We make available some of the computer codes that we have developed in our group and with our collaborators. Enjoy!

- Cosmology Routine Library (CRL) in Fortran: Library of useful routines for cosmological quantities
**Julia code repository**- CleanCMB.jl: Algorithm to remove foreground emission and obtain clean maps of the cosmic microwave background
- Application to the simulated data of Simons Observatory’s Small Aperture Telescope (SO-SAT) and CCAT-prime’s Prime-Cam on the Fred Young Submillimeter Telescope (FYST), Section 6 of arXiv:2107.10364

- HaloMF.jl: Halo multiplicity functions needed to compute the number density of collapsed structures (halos) in the Universe
- MatterPower.jl: Linear growth factor, linear and non-linear power spectra, and variance of cosmological matter density fluctuation fields
- OmegaGrav.jl: Gravitational binding energy in large-scale structure of the Universe
- Reference: Y.-K. Chiang, R. Makiya, E. Komatsu, and B. Ménard, arXiv:2007.01679

- CleanCMB.jl: Algorithm to remove foreground emission and obtain clean maps of the cosmic microwave background
**Cosmic birefringence**- The code to reproduce the measurements of cosmic birefringence reported in arXiv:2205.13962.

**Log-normal simulations**- lognormal_galaxies: Log-normal simulation of the distribution of galaxies in real and redshift space
- Reference: A. Agrawal, R. Makiya, C.-T. Chiang, D. Jeong, S. Saito, and E. Komatsu, arXiv:1706.09195
- Applications: Interlopers, Interlopers II, Fiber assignment, Covariance matrix I, Covariance matrix II, Bispectrum, Gravitational wave sources I, Gravitational wave sources II, Gravitational wave sources III, Harmonic-space power spectrum, Galaxy-lensing cross correlation, New 2-point correlation function estimator, Constrained realisations, pylognormal, Spherical Fourier-Bessel power spectrum I, Spherical Fourier-Bessel power spectrum II, Spherical Fourier-Bessel power spectrum III, Spherical Fourier-Bessel power spectrum IV, ALFALFA, Cosmic homogeneity, Dark sirens, Line intensity mapping, BAO with blue galaxies, Wide-Angle Effects

- lognormal_lens: Log-normal simulation of the weak lensing convergence fields, which can be used to cross-correlate with the distribution of galaxies generated by lognormal_galaxies
- Reference: R. Makiya, I. Kayo, and E. Komatsu, arXiv:2008.13195
- Applications: Fiber assignment

- SIMPLE: Log-normal simulation of the line intensity mapping
- Reference: M.L. Niemeyer, J.L. Bernal, and E. Komatsu, arXiv:2307.08475
- Applications: One-point statistics

- lognormal_galaxies: Log-normal simulation of the distribution of galaxies in real and redshift space
**Codes for the auto and cross-correlation power spectra of the thermal Sunyaev-Zeldovich effect**- class_sz: Angular power spectrum of the thermal Sunyaev-Zeldovich effect, which supersedes the “szfast” code in the CRL. This code is an add-on to a public Boltzmann solver CLASS
- Reference: B. Bolliet, B. Comis, E. Komatsu, and J. F. Macías-Pérez, arXiv:1712.00788

- pysz: Python wrapper for the “szfast” code in the CRL with various improvements documented in this repository
- References: R. Makiya, S. Ando, and E. Komatsu, arXiv:1804.05008; R. Makiya, C. Hikage, and E. Komatsu, arXiv:1907.07870

- class_sz: Angular power spectrum of the thermal Sunyaev-Zeldovich effect, which supersedes the “szfast” code in the CRL. This code is an add-on to a public Boltzmann solver CLASS
**Primodial gravitational waves**- SGWBProbe: Compute sensitivity curves for detecting the primordial gravitational waves by the CMB, pulsar timing arrays (PTA) and laser interferometers
- Reference: P. Campeti, E. Komatsu, D. Poletti, and C. Baccigalupi, arXiv:2007.04241

- Spectrum Reconstructor: Web tool to compute the covariance matrix of the initial tensor power spectra in bins of wavenumbers, given observational specifications of the CMB B-mode polarisation
- Reference: T. Hiramatsu, E. Komatsu, M. Hazumi, and M. Sasaki, arXiv:1803.00176

- SGWBProbe: Compute sensitivity curves for detecting the primordial gravitational waves by the CMB, pulsar timing arrays (PTA) and laser interferometers

*Acknowledgment*

This material is based upon work supported in part by NSF under Grant AST-0807649 and PHY-0758153, NASA under Grant NNX08AL43G, and Alfred P. Sloan Research Foundation via a Sloan Fellowship. This work is also supported in part by JSPS KAKENHI Grant Number JP15H05896, JP20H05850 and JP20H05859, and the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy - EXC-2094 - 390783311.