Power spectrum, correlation function, and tests for luminosity bias in the CfA redshift survey

1994 ◽  
Vol 431 ◽  
pp. 569 ◽  
Author(s):  
Changbom Park ◽  
Michael S. Vogeley ◽  
Margaret J. Geller ◽  
John P. Huchra
Keyword(s):  
Correlation Function ◽  
Power Spectrum ◽  
Redshift Survey ◽  
Spectrum Correlation

Two-point Correlation Function and Power Spectrum at Very Large Scales

2005 ◽  
Vol 201 ◽  
pp. 449-450
Author(s):  
Z.-G. Deng ◽  
X.-Y. Xia
Keyword(s):  
Correlation Function ◽  
Power Spectrum ◽  
Correlation Functions ◽  
Large Scale ◽  
Wave Number ◽  
Scale Fluctuation ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey ◽  
Large Scale Fluctuation

Subsamples of galaxies with different morphological types have been sorted out from Stromlo-APM redshift survey. Two-point correlation function for each subsample has been calculated. The two-point correlation functions for all subsamples show very large scale fluctuation. We show that the two-point correlation function with fluctuation could be fitted by a modified power spectrum with power excess at wave number comparable to the scale of the fluctuation.

scholarly journals Statistical modelling of the cosmological dispersion measure

2021 ◽  
Vol 502 (2) ◽  
pp. 2615-2629
Author(s):  
Ryuichi Takahashi ◽  
Kunihito Ioka ◽  
Asuka Mori ◽  
Koki Funahashi
Keyword(s):  
Dark Matter ◽  
Correlation Function ◽  
Probability Distribution ◽  
Power Spectrum ◽  
Free Electron ◽  
Statistical Modelling ◽  
Dispersion Measure ◽  
Host Galaxies ◽  
Angular Power Spectrum ◽  
Bias Factor

ABSTRACT We have investigated the basic statistics of the cosmological dispersion measure (DM)—such as its mean, variance, probability distribution, angular power spectrum, and correlation function—using the state-of-the-art hydrodynamic simulations, IllustrisTNG300, for the fast radio burst cosmology. To model the DM statistics, we first measured the free-electron abundance and the power spectrum of its spatial fluctuations. The free-electron power spectrum turns out to be consistent with the dark matter power spectrum at large scales, but it is strongly damped at small scales (≲  Mpc) owing to the stellar and active galactic nucleus feedback. The free-electron power spectrum is well modelled using a scale-dependent bias factor (the ratio of its fluctuation amplitude to that of the dark matter). We provide analytical fitting functions for the free-electron abundance and its bias factor. We next constructed mock sky maps of the DM by performing standard ray-tracing simulations with the TNG300 data. The DM statistics are calculated analytically from the fitting functions of the free-electron distribution, which agree well with the simulation results measured from the mock maps. We have also obtained the probability distribution of source redshift for a given DM, which helps in identifying the host galaxies of FRBs from the measured DMs. The angular two-point correlation function of the DM is described by a simple power law, $\xi (\theta) \approx 2400 (\theta /{\rm deg})^{-1} \, {\rm pc}^2 \, {\rm cm}^{-6}$, which we anticipate will be confirmed by future observations when thousands of FRBs are available.

scholarly journals The Two-Dimensional Power Spectrum of the Las Campanas Redshift Survey: Detection of Excess Power on 100 [ITAL]h[/ITAL][TSUP]−1[/TSUP] Mpc Scales

1996 ◽  
Vol 456 (1) ◽  
Author(s):  
Stephen D. Landy ◽  
Stephen A. Shectman ◽  
Huan Lin ◽  
Robert P. Kirshner ◽  
Augustus A. Oemler ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Two Dimensional ◽  
Redshift Survey ◽  
Excess Power

scholarly journals Cosmological Spectrum of Two-Point Correlation Function from Vacuum Fluctuation of Stringy Axion Field in De Sitter Space: A Study of the Role of Quantum Entanglement

Universe ◽  
2020 ◽  
Vol 6 (6) ◽  
pp. 79
Author(s):  
Sayantan Choudhury ◽  
Sudhakar Panda
Keyword(s):  
Correlation Function ◽  
Power Spectrum ◽  
Quantum Entanglement ◽  
De Sitter Space ◽  
Entangled State ◽  
De Sitter ◽  
Vacuum Fluctuation ◽  
Axion Field ◽  
Point Correlation ◽  
Point Correlation Function

In this work, we study the impact of quantum entanglement on the two-point correlation function and the associated primordial power spectrum of mean square vacuum fluctuation in a bipartite quantum field theoretic system. The field theory that we consider is the effective theory of axion field arising from Type IIB string theory compacted to four dimensions. We compute the expression for the power spectrum of vacuum fluctuation in three different approaches, namely (1) field operator expansion (FOE) technique with the quantum entangled state, (2) reduced density matrix (RDM) formalism with mixed quantum state and (3) the method of non-entangled state (NES). For a massless axion field, in all three formalisms, we reproduce, at the leading order, the exact scale invariant power spectrum which is well known in the literature. We observe that due to quantum entanglement, the sub-leading terms for these thee formalisms are different. Thus, such correction terms break the degeneracy among the analysis of the FOE, RDM and NES formalisms in the super-horizon limit. On the other hand, for massive axion field we get a slight deviation from scale invariance and exactly quantify the spectral tilt of the power spectrum in small scales. Apart from that, for massless and massive axion field, we find distinguishable features of the power spectrum for the FOE, RDM, and NES on the large scales, which is the result of quantum entanglement. We also find that such large-scale effects are comparable to or greater than the curvature radius of the de Sitter space. Most importantly, in near future if experiments probe for early universe phenomena, one can detect such small quantum effects. In such a scenario, it is possible to test the implications of quantum entanglement in primordial cosmology.

scholarly journals Measuring the growth rate of structure around cosmic voids

2014 ◽  
Vol 11 (S308) ◽  
pp. 571-574
Author(s):  
A. J. Hawken ◽  
D. Michelett ◽  
B. Granett ◽  
A. Iovino ◽  
L. Guzzo
Keyword(s):  
Growth Rate ◽  
Correlation Function ◽  
Cross Correlation ◽  
Cross Correlation Function ◽  
Redshift Survey ◽  
Cosmic Voids

AbstractUsing an algorithm based on searching for empty spheres we identified 245 voids in the VIMOS Public Extragalactic Redshift Survey (VIPERS). We show how by modelling the anisotropic void-galaxy cross correlation function we can probe the growth rate of structure.

scholarly journals The Anglo-Australian Redshift Survey

1983 ◽  
Vol 104 ◽  
pp. 175-175
Author(s):  
J. Bean ◽  
G. Efstathiou ◽  
R. S. Ellis ◽  
B. A. Peterson ◽  
T. Shanks ◽  
...  
Keyword(s):  
Correlation Function ◽  
Luminosity Function ◽  
Large Scale ◽  
Peculiar Velocities ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey ◽  
Density Inhomogeneities ◽  
The Universe

The aim of the survey is to sample a relatively large, randomly chosen volume of the Universe in order to study the large-scale distribution of galaxies using the two-point correlation function, the peculiar velocities between galaxy pairs and to provide an estimate of the galaxian luminosity function that is unaffected by density inhomogeneities and Virgo infall.

scholarly journals The 2dF QSO Redshift Survey - XIV. Structure and evolution from the two-point correlation function

2005 ◽  
Vol 356 (2) ◽  
pp. 415-438 ◽  
Author(s):  
Scott M. Croom ◽  
B. J. Boyle ◽  
T. Shanks ◽  
R. J. Smith ◽  
L. Miller ◽  
...  
Keyword(s):  
Correlation Function ◽  
Point Correlation ◽  
Point Correlation Function ◽  
Redshift Survey

scholarly journals The power spectrum of galaxies in the 2dF 100k redshift survey

2002 ◽  
Vol 335 (4) ◽  
pp. 887-908 ◽  
Author(s):  
M. Tegmark ◽  
A. J. S. Hamilton ◽  
Y. Xu
Keyword(s):  
Power Spectrum ◽  
Redshift Survey

The Galaxy Correlation Function in the CNOC2 Redshift Survey: Dependence on Color, Luminosity, and Redshift

2001 ◽  
Vol 560 (1) ◽  
pp. 72-85 ◽  
Author(s):  
C. W. Shepherd ◽  
R. G. Carlberg ◽  
H. K. C. Yee ◽  
S. L. Morris ◽  
H. Lin ◽  
...  
Keyword(s):  
Correlation Function ◽  
The Galaxy ◽  
Redshift Survey
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