The Imprints of the Great-Attractor and the Virgo Cluster on the Microwave Background

Details The Imprints of the Great-Attractor and the Virgo Cluster on the Microwave Background The Imprints of the Great-Attractor and the Virgo Cluster on the Microwave Background

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.263..681s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 263, NO. 3/AUG1, P. 681, 1993

Astronomy and Astrophysics

Astronomy

25

Scientific paper

A fully non-linear model based on the Tolman-Bondi solution of the Einstein equations is used to describe the Great Attractor and the Virgo cluster. The background is a Friedmann-Robertson-Walker universe, and the inhomogeneity develops from physically motivated initial profiles of the energy density and the peculiar velocity. Accurate numerical integrations of the field equations of the null geodesics are carried out, and thus the angular temperature distribution of the microwave background produced by the chosen overdensities is found. The observer is located in the Local Group. The quadrupole Q produced by each overdensity is computed and divided into two parts: the relativistic Doppler quadrupole Q_D_ and the reduced quadrupole Q_R_ = Q - Q_D_. The three quadrupoles Q_rms_ ~5 x 10^-6^ (estimated from the COBE maps), Q_D_ and Q_R_ are compared. Even for structures as large as the Great Attractor, Q_R_ appears to be much smaller than Q_rms_ and Q_D_. The quadrupole Q_R_ produced by any observationally acceptable realization of the Great Attractor is proven to be too small to be detected in the near future.

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