Reconstructed density and velocity fields from the 2MASS redshift survey

By P. Erdoğdu, Ofer Lahav, J. Huchra, M. Colless, R. Cutri, Emilio E. Falco, T. George, Thomas H. Jarrett, D. Jones, Lucas Macri and 6 more. 2006

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We present the reconstructed real-space density and the predicted velocity fields from the Two-Micron All-Sky Redshift Survey (2MRS). The 2MRS is the densest all-sky redshift survey to date and includes about 23 200 galaxies with extinction-corrected magnitudes brighter than Ks= 11.25 . Our method is based on the expansion of these fields in Fourier–Bessel functions. Within this framework, the linear redshift distortions only affect the density field in the radial direction and can easily be deconvolved using a distortion matrix. Moreover, in this coordinate system, the velocity field is related to the density field by a simple linear transformation. The shot noise errors in the reconstructions are suppressed by means of a Wiener filter which yields a minimum variance estimate of the density and velocity fields. Using the reconstructed real-space density fields, we identify all major superclusters and voids. At 50 h^−1 Mpc , our reconstructed velocity field indicates a backside infall to the Great Attractor region of vinfall= (491 ± 200) (β/0.5) km s^−1 in the Local Group frame and vinfall= (64 ± 205) (β/0.5) km s^−1 in the cosmic microwave background (CMB) frame and β is the redshift distortion parameter. The direction of the reconstructed dipole agrees well with the dipole derived by Erdogdu et al. The misalignment between the reconstructed 2MRS and the CMB dipoles drops to 13° at around 5000 km s^−1 but then increases at larger distances.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7238a2e5be261bb743a72e73b88d39faeea9edb4

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Citations in the corpus

SFI++. II. A New I-Band Tully-Fisher Catalog, Derivation of Peculiar Velocities, and Data Set Properties (2007, methodology): “Further, in order to account for the inhomogeneous Malmquist bias resulting from large-scale structure, we convolve these probability distributions with the density field reconstructed from the 2MRS (Erdogdu et al. 2006), provided to us by Pirin Erdogdu.”
Groups of Galaxies in the Two Micron All Sky Redshift Survey (2006, background): “We first compute the virial mass of the group, MV , MV = 3π 2 ∑2 PRP G (6) where G is Newton’s constant, σP is the projected velocity dispersion, σ2P = ∑ i(Vi − VG) 2 N − 1 (7) and RP is the projected virial radius, RP = N(N − 1) ∑ i>j R −1 ij (8) 9 See Crook et al. (2007b), in preparation.”
THE EXTRAGALACTIC DISTANCE DATABASE (2009, background): “There are outstanding plots of the distribution of the 2MASS sample in Erdoğdu et al. (2006b).”
The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures (2009, methodology): “Erdogdu et al. (2006a) have used spherical harmonics and Wiener filtering to decompose the density and velocity field of the shallower 2MRS.”
The 2M++ galaxy redshift catalogue (2011, methodology): “It is already possible with currently available data to build a redshift catalogue significantly deeper than previous full-sky galaxy redshift catalogues like PSCz (Saunders et al. 2000) or the Two-Micron-All-Sky Redshift Survey (Huchra et al. 2005; Erdoğdu et al. 2006a; Huchra et al. 2011, 2MRS).”
THE ARECIBO LEGACY FAST ALFA SURVEY: THE α.40 H i SOURCE CATALOG, ITS CHARACTERISTICS AND THEIR IMPACT ON THE DERIVATION OF THE H i MASS FUNCTION (2011, methodology): “However, other options exist, in particular other PSCz maps (smoothed to different levels) and the density reconstruction derived from the 2MASS Redshift Survey (2MRS; Erdogdu et al. (2006)).”
Local gravity versus local velocity: solutions for β and non-linear bias (2010, methodology): “The 2MRS has previously been used to address the gravity field in considerable detail (e.g. Erdoğdu et al. 2006a; Feldman, Hudson & Watkins 2008), and some effort has gone into the comparison of the 2MRS-predicted velocities versus the SFI++ measured velocities, in particular by Pike & Hudson…”
Approaches to understanding cosmic acceleration (2009, background): “Peculiar velocity surveys typically use redshift-independent distance indicators to separate the Hubble flow from the local flow, and nearby SNeIa are therefore good candidates; a number of surveys, like the 6dFGS [222] and the 2MRS [223], use galaxies.”
Our Peculiar Motion Away from the Local Void (2007, methodology): “The debate continues regarding the relative importance of these structures on our motion (Kocevski & Ebeling 2006; Erdoğdu et al. 2006a).”
THE SPIN AND ORIENTATION OF DARK MATTER HALOS WITHIN COSMIC FILAMENTS (2009, background): “Indeed, some recent studies are devoted to density field reconstructions based on galaxy and halo distributions (e.g. Erdogdu et al. 2006 from 2MASS Redshift Survey; and Wang et al. 2009a from halo distribution in simulations).”
THE 2MASS REDSHIFT SURVEY—DESCRIPTION AND DATA RELEASE (2011, methodology): “• Erdoğdu et al. (2006b) calculated density and velocity fields.”
Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field (2014, methodology): “Inclusion of this residual bulk flow with the predicted motion of the LG arising from 2M++ results in a total predicted motion of 656 ± 47 km s−1 in the direction l = 277◦ ± 4◦, b = 32◦ ± 6◦, in even better agreement with both the amplitude and direction of the motion as inferred from the temperatur”