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tokens: CMB temperature maps for the low multipole l from other independent observations? If the answer is yes, then the reconstructed temperature map may be used to determine whether the anomalies are primordial or systematic. CMB polarization is one of the candidates. Due to the poor correlation coefficients (less than 0.5 for multipole l = 2 and l = 3), however, the reconstruction from only CMB polarization cannot achieve our goal. The scattering of CMB photons in clusters of galaxies may shed light on this attempt. The scattering of CMB photons in clusters of galaxies induces a polarization signal, which is determined by the quadrupole anisotropy in the photon distribution at the cluster location (Sazonov Sunyaev 1999 ). Therefore, the remote quadrupole in distant clusters, in principle, is investigable by the measurements of this induced polarization signal. The measurements of these signals were originally proposed to suppress the cosmic variance uncertainty (Kamionkowski Loeb 1997 ; Portsmouth 2004 ; Bunn 2006 ). Moreover, the magnitude of these signals gives some clues about the evolution of the CMB quadrupole to probe the dark energy. Of particular interest here is that it probes three-dimensional information of potential fluctuations around our last scattering surface (Seto Sasaki 2000 ). Even though this induced polarization in galaxy clusters has not been observed, its detection contains rich information for the study of cosmology. In this Letter, we propose an independent observation for the study of the CMB anomalies. We explore a practically useful cosmological probe from the measurements of remote quadrupole: the reconstruction of CMB temperature anisotropies for low multipole. Provided by the strong correlation of the remote quadrupole in low redshifts with the local CMB (Hall Challinor 2014 ), the reconstructed CMB temperature anisotropies are accurate enough for distinguishing the sources of low-quadrupole and axis-of-evil problems. 2 SIMULATIONS OF CMB SKY AND CMB INDUCED POLARIZATION IN DISTANT GALAXY CLUSTERS The CMB temperature anisotropies and E -mode polarization from a single plane wave can be written as (Ma Bertschinger 1995 ) where P l is Legendre polynomial, Δ Xl is the transfer function with X = T, E for temperature anisotropies and E -mode polarization, respectively. To compute the spherical harmonics coefficients of the temperature anisotropy and E -mode polarization a X,lm and some derivations later, we need the additional theorem of the spin-weighted spherical harmonics (Ng Liu 1999 ) where α, β and γ are the Euler angles as being composed of a rotation α around , followed by β around the new and finally γ around . Then, the spherical harmonics coefficients are On the other hand, the polarization effect in the distant clusters of galaxies arises from the presence of the quadrupole component of the CMB in the rest frame of a cluster. For a cluster located in the direction, the primordial CMB quadrupole induced