1. The clustering of galaxy groups in the 2dFGRS (2PIGG) The clustering of 2PIGGs Project zero: CDM predictions and parameter constraints Project one, two,..: Other uses of the clustering of 2PIGG Network-wide project again! Outline:

2. Clustering dependence on group mass from the 2PIGG

3. 2PIGG Subsamples: Padilla & the 2dFGRS Team – Astro-ph/0402577

4. Indicators of amplitude of clustering: Relative bias:   s) = b 2  ’(s) Padilla & the 2dFGRS Team – Astro-ph/0402577 Clustering dependence on group mass from the 2PIGG

5. Clustering length:  (s 0 ) = 1 Indicators of amplitude of clustering: Clustering dependence on group mass from the 2PIGG

6. Clustering dependence on group mass: Comparison with other cluster results Padilla & the 2dFGRS Team – Astro-ph/0402577

7. Project zero: CDM predictions and parameter constraints

8. Clustering dependence on group mass: Comparison with  CDM

9. Clustering dependence on group mass: CDM predictions mh0h0b/m8vmh0h0b/m8v 1. Choose  m h 0 and h 0. Calculate  = 1 -  m 2. Calculate d c using luminosity function and geometry 3. Pick  b /  m 4. Calculate linear mass power spectrum P lin,mass (k) 5. Choose value of  8 6. Calculate b(M), n(M), d c, theory (M)  d c, theory (b) or b(d c, theory ) 7. Choose  v 8. Choose d c 9. Calculate non-linear halo power spectrum P nl,halo (k s ) for this d c 10. Fourier transform power spectrum   nl,halo (s)  s 0,theory Model predictions for d c -s 0 Padilla & Baugh, MNRAS, 2002, 329, 431.

10. Clustering dependence on group mass: CDM predictions 6/6. Cosmology Reference model:  m h 0 =0.21 h 0 =0.7  b /  m =0.2  8 =0.95  v =3.5 d c -s 0 for 2PIGG  Constraints

11. Clustering dependence on group mass: Constraints from s 0 6/6. Cosmology mh0mh0 b/mb/m 88  v /100kms -1

12. Clustering dependence on group mass: Constraints from s 0 6/6. Cosmology mh mh mh mh Percival et al. 2002

13. Project one: matching the clustering of groups with non-gaussian initial fluctuations

14. Project two: use non-gaussian simulations to study higher order correlations and compare to results from the 2dFGRS

15. NETWORK-WIDE PROJECT

16. Telescopes: ESO: Paranal and La Silla CTIO GEMINI CARNEGIE: Magellan Las Campanas