Morphology–spin connection in the SAMI Galaxy Survey

Clicks: 29
ID: 322489
2026
Free PDF
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.
AI Quality Assessment
Not analyzed
Readership in this journal
Steady

Ranked #294 of 1,384 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 1,384 in total.

Mint this article as an NFT
Not yet minted

Create 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
Sign in to mint
Abstract
Abstract The spin parameter ${\lambda _{\mathrm{R_e}}}$ is a proxy for the specific stellar angular momentum of galaxies and is a useful metric for classifying kinematic morphology. This study aims to quantify the relative importance of galaxy properties in explaining ${\lambda _{\mathrm{R_e}}}$ using data from the Sydney-AAO Multi-object Integral-field spectrograph (SAMI) Galaxy Survey. We apply partial correlation analysis and partial least squares regression to assess the relative contributions of different parameters in explaining ${\lambda _{\mathrm{R_e}}}$. We find that morphology indicators, bulge-to-total ratio within one effective radius (B/Te) and ellipticity (ϵe), show the strongest correlations with ${\lambda _{\mathrm{R_e}}}$ and play a leading role in the regression analysis. This result statistically confirms the established fast-rotator sequence, in which fast-rotating early-type galaxies form a continuous structural and kinematic sequence with spiral galaxies, with ${\lambda _{\mathrm{R_e}}}$ decreasing as bulge prominence increases. The light-weighted age (AgeLW) and stellar mass (M⋆) also exhibit significant correlations, but their contributions are secondary to the morphology indicators in multivariate analyses. We also examine whether the observed trends in ${\lambda _{\mathrm{R_e}}}$ can be reproduced using galaxy properties alone. The morphology indicators (B/Te, ϵe) reproduce the overall distribution of observed ${\lambda _{\mathrm{R_e}}}$ with a scatter of about 0.12, while the inclusion of AgeLW and M⋆ provides only modest additional improvement. However, these relations do not reproduce the slow-rotator regime well. Overall, our results show that photometric structural parameters best explain ${\lambda _{\mathrm{R_e}}}$ and suggest that statistical inference of galaxy spin from non-IFS observables may become feasible with improved models and a broader set of parameters.
Reference Key
openalex_W7170199869 Use this key to autocite in the manuscript while using SciMatic Manuscript Manager or Thesis Manager
Authors Youngmin Baek, Sree Oh, Sukyoung K. Yi, S. M. Croom, Matthew Colless, Jesse van de Sande, Stefania Barsanti, Sam P Vaughan
Are you one of these authors? Claim your profile
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1379
URL
https://doi.org/10.1093/mnras/stag1379
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.