On the Cross‐Correlation between Dark Matter Distribution and Secondary Cosmic Microwave Background Anisotropies of the Ionized Intergalactic Medium

2002 ◽  
Vol 569 (1) ◽  
pp. 8-17 ◽  
Author(s):  
Masahiro Takada ◽  
Naoshi Sugiyama
Keyword(s):  
Dark Matter ◽  
Cosmic Microwave Background ◽  
Cross Correlation ◽  
Intergalactic Medium ◽  
Matter Distribution ◽  
Microwave Background ◽  
Dark Matter Distribution ◽  
The Cross ◽  
Microwave Background Anisotropies

scholarly journals Combining Probes

2014 ◽  
Vol 10 (S306) ◽  
pp. 192-201
Author(s):  
Anaïs Rassat ◽  
François Lanusse ◽  
Donnacha Kirk ◽  
Ole Host ◽  
Sarah Bridle
Keyword(s):  
Dark Matter ◽  
Cosmological Parameters ◽  
Fundamental Aspect ◽  
Wide Field ◽  
Matter Distribution ◽  
Microwave Background ◽  
Field Surveys ◽  
Galaxy Surveys ◽  
Dark Matter Distribution ◽  
Combining Information

AbstractWith the advent of wide-field surveys, cosmology has entered a new golden age of data where our cosmological model and the nature of dark universe will be tested with unprecedented accuracy, so that we can strive for high precision cosmology. Observational probes like weak lensing, galaxy surveys and the cosmic microwave background as well as other observations will all contribute to these advances. These different probes trace the underlying expansion history and growth of structure in complementary ways and can be combined in order to extract cosmological parameters as best as possible. With future wide-field surveys, observational overlap means these will trace the same physical underlying dark matter distribution, and extra care must be taken when combining information from different probes. Consideration of probe combination is a fundamental aspect of cosmostatistics and important to ensure optimal use of future wide-field surveys.

scholarly journals Probing the Origins of Voids in the Distribution of Galaxies

2005 ◽  
Vol 22 (2) ◽  
pp. 166-173 ◽  
Author(s):  
Louise M. Ord ◽  
Martin Kunz ◽  
Hugues Mathis ◽  
Joseph Silk
Keyword(s):  
Dark Matter ◽  
Cold Dark Matter ◽  
External Source ◽  
Scientific Meeting ◽  
Acoustic Oscillations ◽  
De Sitter ◽  
Matter Distribution ◽  
Microwave Background ◽  
Sitter Background ◽  
Dark Matter Distribution

AbstractIf the voids that we see today in the distribution of galaxies existed at recombination, they will leave an imprint on the cosmic microwave background (CMB). On the other hand, if these voids formed much later, their effect on the CMB will be negligible and will not be observed with the current generation of experiments. In this paper, presented at the 2004 Annual Scientific Meeting of the Astronomical Society of Australia, we discuss our ongoing investigations into voids of primordial origin. We show that if voids in the cold dark matter distribution existed at the epoch of decoupling, they could contribute significantly to the apparent rise in CMB power on small scales detected by the Cosmic Background Imager (CBI) Deep Field. Here we present our improved method for predicting the effects of primordial voids on the CMB in which we treat a void as an external source in the cold dark matter (CDM) distribution employing a Boltzmann solver. Our improved predictions include the effects of a cosmological constant (Λ) and acoustic oscillations generated by voids at early times. We find that models with relatively large voids on the last scattering surface predict too much CMB power in an Einstein–de Sitter background cosmology but could be consistent with the current CMB observations in a ΛCDM universe.

Structure of the Polarization Field Around High Peaks of the CMB Anisotropy

1997 ◽  
Vol 06 (05) ◽  
pp. 515-533 ◽  
Author(s):  
P. Arbuzov ◽  
E. Kotok ◽  
P. Naselsky ◽  
I. Novikov
Keyword(s):  
Cosmic Microwave Background ◽  
Cross Correlation ◽  
Local Maximum ◽  
Polarization Field ◽  
Specific Structure ◽  
Microwave Background ◽  
Specific Shape ◽  
The Cross

We present computations of the statistics of the polarization field around high peaks of the cosmis microwave background anisotropy. We studied the correlated and uncorrelated with the anisotropy parts of polarization in the vicinity of isolated peaks of anisotropy in order to demonstrate how these peaks determine the structure of the polarization fields. We have shown that the level of cross-correlation between anisotropy and polarization increases in ν times around ν-heigh isolated peaks of anisotropy. Such a peak forms the specific shape of polarization around itself. The polarization of the cosmic microwave background correlated with 3σ-peaks of anisotropy is formed mainly between the cross-levels 1.5σ and 2.5σ. This polarization has a local maximum ~30÷45% around 3σ-peaks and looks like "rings" around the peaks. This specific structure of the polarization field would be effective for further investigation of the primordial signal and noise in the maps of anisotropy and polarization of the cosmic microwave background.

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