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We explore the possibility of characterizing the expansion rate on localcosmic scales $(z \lesssim 0.1)$, where the cosmological principle is violated,in a model-independent manner, i.e. in a more meaningful and comprehensive waythan is possible using the $H_0$ parameter of the Standard Model alone. We dothis by means of the expansion rate fluctuation field $\eta$, an unbiasedGaussian observable that measures deviations from isotropy in theredshift-distance relation. We show that an expansion of $\eta$ in terms ofcovariant cosmographic parameters, both kinematic (expansion rate$\mathbb{H}_o$, deceleration $\mathbb{Q}_o$ and jerk $\mathbb{J}_o$) andgeometric (curvature $\mathbb{R}_o$), allows for a consistent description ofmetric fluctuations even in a very local and strongly anisotropic universe. Thecovariant cosmographic parameters critically depend on the observer's state ofmotion. We thus show how the lower order multipoles of ${\eta}_{\ell}$ ($\ell\leq 4$), measured by a generic observer in an arbitrary state of motion can beused to disentangle expansion effects that are induced by observer's motionfrom those sourced by pure metric fluctuations. We test the formalism usinganalytical, axis-symmetric toy models which simulate large-scale linearfluctuations in the redshift-distance relation in the local Universe and whichare physically motivated by available observational evidences. We show how toexploit specific features of $\eta$ to detect the limit of validity of acovariant cosmographic expansion in the local Universe, and to define theregion where data can be meaningfully analyzed in a model-independent way, forcosmological inference. We also forecast the precision with which future datasets, such as ZTF, will constrain the structure of the expansion rateanisotropies in the local spacetime

Cosmography of the Local Universe by Multipole Analysis of the Expansion Rate Fluctuation Field