Inference of the cosmic rest-frame from supernovae Ia

We determine the proper motion of the Solar system from the Pantheon sample of supernovae (SNe) of type Ia. The posterior distribution of the Solar system proper velocity, its direction and relevant cosmological parameters are obtained based on the observed distance moduli, heliocentric redshifts, and positions of SNe by means of a Markov Chain Monte Carlo method. We account for the unknown peculiar motion of SNe by including their expected covariance from linear theory. We find that the Solar system moves with $v_o = 249 \pm 51$ km/s towards $RA = 166 \pm 16$ deg, $Dec = 10 \pm 19$ deg (J2000) (all at 68\% C.L.). The direction of motion agrees with the direction of the dipole observed in the cosmic microwave background (CMB) ($RA = 166$ deg, $Dec = -7$ deg). The inferred velocity is $2.4 \sigma$ smaller than the value inferred from a purely kinematic interpretation of the CMB dipole ($370$ km/s). Assuming a flat $\Lambda$ cold dark matter model, we find no degeneracy of Solar proper motion with other cosmological parameters. The dimensionless matter density is $\Omega_M = 0.305 \pm 0.022$, in excellent agreement with CMB measurements. We also find no degeneracy of the Solar proper motion with the SN calibration nuisance parameter. We conclude that a larger sample of SNe will allow an independent and robust test of the kinematic nature of the CMB dipole.