1 / 22

The J1051-17 Group: Evolution and Interaction

The J1051-17 Group: Evolution and Interaction. Virginia Kilborn Swinburne University of Technology. Sarah Sweet (Australian National University) Gerhardt Meurer (University of Western Australia) Michael Drinkwater (University of Queensland Kenji Bekki (University of Western Australia).

anne-levine
Download Presentation

The J1051-17 Group: Evolution and Interaction

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The J1051-17 Group: Evolution and Interaction Virginia Kilborn Swinburne University of Technology Sarah Sweet (Australian National University) Gerhardt Meurer (University of Western Australia) Michael Drinkwater (University of Queensland Kenji Bekki (University of Western Australia)

  2. Groups: Galaxy pre-processing • Loose groups – 2-4 spiral members + • dwarf galaxies • Group masses up to approx. 1013 M • HI-rich Kern et al 2008 Grus quartet: Lutz et al. in prep.

  3. SINGG Choirs • Survey for Ionisation in Gas-rich Galaxies (Meurer et al. 2006) • SINGG imaged approx 400 galaxies in Hα, selected from the HIPASS HI catalogue (approx 15’ resolution) • 15 imaging fields contained 4 or more galaxies: dubbed the SINGG “Choirs” (Sweet et al. 2013) 50kpc Hα imaging of 3 SINGG groups (orange), overlaid on optical R-band (blue/white)

  4. HI Mass distribution of SINGG and the Choirs HI mass from HIPASS

  5. SINGG Choirs: Tidal Dwarf Galaxy laboratories? TDGs – important to know how dwarf galaxies are formed for comparison with cosmological simulations Horellou & Koribalski 2007

  6. SINGG Choirs: Tidal Dwarf Galaxy laboratories? Recent galaxy interactions- but dwarfs not situated in optically detected tidal tails Measure metalicity and dynamics to determine properties of TDG candidates in the Choirs

  7. Metalicity of TDG candidates Simulations by Bekki et al. 2014 (in prep) show that TDGs should have moderate metalicity, and faint Sweet et al. 2014

  8. Dynamics and mass: Optical data WiFES and Keck spectra of dwarf galaxies – rotation curves to determine total mass Keck Deimos spectrum Sweet et al. 2014 (in prep)

  9. Dynamics and mass: HI data ATCA and VLA data for all 15 groups

  10. SINGG Choir J1051-17 9 emission line galaxies found in the group SINGG Hα imaging

  11. Keck spectra: 5 more dwarf galaxies in group

  12. J1051-17: HI imaging S1: HI mass = 4x1010M HI excess (HI def = -0.6) S2 (NGC 3431): HI mass =1.4x109M HI deficient (HI def = 0.9)

  13. Galaxy properties: TDGs ? Red stars: J1051-17 group members

  14. Central galaxy: Polar ring? DecCam imaging

  15. S1: UV imaging

  16. Optical dynamics: 2 components

  17. HI dynamics Kilborn et al. 2014, in prep

  18. Ongoing HI accretion?

  19. Summary • SINGG Choirs are excellent laboratories to study the physical processes in evolving groups • J1051-17 is a polar ring galaxy with possible ongoing HI accretion • Implications for gas fuelling scenarios and TDG formation • 14 more Choirs to analyse…

  20. Star formation?

  21. Evolution in galaxy groups Fearly Fearly Log v Log Lx The early-type fraction Increases with increasing X-ray luminosity and Velocity dispersion More evolved groups: -more early type galaxies -higher velocity dispersions -higher X-ray luminosity

More Related