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The J1051-17 Group: Evolution and Interaction
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Transcript of The J1051-17 Group: Evolution and Interaction
The J1051-17 Group: Evolution and InteractionVirginia KilbornSwinburne University of Technology
Sarah Sweet (Australian National University)Gerhardt Meurer (University of Western Australia)Michael Drinkwater (University of QueenslandKenji Bekki (University of Western Australia)
Groups: Galaxy pre-processing
Grus quartet: Lutz et al. in prep.Kern et al 2008
•Loose groups – 2-4 spiral members +dwarf galaxies•Group masses up to approx. 1013 M
•HI-rich
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)
Hα imaging of 3 SINGG groups (orange), overlaid on optical R-band (blue/white)
50kpc
HI Mass distribution of SINGG and the Choirs
HI mass from HIPASS
SINGG Choirs: Tidal Dwarf Galaxy laboratories?
Horellou & Koribalski 2007
TDGs – important to know how dwarf galaxies are formed for comparison with cosmological simulations
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
Metalicity of TDG candidates
Sweet et al. 2014
Simulations by Bekki et al. 2014 (in prep) show that TDGs should have moderate metalicity, and faint
Dynamics and mass: Optical data
WiFES and Keck spectra of dwarf galaxies – rotation curves to determine total mass
Keck Deimos spectrumSweet et al. 2014 (in prep)
Dynamics and mass: HI dataATCA and VLA data for all 15 groups
SINGG Choir J1051-17
SINGG Hα imaging
9 emission line galaxiesfound in the group
Keck spectra: 5 more dwarf galaxies in group
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)
Galaxy properties: TDGs ?
Red stars: J1051-17 group members
Central galaxy: Polar ring?
DecCam imaging
S1: UV imaging
Optical dynamics: 2 components
HI dynamics
Kilborn et al. 2014, in prep
Ongoing HI accretion?
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…
Star formation?
Evolution in galaxy groups
Log Lx
F early F ea
rly
Log v
The early-type fractionIncreases with increasing X-ray luminosity and Velocity dispersion
More evolved groups:-more early type galaxies-higher velocity dispersions-higher X-ray luminosity