  We present the e-TidalGCs Project which aims at modeling and predicting the
extra-tidal features surrounding all Galactic globular clusters for which 6D
phase space information, masses and sizes are available (currently 159 globular
clusters). We focus the analysis and presentation of the results on the
distribution of extra-tidal material on the sky, and on the different
structures found at different heliocentric distances. We emphasize the wide
variety of morphologies found: beyond the canonical tidal tails, our models
reveal that the extra-tidal features generated by globular clusters take a wide
variety of shapes, from thin and elongated shapes, to thick, and complex
halo-like structures. We also compare some of the most well studied stellar
streams found around Galactic globular clusters to our model predictions,
namely those associated to the clusters NGC 3201, NGC 4590, NGC 5466 and Pal 5.
Additionally, we investigate how the distribution and extension in the sky of
the simulated streams vary with the Galactic potential by making use of three
different models, containing or not a central spheroid, or a stellar bar.
Overall, our models predict that the mass lost by the current globular cluster
population in the field from the last 5 Gyrs is between
$0.3-2.1\times10^{7}M_{\odot}$, an amount comparable between 7-55 % of current
mass. Most of this lost mass is found in the inner Galaxy, with the half-mass
radius of this population being between 4-6 kpc. The outputs of the simulations
will be publicly available, at a time when the ESA Gaia mission and
complementary spectroscopic surveys are delivering exquisite data to which
these models can be compared.
