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Type Ia supernovae (SN Ia) are the most important standard candles formeasuring the expansion history of the universe. The thermonuclear explosion ofa white dwarf can explain their observed properties, but neither the progenitorsystems nor any stellar remnants have been conclusively identified.Underluminous SN Ia have been proposed to originate from a so-calleddouble-detonation of a white dwarf. After a critical amount of helium isdeposited on the surface through accretion from a close companion, the heliumis ignited causing a detonation wave that triggers the explosion of the whitedwarf itself. We have discovered both shallow transits and eclipses in thetight binary system CD-30 11223 composed of a carbon/oxygen white dwarf and ahot helium star, allowing us to determine its component masses and fundamentalparameters. In the future the system will transfer mass from the helium star tothe white dwarf. Modelling this process we find that the detonation in theaccreted helium layer is sufficiently strong to trigger the explosion of thecore. The helium star will then be ejected at so large a velocity that it willescape the Galaxy. The predicted properties of this remnant are an excellentmatch to the so-called hypervelocity star US 708, a hot, helium-rich starmoving at more than 750 km/s, sufficient to leave the Galaxy. Theidentification of both progenitor and remnant provides a consistent picture ofthe formation and evolution of underluminous type Ia supernovae.

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae