scholarly journals Testing one-loop galaxy bias: Power spectrum

2020 ◽  
Vol 102 (10) ◽  
Author(s):  
Alexander Eggemeier ◽  
Román Scoccimarro ◽  
Martin Crocce ◽  
Andrea Pezzotta ◽  
Ariel G. Sánchez
Keyword(s):  
Power Spectrum ◽  
Bias Power ◽  
Galaxy Bias

scholarly journals Testing one-loop galaxy bias: Cosmological constraints from the power spectrum

2021 ◽  
Vol 104 (4) ◽  
Author(s):  
Andrea Pezzotta ◽  
Martin Crocce ◽  
Alexander Eggemeier ◽  
Ariel G. Sánchez ◽  
Román Scoccimarro
Keyword(s):  
Power Spectrum ◽  
Cosmological Constraints ◽  
Galaxy Bias

scholarly journals Cross-correlation between cosmological and astrophysical datasets: the Planck and Herschel case

2014 ◽  
Vol 10 (S306) ◽  
pp. 202-205 ◽  
Author(s):  
Federico Bianchini ◽  
Andrea Lapi
Keyword(s):  
Power Spectrum ◽  
Cross Correlation ◽  
Forthcoming Paper ◽  
Joint Analysis ◽  
Atlas Data ◽  
Λcdm Model ◽  
The Galaxy ◽  
The Cross ◽  
Galaxy Bias ◽  
Cross Power Spectrum

AbstractWe present the first measurement of the correlation between the map of the CMB lensing potential derived from the Planck nominal mission data and z ≳ 1.5 galaxies detected by Herschel-ATLAS (H-ATLAS) survey covering about 550 deg2. We detect the cross-power spectrum with a significance of ∼ 8.5σ, ruling out the absence of correlation at 9σ. We check detection with a number of null tests. The amplitude of cross-correlation and the galaxy bias are estimated using joint analysis of the cross-power spectrum and the galaxy survey auto-spectrum, which allows to break degeneracy between these parameters. The estimated galaxy bias is consistent with previous estimates of the bias for the H-ATLAS data, while the cross-correlation amplitude is higher than expected for a ΛCDM model. The content of this work is to appear in a forthcoming paper Bianchini, et al. (2014).

scholarly journals Neutrino masses from CMB B-mode polarization and cosmic growth rate

2015 ◽  
Vol 30 (01) ◽  
pp. 1550001 ◽  
Author(s):  
Koichi Hirano
Keyword(s):  
Growth Rate ◽  
Monte Carlo ◽  
Power Spectrum ◽  
Neutrino Masses ◽  
Mcmc Method ◽  
Microwave Background ◽  
The Galaxy ◽  
Redshift Survey ◽  
Galaxy Bias ◽  
Planck Satellite

Constraints on neutrino masses are estimated based on future observations of the cosmic microwave background (CMB), which includes the B-mode polarization produced by CMB lensing from the Planck satellite, and the growth rate of cosmic structure from the Euclid redshift survey by using the Markov–Chain Monte-Carlo (MCMC) method. The error in the bound on the total neutrino mass is estimated to be Δ ∑ mν = 0.075 eV with a 68% confidence level. By using the growth rate rather than the galaxy power spectrum, accurate constraints are obtained, since the growth rate is less influenced by the uncertainty regarding galaxy bias than by the galaxy power spectrum.

scholarly journals Testing one-loop galaxy bias: Joint analysis of power spectrum and bispectrum

2021 ◽  
Vol 103 (12) ◽  
Author(s):  
Alexander Eggemeier ◽  
Román Scoccimarro ◽  
Robert E. Smith ◽  
Martin Crocce ◽  
Andrea Pezzotta ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Joint Analysis ◽  
Galaxy Bias

The on-line use of histogram data for high-speed correction and alignment of electron microscope images

1984 ◽  
Vol 42 ◽  
pp. 556-557
Author(s):  
William Krakow
Keyword(s):  
Power Spectrum ◽  
High Speed ◽  
Direct Memory Access ◽  
Digital Television ◽  
Contrast Transfer Function ◽  
The Past ◽  
High Resolution Tem ◽  
On Line ◽  
Correction Of Astigmatism ◽  
The Fourier Transform

In the past few years on-line digital television frame store devices coupled to computers have been employed to attempt to measure the microscope parameters of defocus and astigmatism. The ultimate goal of such tasks is to fully adjust the operating parameters of the microscope and obtain an optimum image for viewing in terms of its information content. The initial approach to this problem, for high resolution TEM imaging, was to obtain the power spectrum from the Fourier transform of an image, find the contrast transfer function oscillation maxima, and subsequently correct the image. This technique requires a fast computer, a direct memory access device and even an array processor to accomplish these tasks on limited size arrays in a few seconds per image. It is not clear that the power spectrum could be used for more than defocus correction since the correction of astigmatism is a formidable problem of pattern recognition.

Log-log scale roughness spectroscopy of surfaces

1993 ◽  
Vol 51 ◽  
pp. 224-225
Author(s):  
P. Fraundorf ◽  
B. Armbruster
Keyword(s):  
Power Spectrum ◽  
Autocorrelation Function ◽  
Power Spectra ◽  
Scanning Force Microscopy ◽  
Scanning Tunneling ◽  
Tunneling Microscopy ◽  
Force Microscopy ◽  
Scanning Force ◽  
Lateral Structure ◽  
Scale Roughness

Optical interferometry, confocal light microscopy, stereopair scanning electron microscopy, scanning tunneling microscopy, and scanning force microscopy, can produce topographic images of surfaces on size scales reaching from centimeters to Angstroms. Second moment (height variance) statistics of surface topography can be very helpful in quantifying “visually suggested” differences from one surface to the next. The two most common methods for displaying this information are the Fourier power spectrum and its direct space transform, the autocorrelation function or interferogram. Unfortunately, for a surface exhibiting lateral structure over several orders of magnitude in size, both the power spectrum and the autocorrelation function will find most of the information they contain pressed into the plot’s origin. This suggests that we plot power in units of LOG(frequency)≡-LOG(period), but rather than add this logarithmic constraint as another element of abstraction to the analysis of power spectra, we further recommend a shift in paradigm.

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