  A rare population of massive disk-dominated quiescent galaxies has recently
drawn much attention, which intrudes the red sequence population without
destroying the underlying stellar disks. In this study, we have carefully
identified 48 red sequence (RS), disk-dominated galaxies with $M_{\ast} >
10^{10}M_{\odot}$ between redshift 0.5 and 1.0 in all five CANDELS fields.
These galaxies are well fitted by a two-component bulge plus disk model, and
have the bulge-to-total ratio $B/T<0.4$ in the both F814W and F160W bands. The
fitting results indicate that these galaxies generally have extended stellar
disks ($\rm \sim 3~kpc$ on average) and tiny bulge components ($\rm \sim
0.5~kpc$ on average). To understand their possible origins, we have also
selected two control samples of 156 green valley (GV) and 309 blue cloud (BC)
disk-dominated galaxies according to the same selection criteria. We study the
$UVI$($U-V$ versus $V-I$) color gradients of these galaxies to infer their
specific star formation rate (sSFR) gradients out to the maximum acceptable
radii. We show that on average the disks in disk-dominated RS galaxies are
fully quenched at all radii, whereas both the BC and GV disks are not fully
quenched at any radii. We find that all the BC, GV and RS disk galaxies
generally have nearly flat sSFR profiles. We propose a potential formation
mechanism, acknowledging that various other mechanisms (e.g., central
compaction and AGN feedback) might contribute, where massive quiescent
disk-dominated galaxies are predominantly formed via a process of secular disk
fading.
