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We use magneto-hydrodynamical simulations of Milky Way-mass haloes from theAuriga project to examine the properties of surviving and destroyed dwarfgalaxies that are accreted by these haloes over cosmic time. We show that thecombined luminosity function of surviving and destroyed dwarfs at infall issimilar in the various Auriga haloes, and is dominated by the destroyed dwarfs.There is, however, a strong dependence on infall time: destroyed dwarfs havetypically early infall times, $t_{infall}<6$ Gyr, whereas the majority ofdwarfs accreted at $t_{infall}>10$ Gyr have survived to the present day.Because of their late infall the surviving satellites today had highermetallicites at infall than their destroyed counterparts of similar infallmass; the difference is even more pronounced for the present-day metallicitesof satellites, many of which continue to form stars after infall. In agreementwith previous work, we find that a small number of relatively massive destroyeddwarf galaxies dominate the mass of the stellar haloes. However, there is asignificant radial dependence: while 90 per cent of the mass in the innerregions ($<\,20\,$kpc) is contributed, on average, by only 3 massiveprogenitors, the outer regions ($>\,100\,$kpc) typically have $\sim8$ mainprogenitors of relatively lower mass. Finally, we show that a few massiveprogenitors dominate the metallicity distribution of accreted stars, even atthe metal poor end. Contrary to common assumptions in the literature, dwarfgalaxies of mass $M_{*}<10^7 \, M_{\odot}$ make up less than 10 per cent of theaccreted, metal poor stars ([Fe/H] $<\,-3$) in the inner $50\,$kpc.

A tale of two populations: surviving and destroyed dwarf galaxies and the build up of the Milky Way's stellar halo