We present a comprehensive study of the interstellar NaI \lambda 5890 , 5895 ( NaD ) resonant lines in a complete spectroscopic sample of \sim 600 , 000 galaxies drawn from Sloan Digital Sky Survey ( SDSS , DR7 ) in order to look for cold-gas outflows in the local Universe . This is the first time that doppler blue-shifts of the NaD absorption feature have been investigated as a tracer of cold gas kinematics ( T < 1000 K ) with a statistically significant sample that includes passive , star-forming and starburst galaxies . Individual galaxy spectra are stacked in bins of stellar mass ( M _ { \star } ) and star formation rate ( SFR ) and the dependence of galactic winds , with respect to the galaxies position in the SFR- M _ { \star } plane is investigated . While in most cases the interstellar medium ( ISM ) absorption and emission lines are fixed at the galaxy systemic velocity , at the higher SFR tail ( SFR > 12.5 M _ { \odot } yr ^ { -1 } ) , we find evidence of blue-shifted NaD absorption profiles ( by more than instrumental resolution , 70 km/s ) , which we interpret as evidence of neutral outflowing gas . We explore the properties of the ISM in these galaxies with high SFR , in particular relating the absorption NaD line shape with the galaxy geometry in galaxies with different ionisation mechanisms : Active Galactic Nuclei ( AGN ) and star-formation . We find that : a ) the ISM NaD absorption lines show a clear transition from a strong disk-like component , perfectly centered to the systemic velocity , in the edge-on system ( inclination i > 50 ^ { \circ } of the disk rotation axis ) , to an outflow , blue-shifted , component in face-on galaxies ( i < 50 ^ { \circ } ) ; b ) these trends are observed in galaxies classified as ” purely ” star-forming and AGN dominated objects . In addition to this , we compare the kinematics of the neutral gas with the kinematics of the ionized gas as traced by the [ OIII ] \lambda 5007 emission lines . We find that , in these high SFR galaxies , the perturbations of the [ OIII ] emission line are present only in AGN or composite AGN / star-forming systems , consistent with [ ] . In our AGN sample , the presence of the oxygen line perturbation is independent to the stellar disk inclination : in both the face-on and edge-on systems , the velocity associated with the broad and blue-shifted gaussian component is \sim 125 \pm 45 km/s , velocity dispersion of \sim 460 \pm 30 km/s and a mean maximum velocity of \sim - 1042 \pm 106 km/s . In conclusion , we find that , in the local Universe , galactic winds show two faces which are related to two different ejection mechanisms , namely the neutral outflowing gas phase related to the star formation rate along the galaxy disk and the ionized winds related to the AGN feedback .