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We have constructed a mass-selected sample of Mstar>10^11Msolar galaxies at1<z<3 in the CANDELS UDS and COSMOS fields and have decomposed these systemsinto their separate bulge and disk components according to their H(160)-bandmorphologies. By extending this analysis to multiple bands we have been able toconduct individual bulge and disk component SED fitting which has provided uswith stellar-mass and star-formation rate estimates for the separate bulge anddisk components. These have been combined with size measurements to explore theevolution of these massive high-redshift galaxies. By utilising the newdecomposed stellar-mass estimates, we confirm that the bulge components displaya stronger size evolution than the disks. This can be seen from both thefraction of bulge components which lie below the local relation and the mediansizes of the bulge components, where the bulges are a median factor of2.93+/-0.32 times smaller than similarly massive local galaxies at 1<z<2 and3.41+/-0.58 smaller at 2<z<3; for the disks the corresponding factors are1.65+/-0.14 and 1.99+/-0.25. Moreover, by splitting our sample into the passiveand star-forming bulge and disk sub-populations and examining their sizes as afraction of their present-day counter-parts, we find that the star-forming andpassive bulges are equally compact, star-forming disks are larger, while thepassive disks have intermediate sizes. This trend is not evident whenclassifying galaxy morphology on the basis of single-Sersic fits and adoptingthe overall star-formation rates. Finally, by evolving the star-formationhistories of the passive disks back to the redshifts when the passive diskswere last active, we show that the passive and star-forming disks haveconsistent sizes at the relevant epoch. These trends need to be reproduced byany mechanisms which attempt to explain the morphological evolution ofgalaxies.

The Decomposed Bulge and Disk Size-Mass Relations of Massive Galaxies at 1