Galaxy Zoo: Passive Red Spirals
Karen L. Masters (ICG, Portsmouth), Moein Mosleh (Sussex/Leiden), A., Kathy Romer (Sussex), Robert C. Nichol (ICG, Portsmouth), Steven P. Bamford, (Nottingham), Kevin Schawinski (Yale), Chris J. Lintott (Oxford), Dan, Andreescu, Heather C. Campbell, Ben Crowcroft, Isabelle Doyle

TL;DR
This study investigates red spiral galaxies, revealing their properties, environments, and potential evolutionary paths, suggesting they are old, gas-depleted disks possibly influenced by bar instabilities and environmental factors.
Contribution
It provides a detailed analysis of red spirals' physical and environmental characteristics, highlighting their potential as transition objects and their association with bars and active galactic nuclei.
Findings
Red spirals are more common at high stellar masses.
They have older stellar populations and less recent star formation.
Red spirals are more likely to host Seyfert or LINER activity.
Abstract
We study the spectroscopic properties and environments of red spiral galaxies found by the Galaxy Zoo project. By carefully selecting face-on, disk dominated spirals we construct a sample of truly passive disks (not dust reddened, nor dominated by old stellar populations in a bulge). As such, our red spirals represent an interesting set of possible transition objects between normal blue spirals and red early types. We use SDSS data to investigate the physical processes which could have turned these objects red without disturbing their morphology. Red spirals prefer intermediate density regimes, however there are no obvious correlations between red spiral properties and environment - environment alone is not sufficient to determine if a spiral will become red. Red spirals are a small fraction of spirals at low masses, but are a significant fraction at large stellar masses - massive…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
