Testing the lognormality of the galaxy and weak lensing convergence distributions from Dark Energy Survey maps

L. Clerkin, D. Kirk, M. Manera, O. Lahav, F. Abdalla, A. Amara, D. Bacon, C. Chang, E. Gaztañaga, A. Hawken, B. Jain, B. Joachimi, V. Vikram, T. Abbott, S. Allam, R. Armstrong, A. Benoit-Lévy, G. M. Bernstein, R. A. Bernstein, E. BertinD. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, M. Crocce, C. E. Cunha, C. B. D'Andrea, L. N. da Costa, S. Desai, H. T. Diehl, J. P. Dietrich, T. F. Eifler, A. E. Evrard, B. Flaugher, P. Fosalba, J. Frieman, D. W. Gerdes, D. Gruen, R. A. Gruendl, G. Gutierrez, K. Honscheid, D. J. James, S. Kent, K. Kuehn, N. Kuropatkin, M. Lima, P. Melchior, R. Miquel, B. Nord, A. A. Plazas, A. K. Romer, A. Roodman, E. Sanchez, M. Schubnell, I. Sevilla-Noarbe, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, A. R. Walker

Research output: Contribution to journalArticle

23 Scopus citations

Abstract

It is well known that the probability distribution function (PDF) of galaxy density contrast is approximately lognormal; whether the PDF of mass fluctuations derived from weak lensing convergence (κWL) is lognormal is less well established. We derive PDFs of the galaxy and projected matter density distributions via the counts-in-cells (CiC) method. We use maps of galaxies and weak lensing convergence produced from the Dark Energy Survey Science Verification data over 139 deg2. We test whether the underlying density contrast is well described by a lognormal distribution for the galaxies, the convergence and their joint PDF. We confirm that the galaxy density contrast distribution is well modelled by a lognormal PDF convolved with Poisson noise at angular scales from 10 to 40 arcmin (corresponding to physical scales of 3-10 Mpc). We note that as κWL is a weighted sum of the mass fluctuations along the line of sight, its PDF is expected to be only approximately lognormal. We find that the κWL distribution is well modelled by a lognormal PDF convolved with Gaussian shape noise at scales between 10 and 20 arcmin, with a best-fitting χ2/dof of 1.11 compared to 1.84 for a Gaussian model, corresponding to p-values 0.35 and 0.07, respectively, at a scale of 10 arcmin. Above 20 arcmin a simple Gaussian model is sufficient. The joint PDF is also reasonably fitted by a bivariate lognormal. As a consistency check, we compare the variances derived from the lognormal modelling with those directly measured via CiC. Our methods are validated against maps from the MICE Grand Challenge N-body simulation.

Original languageEnglish (US)
Pages (from-to)1444-1461
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Volume466
Issue number2
DOIs
StatePublished - Apr 1 2017

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Cosmology: observations
  • Gravitational lensing: weak
  • Large-scale structure of Universe

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