COSMIC FLOW FROM TWO MICRON ALL-SKY REDSHIFT SURVEY: THE ORIGIN OF COSMIC MICROWAVE BACKGROUND DIPOLE AND IMPLICATIONS FOR LAMBDACDM COSMOLOGY

Journal Article · Wed Jan 20 00:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/709/1/483· OSTI ID:21392326

Lavaux, Guilhem; Mohayaee, Roya; Colombi, Stephane ^[1]; Tully, R Brent ^[2]

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1. Institut d'Astrophysique de Paris, UMR 7095 CNRS/Universite Pierre et Marie Curie, 98bis bd Arago (France)
2. Institute for Astronomy, University of Hawaii, Honolulu, HI (United States)

We generate the peculiar velocity field for the Two Micron All-Sky Redshift Survey (2MRS) catalog using an orbit-reconstruction algorithm. The reconstructed velocities of individual objects in 2MRS are well correlated with the peculiar velocities obtained from high-precision observed distances within 3000 km s{sup -1}. We estimate the mean matter density to be OMEGA{sub m} = 0.31 +- 0.05 by comparing observed to reconstructed velocities in this volume. The reconstructed motion of the Local Group in the rest frame established by distances within 3000 km s{sup -1} agrees with the observed motion and is generated by fluctuations within this volume, in agreement with observations. Having tested our method against observed distances, we reconstruct the velocity field of 2MRS in successively larger radii, to study the problem of convergence toward the cosmic microwave background (CMB) dipole. We find that less than half of the amplitude of the CMB dipole is generated within a volume enclosing the Hydra-Centaurus-Norma supercluster at around 40 h {sup -1} Mpc. Although most of the amplitude of the CMB dipole seems to be recovered by 120 h {sup -1} Mpc, the direction does not agree and hence we observe no convergence up to this scale. Due to dominant superclusters such as Shapley or Horologium-Reticulum in the southern hemisphere at scales above 120 h {sup -1} Mpc, one might need to go well beyond 200 h {sup -1} Mpc to fully recover the dipole vector. We develop a statistical model which allows us to estimate cosmological parameters from the reconstructed growth of convergence of the velocity of the Local Group toward the CMB dipole motion. For scales up to 60 h {sup -1} Mpc, assuming a Local Group velocity of 627 km s{sup -1}, we estimate OMEGA{sub m} h {sup 2} = 0.11 +- 0.06 and sigma{sub 8} = 0.9 +- 0.4, in agreement with WMAP5 measurements at the 1sigma level. However, for scales up to 100 h {sup -1} Mpc, we obtain OMEGA{sub m} h {sup 2} = 0.08 +- 0.03 and sigma{sub 8} = 1.0 +- 0.4, which agrees at the 1sigma to 2sigma level with WMAP5 results.

• OSTI ID: 21392326
• Journal Information: Astrophysical Journal, Vol. 709, Issue 1; Other Information: DOI: 10.1088/0004-637X/709/1/483; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ALGORITHMS
CATALOGS
CONVERGENCE
COSMOLOGY
DATA ANALYSIS
DIPOLES
DISTANCE
GALAXIES
MATTER
ORBITS
RED SHIFT
RELICT RADIATION
SOUTHERN HEMISPHERE
UNIVERSE
DOCUMENT TYPES
EARTH PLANET
ELECTROMAGNETIC RADIATION
MATHEMATICAL LOGIC
MICROWAVE RADIATION
MULTIPOLES
PLANETS
RADIATIONS