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Astrophysics Source Code Library

Making codes discoverable since 1999

Searching for codes credited to 'Eisenstein, Daniel J.'

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Found 3 codes.

[ascl:2105.014] encore: Efficient isotropic 2-, 3-, 4-, 5- and 6-point correlation functions
encore (Efficient N-point Correlator Estimation) estimates the isotropic NPCF multipoles for an arbitrary survey geometry in O(N2) time, with optional GPU support. The code features support for the isotropic 2PCF, 3PCF, 4PCF, 5PCF and 6PCF, with the option to subtract the Gaussian 4PCF contributions at the estimator level. For the 4PCF, 5PCF and 6PCF algorithms, the runtime is dominated by sorting the spherical harmonics into bins, which has complexity O(N_galaxy x N_bins3 x N_ell5) [4PCF], O(N_galaxy x N_bins4 x N_ell8) [5PCF] or O(N_galaxy x N_bins5 x N_ell11) [6PCF]. The higher-point functions are slow to compute unless N_bins and N_ell are small.
[ascl:2005.020] HIPSTER: HIgh-k Power Spectrum EstimatoR
HIPSTER (HIgh-k Power Spectrum EstimatoR) computes small-scale power spectra and isotropic bispectra for cosmological simulations and galaxy surveys of arbitrary shape. The code computes the Legendre multipoles of the power spectrum, P(k), or bispectrum B(k1,k2), by computing weighted pair counts over the simulation box or survey, truncated at some maximum radius. The code can be run either in 'aperiodic' or 'periodic' mode for galaxy surveys or cosmological simulations respectively. HIPSTER also supports weighted spectra, for example when tracer particles are weighted by their mass in a multi-species simulation. Generalization to anisotropic bispectra is straightforward (and requires no additional computing time) and can be added on request.
[ascl:1509.007] pycola: N-body COLA method code
pycola is a multithreaded Python/Cython N-body code, implementing the Comoving Lagrangian Acceleration (COLA) method in the temporal and spatial domains, which trades accuracy at small-scales to gain computational speed without sacrificing accuracy at large scales. This is especially useful for cheaply generating large ensembles of accurate mock halo catalogs required to study galaxy clustering and weak lensing. The COLA method achieves its speed by calculating the large-scale dynamics exactly using LPT while letting the N-body code solve for the small scales, without requiring it to capture exactly the internal dynamics of halos.