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[ascl:2103.009]
DarkEmulator: Cosmological emulation code for halo clustering statistics

Nishimichi, Takahiro; Takada, Masahiro; Takahashi, Ryuichi; Osato, Ken; Shirasaki, Masato; Oogi, Taira; Miyatake, Hironao; Oguri, Masamune; Murata, Ryoma; Kobayashi, Yosuke; Yoshida, Naoki

The cosmology code DarkEmulator calculates summary statistics of large scale structure constructed as a part of Dark Quest Project. The “dark_emulator” python package enables fast and accurate computations of halo clustering quantities. The code supports the halo mass function, halo-matter cross-correlation, and halo auto-correlation as a function of halo masses, redshift, separations and cosmological models.

[ascl:2106.030]
DM_statistics: Statistics of the cosmological dispersion measure (DM)

DM_statistics calculates the free-electron power spectrum and the cosmological dispersion measure (DM) statistics (such as its mean and variance, angular power spectrum and correlation function). The default cosmological parameters are consistent with the Planck 2015 LambdaCDM model; the cosmological model can be easily changed by editing a few lines of the C code.

[ascl:2106.031]
BiHalofit: Fitting formula of non-linear matter bispectrum

Takahashi, Ryuichi; Nishimichi, Takahiro; Namikawa, Toshiya; Taruya, Atsushi; Kayo, Issha; Osato, Ken; Kobayashi, Yosuke; Shirasaki, Masato

BiHalofit fits the matter bispectrum in the nonlinear regime calibrated by high-resolution cosmological N-body simulations of 41 cold dark matter models around the Planck 2015 best-fit parameters. The parameterization is similar to that in Halofit (ascl:1402.032). The simulation volume is sufficiently large to cover almost all measurable triangle bispectrum configurations in the universe, and the function is calibrated using one-loop perturbation theory at large scales. BiHaloFit predicts the weak-lensing bispectrum and will assist current and future weak-lensing surveys and cosmic microwave background lensing experiments.

[ascl:2307.032]
AmpF: Amplification factor for solar lensing

AmpF numerically calculates the amplification factor for solar lensing. The import parameters are the gravitational-wave frequency and the source angular position with respect to the solar center; the code outputs are the amplification factor and its geometrical-optics limit. AmpF accepts variables for several attributes and the overall amplitude of the lensing potential can be changed as needed. The method has been implemented in both C and Python.