Large-scale non-Gaussian mass function and halo bias: tests on N-body simulations

By M. Grossi, L. Verde, C. Carbone, Klaus Dolag, E. Branchini, F. Iannuzzi, S. Matarrese, L. Moscardini. 2009

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A B ST R A C T Thedescription oftheabundanceand clusteringofhalosfornon-Gaussian initialconditions has recently received renewed interest,m otivated by the forthcom ing large galaxy and clustersurveys,which can potentially yield constraintsoforderunity on thenon-Gaussianity param eter fN L.W epresenttestson N-body sim ulationsofanalyticalform ulaedescribing thehalo abundanceand clusteringfornon-Gaussian initial conditions.W e calibratethe analyticnon-Gaussian m assfunction ofM atarreseetal. (2000) and LoVerdeetal.(2008) and the analytic description ofclustering ofhalos

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Formation of Galaxy Clusters (2012, background): “…Matarrese & Verde 2008; McDonald 2008; Slosaret al. 2008; Taruya, Koyama & Matsubara 2008) and numerical studies (Desjacques, S ljak & Iliev 2009; Grossi et al. 2009; Pillepich, Porciani & Hahn 2010; Shandera, Dalal & Huterer 2011), the linear bias of collapsed objects in the models withlocal…”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, background): “…al. (2007) for an brief overview of previous work andAfshordi & Tolley (2008); Dalal et al. (2008); Desjacques et al. (2009); Fedeli et al. (2009); Grossi et al. (2009); Lam & Sheth (2009); Lo Verde et al. (2008); Maggiore & Riotto (2009); Oguri (2009); Pillepich et al. (2008); Valageas (2009)…”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “, [787, 545, 954, 807, 369, 1197, 956] and references therein) and might represent a promising tool for Euclid science.”
Large-scale bias and efficient generation of initial conditions for nonlocal primordial non-Gaussianity (2011, background): “75) on top of the standard prediction [28, 69, 70, 82].”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “N-body simulations have been used to study cluster formation under non-Gaussian initial conditions (e.g. Desjacques, Seljak & Iliev 2009; Grossi et al. 2009; Pillepich, Porciani & Hahn 2010).”
PRIMORDIAL NON-GAUSSIANITY, SCALE-DEPENDENT BIAS, AND THE BISPECTRUM OF GALAXIES (2009, background): “…et al. 2008; Matarrese & Verde 2008; Slosar et al. 2008; Afshordi & Tolley 2008; Taruya et al. 2008; McDonald 2008) and numerical (Dalal et al. 2008; Desjacques et al. 2008; Pillepich et al. 2008; Grossi et al. 2009) studies of the effects of primordial non-Gaussianity on the galaxy power spectrum.”
Probing primordial non-Gaussianity with SKA galaxy redshift surveys: a fully relativistic analysis (2014, methodology): “(4) we have used the large-scale structure (LSS) convention for defining fNL, as opposed to the CMB convention (Afshordi & Tolley 2008; Pillepich et al. 2010; Carbone et al. 2008; Grossi et al. 2009).”
Observational probes of cosmic acceleration (2012, background): “A final caveat related to the halo mass function is that primordial non-Gaussianity could alter its form (e.g., Weinberg and Cole, 1992; Dalal et al., 2008; Grossi et al., 2009; LoVerde and Smith, 2011; D’Amico et al., 2011) and thereby change the cluster abundances predicted for a given dark energy”
Primordial non-Gaussianity from the large-scale structure (2010, background): “However, while a number of numerical studies of the f loc NL model have confirmed the scaling ∆bκ(k, f loc NL) ∝ MR(k) and the redshift dependence ∝ D(z) [13, 42, 43, 98], the exact amplitude of the non-Gaussian bias correction remains somewhat debatable.”
Constraining primordial non-Gaussianity with future galaxy surveys (2011, methodology): “On the other hand, other authors use the correction √ qδc in the halo mass function and qδc in the halo bias (Grossi et al. 2009).”