The microquasar MAXI J(1820+070) went into outburst from mid-March until mid-July 2018 with several faint rebrightenings afterwards. With a peak flux of approximately 4 Crab in the (20-50) keV, energy range the source was monitored across the electromagnetic spectrum with detections from radio to hard X-ray frequencies. Using these multi-wavelength observations, we analyzed quasi-simultaneous observations from 12 April, near the peak of the outburst ((sim 23) March). Spectral analysis of the hard X-rays found a (kT_e sim 30 ) keV and ( tau sim 2) with a texttt{CompTT} model, indicative of an accreting black hole binary in the hard state. The flat/inverted radio spectrum and the accretion disk winds seen at optical wavelengths are also consistent with the hard state. Then we constructed a spectral energy distribution spanning (sim 12) orders of magnitude using modelling in texttt{JetSeT}. The model is composed of an irradiated disk with a Compton hump and a leptonic jet with an acceleration region and a synchrotron-dominated cooling region. texttt{JetSeT} finds the spectrum is dominated by jet emission up to approximately (10^{14}) Hz after which disk and coronal emission dominate. The acceleration region has a magnetic field of ( B sim 1.6 times 10^4 ) G, a cross section of (R sim 2.8 times 10^{9} ) cm, and a flat radio spectral shape naturally obtained from the synchroton cooling of the accelerated electrons. The jet luminosity of (> 8 times 10^{37} ) erg/s ((> 0.15L_{Edd})) compared to an accretion luminosity of ( sim 6 times 10^{37}) erg/s, assuming a distance of 3 kpc. Because these two values are comparable, it is possible the jet is powered predominately via accretion with only a small contribution needed from the Blanford-Znajek mechanism from the reportedly slowly spinning black hole.
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