Some supernovae ( SNe ) show evidence for mass-loss events taking place prior to their explosions .
Measuring their pre-outburst mass-loss rates provide essential information regarding the mechanisms that are responsible for these events .
Here we present XMM -Newton and Swift X-ray observations taken after the latest , and presumably the final , outburst of SN 2009ip .
We use these observations as well as new near infra-red and visible light spectra , and published radio and visible light observations to put six independent order-of-magnitude constrains on the mass-loss rate of the SN progenitor prior to the explosion .
Our methods utilize : the X-ray luminosity , the bound-free absorption , the H \alpha luminosity , the SN rise-time , free-free absorption , and the bolometric luminosity of the outburst detected prior to the explosion .
Assuming spherical mass-loss with a wind density profile , we estimate that the effective mass-loss rate from the progenitor was between 10 ^ { -3 } to 10 ^ { -2 } M _ { \odot } yr ^ { -1 } , over a few years prior to the explosion , with a velocity of \sim 10 ^ { 3 } km s ^ { -1 } .
This mass-loss rate corresponds to a total circum stellar matter mass of \sim 0.04 M _ { \odot } , within 6 \times 10 ^ { 15 } cm of the SN .
We note that the mass-loss rate estimate based on the H \alpha luminosity is higher by an order of magnitude .
This can be explained if the narrow line H \alpha 
component is generated at radii larger than the shock radius , or if the CSM has an aspherical geometry .
We discuss simple geometries which are consistent with our results .