BULK FLOW OF HALOS IN ΛCDM SIMULATION

Analysis of the Pangu N-body simulation validates that the bulk flow of halos follows a Maxwellian distribution with variance that is consistent with the prediction of the linear theory of structure formation. We propose that the consistency between the observed bulk velocity and theories should be examined at the effective scale of the radius of a spherical top-hat window function yielding the same smoothed velocity variance in linear theory as the sample window function does. We compared some recently estimated bulk flows from observational samples with the prediction of the ΛCDM model we used; some results deviate from expectation at a level of ∼3σ, but the discrepancy is not as severe as previously claimed. We show that bulk flow is only weakly correlated with the dipole of the internal mass distribution, that the alignment angle between the mass dipole and the bulk flow has a broad distribution peaked at ∼30°–50°, and also that the bulk flow shows little dependence on the mass of the halos used in the estimation. In a simulation of box size 1 h−1 Gpc, for a cell of radius 100 h−1 Mpc the maximal bulk velocity is >500 km s−1; dipoles of the environmental mass outside the cell are not tightly aligned with the bulk flow, but are rather located randomly around it with separation angles ∼20°–40°. In the fastest cell there is a slightly smaller number of low-mass halos; however, halos inside are clustered more strongly at scales ≳ 20 h−1 Mpc, which might be a significant feature since the correlation between bulk flow and halo clustering actually increases in significance beyond such scales.

[1]  Emilio Molina,et al.  Summary and Discussion , 2014 .

[2]  R. Nichol,et al.  The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: analysis of potential systematics , 2012, 1203.6499.

[3]  H. Feldman,et al.  Detected fluctuations in Sloan Digital Sky Survey luminous red galaxy magnitudes: bulk flow signature or systematic? , 2012 .

[4]  Robert P. Kirshner,et al.  Cosmic flows in the nearby universe from Type Ia supernovae , 2011, 1111.0631.

[5]  Detected fluctuations in SDSS LRG magnitudes: Bulk flow signature or systematic? , 2011, 1106.5791.

[6]  L. Wasserman,et al.  AN UNBIASED METHOD OF MODELING THE LOCAL PECULIAR VELOCITY FIELD WITH TYPE Ia SUPERNOVAE , 2011, 1103.1603.

[7]  E. Branchini,et al.  BULK FLOWS FROM GALAXY LUMINOSITIES: APPLICATION TO 2MASS REDSHIFT SURVEY AND FORECAST FOR NEXT-GENERATION DATA SETS , 2011, 1102.4189.

[8]  A. Nusser,et al.  THE COSMOLOGICAL BULK FLOW: CONSISTENCY WITH ΛCDM AND z ≈ 0 CONSTRAINTS ON σ8 AND γ , 2011, 1101.1650.

[9]  E. Pierpaoli,et al.  MEASURING BULK FLOW OF GALAXY CLUSTERS USING KINEMATIC SUNYAEV–ZELDOVICH EFFECT: PREDICTION FOR PLANCK , 2011, 1101.1581.

[10]  A. Kashlinsky,et al.  MEASURING THE DARK FLOW WITH PUBLIC X-RAY CLUSTER DATA , 2010, 1012.3214.

[11]  E. Pierpaoli,et al.  MEASURING THE GALAXY CLUSTER BULK FLOW FROM WMAP DATA , 2010, 1011.2781.

[12]  Edward J. Wollack,et al.  SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: SKY MAPS, SYSTEMATIC ERRORS, AND BASIC RESULTS , 2010, 1001.4744.

[13]  Subir Sarkar,et al.  Probing the anisotropic local Universe and beyond with SNe Ia data , 2010, 1011.6292.

[14]  P. Ferreira,et al.  A slight excess of large-scale power from moments of the peculiar velocity field , 2010, 1010.2651.

[15]  J. Khoury,et al.  Enhanced peculiar velocities in brane-induced gravity , 2010, 1004.2046.

[16]  M. S. Burns,et al.  SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION , 2010, 1004.1711.

[17]  D. Kocevski,et al.  A NEW MEASUREMENT OF THE BULK FLOW OF X-RAY LUMINOUS CLUSTERS OF GALAXIES , 2009, 0910.4958.

[18]  M. Hudson,et al.  Cosmic flows on 100 h−1 Mpc scales: standardized minimum variance bulk flow, shear and octupole moments , 2009, 0911.5516.

[19]  Astronomy,et al.  THE LINEARITY OF THE COSMIC EXPANSION FIELD FROM 300 TO 30, 000 km s−1 AND THE BULK MOTION OF THE LOCAL SUPERCLUSTER WITH RESPECT TO THE COSMIC MICROWAVE BACKGROUND , 2009, 0911.4925.

[20]  M. Hudson,et al.  Consistently large cosmic flows on scales of 100 h−1 Mpc: a challenge for the standard ΛCDM cosmology , 2008, 0809.4041.

[21]  K. Masters,et al.  SFI++. II. A New I-Band Tully-Fisher Catalog, Derivation of Peculiar Velocities, and Data Set Properties , 2007 .

[22]  J. Fynbo,et al.  The Velocity Field of the Local Universe from Measurements of Type Ia Supernovae , 2006, astro-ph/0612137.

[23]  A. Riess,et al.  Improved Distances to Type Ia Supernovae with Multicolor Light-Curve Shapes: MLCS2k2 , 2006, astro-ph/0612666.

[24]  T. Pham-Gia,et al.  Density of the Ratio of Two Normal Random Variables and Applications , 2006 .

[25]  Changbom Park,et al.  Power Spectrum of Cosmic Momentum Field Measured from the SFI Galaxy Sample , 2005, astro-ph/0509740.

[26]  E. Linder Cosmic growth history and expansion history , 2005, astro-ph/0507263.

[27]  V. Springel The Cosmological simulation code GADGET-2 , 2005, astro-ph/0505010.

[28]  K. Gorski,et al.  HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere , 2004, astro-ph/0409513.

[29]  R. Scoccimarro Redshift-space distortions, pairwise velocities and nonlinearities , 2004, astro-ph/0407214.

[30]  M. Chodorowski,et al.  Likelihood analysis of the Local Group acceleration revisited , 2004, astro-ph/0401195.

[31]  S. Maddox,et al.  The PSCz catalogue , 1999, astro-ph/9909191.

[32]  A. Lewis,et al.  Efficient computation of CMB anisotropies in closed FRW models , 1999, astro-ph/9911177.

[33]  I. Szapudi A New Method for Calculating Counts in Cells , 1997, astro-ph/9711221.

[34]  L. Moscardini,et al.  The Cluster Distribution as a Test of Dark Matter Models. III: The Cluster Velocity Field , 1995, astro-ph/9511066.

[35]  J. Willick,et al.  The density and peculiar velocity fields of nearby galaxies , 1995, astro-ph/9502079.

[36]  R. Cen,et al.  Probing the large scale velocity field with clusters of galaxies , 1994, astro-ph/9405075.

[37]  A. Nusser,et al.  On the prediction of velocity fields from redshift space galaxy samples , 1993, astro-ph/9309009.

[38]  A. Szalay,et al.  Bias and variance of angular correlation functions , 1993 .

[39]  A. Dekel,et al.  Cosmological Velocity-Density Relation in the Quasi-linear Regime , 1991 .

[40]  Joel R. Primack,et al.  Dynamical effects of the cosmological constant. , 1991 .

[41]  Y. Zel’dovich,et al.  The velocity of clusters of galaxies relative to the microwave background. The possibility of its measurement , 1980 .

[42]  M. Rees,et al.  Large-scale Density Inhomogeneities in the Universe , 1968, Nature.