EIICHIRO KOMATSU

Miscellaneous 

• Playing With A Differential Equation
• Interpolating Numerical Data

Geometry

• Proper Luminosity Distance, D_L(z)
• Proper Angular Diameter Distance, D_A(z)
• Volume, V(z)

Fluctuation

• Growth Factor of Linear Density Fluctuations, g(z)=D(z)(1+z), and Derivative, dg/dlna(z)
• Evolve the Linear Matter Power Spectrum
• R.m.s. Mass Fluctuation, sigma(R)
• Non-linear Mass, M_*
• Fractional Error on the Mean Density of Galaxies in a Given Survey Volume

Power Spectrum

• Linear Power Spectrum with No Baryonic Acoustic Oscillation
• Non-linear Power Spectrum of Matter Density Fluctuations from 3rd-order Perturbation Theory, P_dd(k)
• Non-linear Power Spectrum of Velocity Divergence Fields from 3rd-order Perturbation Theory, P_tt(k)
• Non-linear Power Spectrum of Density-Velocity Divergence Cross Correlation from 3rd-order Perturbation Theory, P_dt(k)
• Two-point Correlation Function from 3rd-order Perturbation Theory, xi(R)
• Spherically Averaged Power Spectrum from 3rd-order Perturbation Theory, P(k)
• Galaxy Power Spectrum with Non-linear Bias in Real Space from 3rd-order Perturbation Theory, P_galaxy(k)
• Non-linear Power Spectrum of Matter Density Fluctuations from Empirical Fitting Formulae: Peacock&Dodds 1996; Ma et al. 1999; and Halofit [Smith et al. 2003]
• Redshift Derivative, dlnP(k,z)/dz, of Non-linear Power Spectrum of Matter Density Fluctuations from Empirical Fitting Formulae: Peacock&Dodds 1996; Ma et al. 1999; and Halofit [Smith et al. 2003]
• Redshift Derivative, dlnP(k,z)/dz, of Non-linear Power Spectrum of Matter Density Fluctuations from 3rd-order Perturbation Theory

Mass Function

• Press-Schechter Mass Function, dn_PS/dM
• Sheth-Tormen Mass Function, dn_ST/dM
• Jenkins et al. Mass Function, dn_Jenkins/dM
• Tinker et al. Mass Function, dn_Tinker/dM Without Redshift Evolution Factors
• Tinker et al. Mass Function, dn_Tinker/dM With Redshift Evolution Factors
• Sheth-Tormen Bias Parameters, b₁, b₂ and b₃
• Collapse Fraction (Press-Schechter)
• Collapse Fraction (Sheth-Tormen)

Fisher Matrix

• Fisher Matrix for the Angular Diameter Distance and the Hubble Expansion Rate from a Cosmic-variance Limited Galaxy Survey
• Fisher Matrix for the Angular Diameter Distance and the Hubble Expansion Rate from a Realistic Galaxy Survey
• Fisher Matrix for the Angular Diameter Distance and the Hubble Expansion Rate from a Realistic Galaxy Survey (Real Space Only)
• Fisher Matrix for the Angular Diameter Distance and the Hubble Expansion Rate from a Realistic Galaxy Survey, Using Information of Baryon Acoustic Oscillations (BAOs) Only
• Fisher Matrix for the Angular Diameter Distance and the Hubble Expansion Rate from a Realistic Galaxy Survey, Using Information of Baryon Acoustic Oscillations (BAOs) Only (Real Space Only)

Non-Gaussianity

• Radiation Transfer Function of Temperature, g_Tl(k), and Polarization, g_Pl(k)
• alpha_l(r) and beta_l(r) for the Local-form Bispectrum of Cosmic Microwave Background
• Full-sky, Cosmic-variance Only 1-sigma Error on the Local-form fNL [Gaussian covariance matrix]
• Cross-power spectrum of CMB lensing potential and the linear Integrated Sachs-Wolfe effect, Q_linear(l)
• Cross-power spectrum of CMB lensing potential and the Rees-Sciama effect, Q_non-linear(l), from the 3rd-order Perturbation Theory
• Cross-power spectrum of CMB lensing potential and the Rees-Sciama effect, Q_non-linear(l), from Empirical Fitting Formulae: Peacock&Dodds 1996; Ma et al. 1999; and Halofit [Smith et al. 2003]
• Chi² Differences for the Lensing-ISW and the Lensing-RS Bispectra [Gaussian covariance matrix]
• Contamination of the Local-form fNL due to the lensing-ISW and lensing-RS Bispectra [Gaussian covariance matrix]
• Chi² for the Lensing-Temperature Cross-power Spectrum

Reionization

• Nebular Spectrum, L_nu(Q_H)
• Near Infrared Background nu*I_nu (PopIII, Salpeter, SFR=1)
• Near Infrared Background nu*I_nu (PopIII, Salpeter)

Neutrino

• Massless Neutrino Perturbation
• Massive Neutrino Perturbation

Clusters of Galaxies

• Converting Virial Mass to Overdensity Mass
• Gas Pressure and Sunyaev-Zel'dovich Effect Profiles (Arnaud et al.)
• Fourier Transform of the Sunyaev-Zel'dovich Effect Profile (Arnaud et al.)
• Power Spectrum of the Sunyaev-Zel'dovich Effect (Arnaud et al.)
• Gas Pressure and Sunyaev-Zel'dovich Effect Profiles (Komatsu-Seljak)
• Fourier Transform of the Sunyaev-Zel'dovich Effect Profile (Komatsu-Seljak)
• Power Spectrum of the Sunyaev-Zel'dovich Effect (Komatsu-Seljak)
• Power Spectrum of the Sunyaev-Zel'dovich Effect (Self-similar Arnaud et al., as in Shaw et al. 2010)
• Gas Pressure and Sunyaev-Zel'dovich Effect Profiles (Planck 2013)
• Power Spectrum of the Sunyaev-Zel'dovich Effect (Planck profile and parameters, as in Dolag et al. 2015)
• Mean Compton Y (Planck profile and parameters, as in Dolag et al. 2015)
• Gas Pressure and Sunyaev-Zel'dovich Effect Profiles (Battaglia et al.)
• Mean Compton Y (Battaglia et al. profile and WMAP9 parameters, as in Hill et al. 2015)
• Bin-integrated PDF of Compton Y (Planck profile and Magneticum parameters, as in Dolag et al. 2015)
• Electron density, X-ray temperature, and electron pressure profiles of Vikhlinin's low-z sample
• Sunyaev-Zel'dovich Effect profiles of Vikhlinin's low-z sample

Analysis of Cosmic Microwave Background Maps

• MASTER Algorithm to Deconvolve the Power Spectrum for the Effect of a Mask [unbinned - suitable for a near-full-sky analysis]
  
• MASTER Algorithm to Deconvolve the Power Spectrum for the Effect of a Mask [binned l(l+1)cl/twopi - suitable for CMB analysis on a small fraction of the sky]
  
• MASTER Algorithm to Deconvolve the Power Spectrum for the Effect of a Mask [binned cl - suitable for Poisson-dominated sources as such Gamma-ray data]
  
• Secondary Parameter Code Used for WMAP 5-year and 7-year Papers