Sommaire:

The observed clustering of quasars on large angular scales is imprinted with information of our motion with respect to the cosmological rest-frame. Using the Catwise catalogue, based upon data from the Wide-field Infrared Survey Explorer (WISE), we infer posteriors for the kinematic dipole and the intrinsic quasar clustering dipole. We present a methodology for simulating dipole measurements including survey systematics such as; the survey mask, variable photometric errors, biased dust extinction modelling and contamination along the ecliptic plane. We then use Simulation-based Inference to infer our posteriors. We examine a range of different prior hypotheses, dipole estimators and magnitude cuts . When compared to measurements inferred from the Cosmic Microwave Background dipole and with a $\Lambda$CDM prior on the expected intrinsic quasar clustering dipole in agreement with past measurements we get a greater than 6 $\sigma$ tension with the CMB measured kinematic dipole when estimating the dipole for the entire sample and a greater than 9 $\sigma$ tension with a spectrally binned dipole estimator.

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