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Galaxy Groups

Galaxy Groups. Duncan A. Forbes Centre for Astrophysics & Supercomputing, Swinburne University. Galaxy Environments. Clusters : party animals that love being in a crowd Groups : social butterflies that like to mingle Field : hermits that prefer isolation.

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Galaxy Groups

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  1. Galaxy Groups Duncan A. Forbes Centre for Astrophysics & Supercomputing, Swinburne University

  2. Galaxy Environments • Clusters: party animals that love being in a crowd • Groups: social butterflies that like to mingle • Field: hermits that prefer isolation In which environment do we find most galaxies ? How do we define the different environments ?

  3. Specs Loose Compact Cluster Number of galaxies ~20 ~5 ~100 Density over field 20x 10^6x 10^6x Velocity dispersion ~150 ~150 ~700 Hot gas temp. <1keV <1keV >1keV Which environment is most conducive to ongoing mergers today (ie z~0) ?

  4. Galaxy Mergers The rule of thumb for mergers to occur is: vel. disp of group / galaxy internal vel. disp. < 2. Dynamical friction (deceleration of a galaxy moving through a background medium of masses) is a key process in determining the merger timescale. Tdyn ~ (mass of galaxy)^-1 (background density)^-1 => smaller galaxies have a longer merger timescale. Richstone & Malumuth 1983 ApJ 268 30

  5. Hickson Compact Groups Optical selection based on richness: >= 4 galaxies within 3 magnitudes of the brightest galaxy isolation: no galaxies within 3x group radius compactness: surface brightness < 26 mag/sq arc => ~100 HCGs (~90% are real). Hickson 1982 ApJ 255 382

  6. HCGs shouldn’t exist ! Tmerger < < Hubble time => HCGs should have merged into a single larger galaxy by z=0 Why haven’t they ? Athanassoula etal. 1997 MNRAS 286 825

  7. Loose Groups Using a friends-of-friends algorithm Garcia (1993, A&AS, 100, 47) on a database of 6,392 galaxies to B < 14.0 and Vres < 5,500 km/s derived an all-sky catalog of 485 groups of at least 3 galaxies. Garcia (1995, A&A, 297, 56) defined ~120 compact groups from the 1993 group catalog. Compact groups are often found at the centres of larger loose groups.

  8. X-ray Properties of Galaxy Groups Hot gas in groups may be the dominant baryon component in the Universe. The gas has a temperature of about 10^6 K or 1keV and radiates (cools) via thermal bremmstrahlung. Loose and compact groups have similar (identical) X-ray properties. The X-ray luminosity of individual group galaxies appears to be the same as for the field galaxies. Are groups simply scaled down clusters ? Mulchaey 2000 ARAA 38 289

  9. LX vs T relation

  10. Survey of Nearby Galaxy Groups Despite their ubiquity, groups are poorly studied relative to clusters... => Multiwavelength study of 35 nearby galaxy groups. Aim: to understand how the group environment affects the galaxies and how groups evolve. Selection: on the basis of their X-ray luminosity (a rough measure of the group dynamical state). Data: X-ray, optical, IR, and HI

  11. Optical Imaging of Galaxy Groups Colour-magnitude relation Galaxy luminosity function Giant to dwarf galaxy ratio Globular cluster systems

  12. Galaxy Luminosity Function Shape of HCG galaxy LF correlates with X-ray luminosity. Note lack of moderate sized galaxies. Loose group galaxy LF is largely unconstrained. Hunsberger etal. 1998 ApJ, 505, 536

  13. X-ray Gas in Galaxy Groups Early type galaxy fraction vs LX

  14. HI Gas in Galaxy Groups NGC 1052 Group Tidal HI gas ?

  15. Spectral follow-up Measure redshifts Age-date galaxies via spectral line indices Terlevich & Forbes 2001, MNRAS, submitted

  16. Fossils Fossils: massive isolated elliptical galaxies with group-like X-ray halos. Are fossils merged compact groups ? Jones, Ponman & Forbes 2000 MNRAS 312 319

  17. Group Evolution • Compact groups do merge but they are replenished from the surrounding loose group. • Loose groups continually collapse to form new compact groups. • Compact groups have common dark matter halos which suppress merging.

  18. Groups make cDs It has been suggested (Merritt 1984, ApJ, 276, 26) that cD galaxies at the centre of clusters formed from group ellipticals. The group, containing a large elliptical, falls into the cluster at early epochs, accreting galaxies and growing its cD envelope by shredding nearby galaxies.

  19. Concluding Remarks Most galaxies in the Universe are found in Groups. The Group environment is most conducive to mergers. Groups contain 3-30 large galaxies, an unknown number of dwarf galaxies and an intragroup medium of hot gas. Groups provide the link between clusters and the field but the physical processes in galaxy groups are poorly understood. IAU Conference on “Small Galaxy Groups” in 1999, ASP press., Valtonen and Flynn editors.

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