We have recently entered the era of Day-1 supernova (SN) observations, enabling us to probe temporal regimes that were previously hardly accessible. Discovering a SN in its infancy, several hours from explosion, and utilizing quick and efficient follow-up capabilities allows us to directly probe the immediate surrounding of the star that has just exploded, before the whole region is “destroyed” by the several solar masses of the SN ejecta. A sample of “Flash-Spectroscopy” events from the last several years revealed stark evidence for the existence of nearby circum-stellar distribution of material (CSM) that is likely ejected from the progenitor star at an elevated, maybe eruptive, manner, shortly (months to several years) before the final demise of the massive star. A recent detailed study of the unique flash-spectroscopy event of SN 2013fs (iPTF13dqy), which turned out to be a fairly regular Type-II SN, has taught us that this phenomenon is possibly more widespread than previously anticipated. These realizations have already began providing additional boost for theoretical studies that aim at improving our understanding of the very final stages in the evolution of massive stars. Constraining (by direct prompt observations) the mass-loss history, surface composition and profiles of various thermodynamic properties of the progenitor star at the onset of explosion also provides meaningful initial conditions (possibly somewhat altered than what was previously assumed), for the explosion calculations themselves. I will also briefly mention near-future prospects of both ground and space-based transient-hunting facilities; all of which have the potential to further shorten our discovery and follow-up capabilities to within the 1-hour(!) timespan from explosion.