A redshift tomography of the Pantheon type Ia supernovae (SnIa) data focusing on the best fit value of the absolute magnitude M and/or Hubble constant H0 in the context of ΛCDM indicates a local variation (z≤ 0.2) at 2σ level, with respect to the best fit of the full dataset. If this variation is physical, it can be interpreted either as a locally higher value of H0, corresponding to a local matter underdensity δρ0/ρ0≃-0.10 ±0.04 or as a time variation of Newton’s constant which implies an evolving Chandrasekhar mass and thus an evolving absolute magnitude M of SnIa. The local void scenario would predict an anisotropy in the best fit value of H0 since it is unlikely that we are located at the center of a local spherical underdensity. Using a hemisphere comparison method we find an anisotropy level consistent with simulated isotropic datasets. We show however, that the anisotropic sky distribution of the Pantheon SnIa data induces a preferred range of directions even in simulated Pantheon data obtained in the context of isotropic ΛCDM. We thus construct a more isotropically distributed subset of the Pantheon SnIa and show that the preferred range of directions disappears. Using this subset we again find no evidence for anisotropy using either the hemisphere comparison method or the dipole fit method. In the context of the modified gravity scenario, we allow for a specific evolving normalized Newton’s constant consistent with General Relativity (GR) at early and late times that depends on a phenomenological parameter gα and fit for gα assuming L≃Gbeff. For b=−3/2 indicated by previous studies we find gα=−0.47±0.36 which is more than 1.5σ away from the GR value of gα=0. This weak hint for weaker gravity at low z is consistent with similar evidence from growth and weak lensing data.
If you use any of the above codes or the figures in a published work please cite the following paper:
Hints of a Local Matter Underdensity or Modified Gravity in the Low z Pantheon data.
Lavrentios Kazantzidis and Leandros Perivolaropoulos
Phys.Rev.D 102 (2020) 2, 023520, arxiv:2004.02155.
Any further questions/comments are welcome.