  Context. The properties of the accretion flow surrounding the supermassive
central black hole of the Galaxy, Sgr A*, will be scrutinized by the
new-generation instrument GRAVITY and the Event Horizon Telescope (EHT).
Developing fast, robust, and simple models of such flows is thus important and
very timely. Aims. We want to model the quiescent emission of Sgr A* from radio
to mid-infrared by considering a magnetized compact torus and an extended jet.
Results. We find perfect spectral fit both for face-on and edge-on views. These
best fits give parameters values very close to that found by the most recent
numerical simulations, which are much more complex than our model. The
intrinsic radio size of Sgr A* is found to be in reasonable agreement with the
centimetric observed constraints. Our best-fit infrared spectral index is in
perfect agreement with the latest constraints. Our emission region at 1.3 mm,
although larger than the Doeleman et al. (2008) Gaussian best-fit, does contain
bright features at the 40 microarcsec scale. EHT-reconstructed images show that
torus/jet-specific features persist after the reconstruction procedure, and
that these features are sensitive to inclination. Conclusions. The main
interest of our model is to give a simple and fast model of the quiescent state
of Sgr A*, which gives extremely similar results as compared to
state-of-the-art numerical simulations. Our model is easy to use and we publish
all the material necessary to reproduce our spectra and images, so that anyone
interested can use our results rather straightforwardly. We hope that such a
public tool can be useful in the context of the recent and near-future GRAVITY
and EHT results. Our model can in particular be easily used to test alternative
compact objects models, or alternative gravity theories. The main limitation of
our model is that we do not yet treat the X-ray emission.
