Angpow: a software for the fast computation of accurate tomographic power spectra


The statistical distribution of galaxies is a powerful probe to constrain cosmological models and gravity. In particular the matter power spectrum P(k)P(k) brings information about the cosmological distance evolution and the galaxy clustering together. However the building of P(k)P(k) from galaxy catalogues needs a cosmological model to convert angles on the sky and redshifts into distances, which leads to difficulties when comparing data with predicted P(k)P(k) from other cosmological models, and for photometric surveys like LSST. The angular power spectrum Cℓ(z1,z2)C_\ell(z_1,z_2) between two bins located at redshift z1z_1 and z2z_2 contains the same information than the matter power spectrum, is free from any cosmological assumption, but the prediction of Cℓ(z1,z2)C_\ell(z_1,z_2) from P(k)P(k) is a costly computation when performed exactly. The Angpow software aims at computing quickly and accurately the auto (z1=z2z_1=z_2) and cross (z1≠z2z_1 \neq z_2) angular power spectra between redshift bins. We describe the developed algorithm, based on developments on the Chebyshev polynomial basis and on the Clenshaw-Curtis quadrature method. We validate the results with other codes, and benchmark the performance. Angpow is flexible and can handle any user defined power spectra, transfer functions, and redshift selection windows. The code is fast enough to be embedded inside programs exploring large cosmological parameter spaces through the Cℓ(z1,z2)C_\ell(z_1,z_2) comparison with data. We emphasize that the Limber's approximation, often used to fasten the computation, gives wrong CℓC_\ell values for cross-correlations.Comment: Published in Astronomy & Astrophysic

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