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We consider (p + 1)-form gauge fields in flat (2p + 4)-dimensions for which radiation and Coulomb solutions have the same asymptotic fall-off behavior. Imposing appropriate fall-off behavior on fields and adopting a Maxwell-type action, we construct the boundary term which renders the action principle well-defined in the Lorenz gauge. We then compute conserved surface charges and the corresponding asymptotic charge algebra associated with nontrivial gauge transformations. We show that for p ≥ 1, there are three sets of conserved asymptotic charges associated with exact, coexact and zero-mode parts of the corresponding p-form gauge transformations on the asymptotic S 2p+2 . The coexact and zero-mode charges are higher form extensions of the four dimensional electrodynamics (p = 0), and are commuting. Charges associated with exact gauge transformations have no counterparts in four dimensions and form infinite copies of Heisenberg algebras. We briefly discuss physical implications of these charges and their algebra.

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Flat ΛCDM cosmology is specified by two constant fitting parameters in the late Universe, the Hubble constant H 0 and matter density (today) Ω m . Through fitting (H 0 , Ω m ) to mock ΛCDM simulations in redshift bins, we confirm that A := H 2 0 (1−Ω m ) and B := H 2 0 Ω m distributions spread and contract, respectively, with increasing bin redshift. Noting that A = H 2 0 − B, the spread in A and contraction in B corresponds to a spread in H 0 , and consequently in Ω m . Restricted to non-negative energy densities, A, B ≥ 0, the spread in A yields a 'pile up' around A = 0 or Ω m = 1. At even higher redshifts, further spreading flattens A and causes pile up near Ω m = 0. Thus, in generic higher redshift bins the Planck value Ω m ∼ 0.3 appears with low probability. We explore if observational Hubble data, Type Ia supernovae and standardisable quasars substantiate the features. We confirm that observed data exhibit an increasing Ω m (decreasing H 0 ) trend with increasing bin redshift and that such behaviour can arise randomly within the flat ΛCDM model with probability p = 0.0021 (3.1 σ).