English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We investigate the assembly history of massive disk galaxies and describe howthey shape their morphology through cosmic time. Using SHARDS and HST data, wemodeled the surface brightness distribution of 91 massive galaxies at redshift$0.14<z\leq 1$ in the wavelength range $0.5-1.6$ $\mu$m, deriving theuncontaminated spectral energy distributions of their bulges and disksseparately. This spectrophotometric decomposition allows us to compare thestellar populations properties of each component in individual galaxies. Wefind that the majority of massive galaxies ($\sim85\%$) builds inside-out,growing their extended stellar disk around the central spheroid. Some bulgesand disks could start forming at similar epochs, but these bulges grow morerapidly than their disks, assembling $80\%$ of their mass in $\sim0.7$ Gyr and$\sim3.5$ Gyr, respectively. Moreover, we infer that both older bulges andolder disks are more massive and compact than younger stellar structures. Inparticular, we find that bulges display a bimodal distribution of mass-weightedages, i.e., they form in two waves. In contrast, our analysis of the diskcomponents indicates that they form at $z\sim1$ for both first and second-wavebulges. This translates to first-wave bulges taking longer in acquiring astellar disk ($5.2$ Gyr) compared to second-wave less-compact spheroids ($0.7$Gyr). We do not find distinct properties (e.g., mass, star formation timescale,and mass surface density) for the disks in both types of galaxies. We concludethat the bulge mass and compactness mainly regulate the timing of the stellardisk growth, driving the morphological evolution of massive disk galaxies.

From naked spheroids to disky galaxies: how do massive disk galaxies shape their morphology?