1. Large Scale Structure in 2MRS & 6dF Ofer Lahav (University College London) 6dF workshop, AAO/Sydney, 26-27 April 2005

2. LSS in 2MRS The Local Group Dipole Wiener reconstruction Future work with 2MRS+2MASS+6dF Pirin Erdogdu (Cambridge/Ankara), John Huchra (CfA), Ofer Lahav (UCL) & the 2MRS/6dF teams

3. F 2MASS Galactic chart

4. The Near IR Local Universe

5. 2MRS + mock ZoA ~25000 galaxies K s < 11.25 Huchra & 2MRS/6dF teams Random ZoA Interpolated ZoA

6. 2MRS vs. PSCz radial selection fn

7. Spectral PCA types in 2MASS 62% E’s in 2MASS 35% E’s in 2dF Madgwick, OL et al.

8. Dipole – weighting schemes  m 0.6 /b g / L/ (4  r 2 )  L = (7.67+- 1.02) x 10 8 L_sun h Mpc -3

9. Number and Flux dipoles in the LG frame 15 o @ 50 Mpc/h 24 o @ 130 Mpc/h  m < 0.37+- 0.20  < 0.57 +- 0.07 b 2mrs > 0.85 +- 0.15 (for  m = 0.30) Erdogdu et al., In preparation

10. Out to 200 Mpc/h- LG frame

11. Number and Flux dipoles in the CMB frame

12. Out to 200 Mpc/h – CMB frame

13. Dipole – Wiener reconstruction  0.4  0.6

14. 2MRS dipole directions @ 130 Mpc/h

15. Spherical harmonics

16. Wiener filtering ) Redshift distortion Signal/(Signal+Noise) Fisher, OL et al (1995)

17. WF 2MRS @ 2000 km/sec Erdogdu et al.

18. WF 2MRS @ 4000 km/sec

19. WF 2MRS @ 6000 km/sec

20. WF 2MRS @ 10000 km/sec

21. WF 2MRS velocity field CMB frame Erdogdu et al.

22. WF 2MRS velocity field LG frame

23. The Concordance Model Bulk flows are expected to have in linear theory: For  m < 1 lower amplitude and larger coherence length than in  m =1 universe Bulk flows are not sensitive to Dark Energy

24. Photometric redshifts

26. Photo-z Other work: * HYPERZ: Bolozonella et al., 2000, A&A, 363, 476 * Csabai et al,. 2003, AJ, 125, 580 ANNz: * Firth, Lahav & Somerville, 2003, MNRAS, 339, 1195 * Collister & Lahav, 2004, PASP, 116, 345 http://www.ast.cam.ac.uk/~aac Applications to: SDSS LRGs, Dark Energy Survey, 2MASS, …

27. Artificial Neural Network Output: redshift Input: magnitudes

28. SDSS data (ugriz; r < 17.77) ANNz (5:10:10:1) HYPERZ

29. DES (griz) 5-yr aloneDES + VISTA (YJHKs) Photo-z with ANNz  z = 0.13  z =0.08

30. 2MASS + photo-z  z = 0.02 z=0 cyan z=0.05 yellow z=0.08 red Collister & Lahav, ANNz

31. The 2dFGRS Team Members I.J. Baldry, C.M. Baugh, J. Bland-Hawthorn, T.J. Bridges, R.D. Cannon, S. Cole, C.A. Collins, M. Colless (PI),W.J. Couch, N.G.J. Cross, G.B. Dalton, R. DePropris, S.P. Driver, G. Efstathiou, R.S. Ellis, C.S. Frenk, K. Glazebrook, E. Hawkins, C.A. Jackson, O. Lahav, I.J. Lewis, S.L. Lumsden, S. Maddox (PI), D.S. Madgwick, S. Moody, P. Norberg, J.A. Peacock (PI), B.A. Peterson, W. Sutherland, K. Taylor http://www.mso.anu.edu.au/2dFGRS/ On 2dF Sociology see OL, astro-ph/0105351

32. 2dFGRS PhD students & collaborators Spectral classification (PCA): S. Folkes, S. Ronen, D. Madgwick Biasing from 2dF+CMB: S. Bridle Neutrino mass: O. Elgaroy Wiener Reconstruction: P. Erdogdu Stochastic Biasing: V. Wild Testing the halo model: A. Collister Ofer Lahav, UCL

33. Future work and interests @ London Compare predicted 2MRS peculiar velocities with observed 6dF pec vel. Combine 2MRS with 2MASS photo-z and 6dF Cosmological parameters Halo model & biasing The cosmic web Galaxy spectral classification Alexandra Abate, Sarah Bridle, Ofer Lahav, Anais Rassat

34. Clustering of Red vs. Blue 2dF galaxies Madgwick, Hawkins, Lahav & 2dFGRS team, astro-ph/0303668

35. What’s next? The 6dF NIR Galaxy Survey 2MASS NIR selected 150k redshifts (Southern hemisphere) Peculiar Velocities for 15k galaxies  Reconstruction of the MASS distribution

36. Great Walls of the Universe

37. The 2dFGRS Power Spectrum 50 Mpc/h8 Mpc/h Linear Non- linear

38. The latest2dFGRS power spectrum Cole et al. 2005

39. The SDSS LRG correlation fn (Eisenstein et al 2005)

40. Weighing Neutrinos with 2dFGRS Free streaming effect:   /  m  < 0.13 Total mass M< 1.8 eV   (Oscillations) (2dF) a Four-Component Universe ? Elgaroy, Lahav & 2dFGRS team, astro-ph/0204152, PRL   = 0.05 0.01 0.00

41. Absolute Masses of Neutrinos Based on measured squared mass differences from solar and atmospheric oscillations Assuming m 1 < m 2 < m 3   Elgaroy& Lahav, JCAP 03

42. Ratio of bulk flows with massive neutrinos  =0.04 Elgaroy&Lahav, NJP, 2005

43. Principal Component Analysis Projections on the First two eigen- spectra Cf. traditional line indices

44. PCA for data compression (by a factor ~1000)  = 0.5 pc 1 – pc 2 Madgwick, OL et al.

45. Correlation Function per Type Madgwick & 2dFGRS Why a power law? dP / n [1+  (r)] dV  r) = (r/r 0 ) - 

46. An empirical test of the halo model P gal (k) = P gal (1h) (k) + P gal (2h) (k) The 1-halo term depends on the halo mass function, the halo occupation number the radial distribution of the galaxies within the halo The 2-halo also term depends on the above, roughly P gal (2h) (k)= b gal 2 P dm (lin) (k) Each of the three terms can actually be measured directly from e.g 2dFGRS: Is the model satisfied for all, blue and red galaxies? Collister & OL, astro-ph/0412516

47. 2dFGRS galaxy groups Eke et al. 2004

48. An empirical test of the halo model Non-linear clustering P(k) = P lin (k) + P halo (k) Co-added profile of 2dF groups Truncated NFW fit with C = 2.4 +- 0.3 A. Collister & OL, astro-ph/0412516

49. The halo model P(k) = P lin (k) + P halo (k) Blue galaxies Red galaxies = (M/M 0 )  for M > M cut  1.05 § 0.19  = 0.88 § 0.17 C=3.9 § 0.5 C=1.3 § 0.2

50. Relative biasing (Blue/Red)

51. Future work and interests @ UCL Compare predicted 2MRS peculiar velocities with observed 6dF pec vel. Combine 2MRS with 2MASS photo-z and 6dF Cosmological parameters Halo model & biasing The cosmic web Galaxy spectral classification Alexandra Abate, Sarah Bridle, Ofer Lahav, Anais Rassat

52. University College London http://www.star.ucl.ac.uk http://www.star.ucl.ac.uk ASTROPHYSICS @ UCL 20 academic staff, 15 pos-docs, 35 PhDs, 15 support stuff Research Stellar Astrophysics, Star formation, Cosmology, Astro-Chemistry, Atmospheric Physics, Astro-biology, Instrumentation, Mill Hill Observatory & the MSSL Department