Warped Disk Galaxies. I. Linking U type Warps in Groups/Clusters to Jellyfish Galaxies
arXiv:2208.05534 · doi:10.3847/1538-4357/ac7462
Abstract
arped disk galaxies are classified into two morphologies: S- and U-types. Conventional theories routinely attribute both types to galactic tidal interaction and/or gas accretion, but reproducing of U-types in simulations is extremely challenging. Here we investigate whether both types are governed by the same mechanisms using the most extensive sample of 8000 nearby (0.02\,\,z\,\,0.06) massive (\,\,) edge-on disks from SDSS. We find that U-types show on average bluer optical colors and higher specific star formation rate (sSFR) than S-types, with more strongly warped U-types having higher sSFR. We also find that while the S-type warp properties correlate with the tidal force by the nearest neighbor regardless of the environment, there is no such correlation for U-types in groups/clusters, suggesting a non-tidal environmental could be at play for U-types, such as ram pressure stripping (RPS). Indeed, U-types are more common in groups/clusters than in fields and they have stellar mass, gas fraction, sSFR enhancement and phase-space distribution closely analogous to RPS-induced jellyfish galaxies in clusters. We furthermore show that the stellar disks of most RPS galaxies in the IllustirsTNG simulation are warped in U-shape and bent in opposite direction of stripped gas tails, satisfying theoretical expectations for stellar warps embeded in jellyfishes. We therefore suggest that despite the majority of U-types that live in fields being still less explained, RPS can be an alternative origin for those in groups/clusters.
28 pages, 15 figures, accpeted for publication in ApJ
References in corpus (26)
- The effect of galaxy mass ratio on merger--driven starbursts
- BUDHIES II: A phase-space view of HI gas stripping and star-formation quenching in cluster galaxies
- MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic study of the archetypal galaxy ESO137-001
- An intuitive 3D map of the Galactic warp's precession traced by classical Cepheids
- A Magellanic Origin for the Warp of the Galaxy
- Physical properties of SDSS satellite galaxies in projected phase-space
- LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters
- Ram pressure stripping candidates in the Coma Cluster: Evidence for enhanced star formation
- GASP XXI. Star formation rates in the tails of galaxies undergoing ram-pressure stripping
- GASP XVII. HI imaging of the jellyfish galaxy JO206: gas stripping and enhanced star formation
- Lopsided galaxies: the case of NGC 891
- Formation of Warped Disks by Galactic Fly-by Encounters. I. Stellar Disks
- Observational signatures of a warped disk associated with cold-flow accretion
- Star formation in galaxies falling into clusters along supercluster-scale filaments
- WALLABY Early Science - III. An HI Study of the Spiral Galaxy NGC 1566
- GASP XXVI. HI Gas in Jellyfish Galaxies: The case of JO201 and JO206
- The Large-Scale Atomic and Molecular Gas in the Circinus Galaxy
- LoTSS Jellyfish Galaxies III. The first identification of jellyfish galaxies in the Perseus cluster
- Galaxies with conspicuous optical warps
- Investigating the Stellar Mass Growth Histories of Satellite Galaxies as a Function of Infall Time using Phase-Space
- Transforming gas-rich low-mass disky galaxies into ultra-diffuse galaxies by ram pressure
- Near-infrared and optical observations of galactic warps: A common, unexplained feature of most discs
- Jellyfish: Resolving the kinematics of extreme ram-pressure stripping at
- Explaining the enhanced star formation rate of Jellyfish galaxies in galaxy clusters
- Probing IGM large-scale flows: warps in galaxies at shells of voids
- A Lack of Evidence for Global Ram-pressure Induced Star Formation in the Merging Cluster Abell 3266