The case studies described in Section 3 are interesting, but the natural question is how common are the features shown in Figure 3. While SINFONI has played a major role in this area, the wide-field IFU MUSE, one of the second generation instrument for the VLTs which started operation in the Fall of 2014, is changing our view of the CGM and will allow for a major leap forward in our knowledge of gas inflows and outflows. Indeed, thanks to its large 1' x 1' field of view sampled at 0.2 arcsec/spaxel, large wavelength range from 480nm to 930 nm sampled at 1.25Å, and to its unprecedented sensitivity, MUSE (Bacon et al. 2010) will allow us to study gas flows around galaxies with samples 10 times larger (i.e. ≈ 100) than current surveys. In particular, we started the MusE Gas FLO and Wind (MEGAFLOW) survey designed to yield ≈ 100 galaxy-quasar pairs in about 22 quasar sight-lines selected from the SDSS database (DR12) which have multiple (4 or more) Mg ii λλ 2796,2803 absorbers at redshifts 0.3 < z < 1.4 suitable for [O ii] λλ3726,3729 emitters. Results on outflows from the first two fields appeared in Schroetter et al. (2016) and the first results on accretion from this survey are to appear in J. Zabl (2017, in prep.).