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Dust-enshrouded, starbursting, submillimeter galaxies (SMGs) at $z \geq 3$have been proposed as progenitors of $z \geq 2$ compact quiescent galaxies(cQGs). To test this connection, we present a detailed spatially resolved studyof the stars, dust and stellar mass in a sample of six submillimeter-brightstarburst galaxies at $z \sim 4.5$. The stellar UV emission probed by HST isextended, irregular and shows evidence of multiple components. Informed by HST,we deblend Spitzer/IRAC data at rest-frame optical finding that the systems areundergoing minor mergers, with a typical stellar mass ratio of 1:6.5. The FIRdust continuum emission traced by ALMA locates the bulk of star formation inextremely compact regions (median $r_{\rm{e}} = 0.70 \pm 0.29$ kpc) and it isin all cases associated with the most massive component of the mergers (median$\log (M_{*}/M_{\odot}) = 10.49 \pm 0.32$). We compare spatially resolved UVslope ($\beta$) maps with the FIR dust continuum to study the infrared excess($\rm{IRX} = L_{\rm{IR}}/L_{\rm{UV}}$)-$\beta$ relation. The SMGs displaysystematically higher $\rm{IRX}$ values than expected from the nominal trend,demonstrating that the FIR and UV emissions are spatially disconnected.Finally, we show that the SMGs fall on the mass-size plane at smaller stellarmasses and sizes than cQGs at $z = 2$. Taking into account the expectedevolution in stellar mass and size between $z = 4.5$ and $z = 2$ due to theongoing starburst and mergers with minor companions, this is in agreement witha direct evolutionary connection between the two populations.

Starburst to quiescent from HST/ALMA: Stars and dust unveil minor mergers in submillimeter galaxies at $z \sim 4.5$