The evolution of the sizes and angular momentum content of galaxies in the COLIBRE simulations
Clicks: 1
ID: 320968
2026
Article Quality & Performance Metrics
Overall Quality
Not rated
Combines reader engagement with the AI quality analysis. This
article has not been analysed, so there is no overall score —
reader engagement is measured and shown alongside.
Reader Engagement
0.0
/100
1 views
0 readers
AI Quality Assessment
Not analyzed
Readership in this journal
Ranked #813 of 900 articles by views in monthly notices of the royal astronomical society
Most read
Least read
Bar heights use a square-root scale. Only the 120 most-read articles are drawn; the journal has 900 in total.
Mint this article as an NFT
Not yet mintedCreate a permanent, verifiable on-chain record of this article on the Scimatic Network. The NFT is held in your Journament account, and you can withdraw it to your own wallet at any time.
5
SUSD
one-off · no wallet required
Abstract
Abstract We analyse the sizes and specific angular momentum content of galaxies in the colibre cosmological hydrodynamical simulations spanning two orders of magnitude in mass resolution. We compare the predicted size–mass and angular momentum–mass relations to a broad range of observational measurements spanning redshifts z = 0 to 4. At z = 0, colibre reproduces observed size–mass relations over the sampled mass range 108 ≲ M⋆/M⊙ ≲ 1011.5, and for multiple size definitions, including two- and three-dimensional stellar half-mass radii, half-light radii across several wavelengths, as well as alternative measures such as baryonic half-mass radii and characteristic radii defined by stellar surface density thresholds. The simulations also recover the observed segregation of galaxies in the size–mass plane by morphological type and star formation rate, and reproduce the distinct, approximately parallel sequences followed by star-forming discs and quenched spheroids in the stellar specific angular momentum–mass plane. The angular momentum content of star-forming colibre galaxies match that of observed systems out to z ≈ 1.5. At higher redshifts, massive galaxies (109.5 ≲ M⋆/M⊙ ≲ 1011) in the simulations are somewhat smaller than observed, and the separation between star-forming and passive populations in the size–mass plane is reduced relative to observations, while at lower masses the agreement remains good. This apparent discrepancy may reflect the effects of dust attenuation, which is neglected in our analysis and may preferentially obscure the central regions of observed systems. Overall, our findings highlight the close connection between galaxy size, angular momentum, and morphology over cosmic time.
| Reference Key |
openalex_W7168258624
Use this key to autocite in the manuscript while using
SciMatic Manuscript Manager or Thesis Manager
|
|---|---|
| Authors | Aaron D Ludlow, Katy L Proctor, Joop Schaye, Filip Huško, Victor J Forouhar Moreno, Danail Obreschkow, Evgenii Chaikin, Matthieu Schaller, Sylvia Ploeckinger, Alejandro Benítez-Llambay, Kyle A Oman, Robert J McGibbon, James W Trayford, Carlos S Frenk, Alexander J Richings |
| Journal | monthly notices of the royal astronomical society |
| Year | 2026 |
| DOI |
10.1093/mnras/stag1319
|
| URL | |
| Keywords | Keywords not found |
Citations
No citations found. To add a citation, contact the admin at info@scimatic.org
Comments
No comments yet. Be the first to comment on this article.