular scales $theta
sim 0.13 ^circ$. The MG clustering of the smooth dark matter field is
characterized by even stronger deviations ($stackrel{>}{{}_sim} 5sigma$)
from GR, albeit at a bit smaller scales of $thetasim0.08^circ$, where
baryonic physics is already important. Finally, we stress out that our mock
halo and galaxy catalogs are characterized by rather low surface number
densities when compared to existing and forthcoming state-of-the-art
photometric surveys. This opens up exciting potential for testing GR and MG
using angular clustering in future applications, with even higher precision and
significance than reported here.
http://arxiv.org/icons/sfx.gif
