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The Dipole Anisotropy of the 2MASS Redshift Survey Pirin Erdoğdu (University of Nottingham) and the 2MRS Team MNRAS, in press.

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Presentation on theme: "The Dipole Anisotropy of the 2MASS Redshift Survey Pirin Erdoğdu (University of Nottingham) and the 2MRS Team MNRAS, in press."— Presentation transcript:

1 The Dipole Anisotropy of the 2MASS Redshift Survey Pirin Erdoğdu (University of Nottingham) and the 2MRS Team MNRAS, in press

2 OUTLINE  What is the 2MASS Redshift Survey?  What is the acceleration on our Local Group of galaxies?  Why do I think I am right?

3 Main Assumptions  CMB dipole is due to the motion of the Sun.  Linear theory of density perturbations is acceptable.  The 2MASS has constant mass-to-light ratio and linear bias.

4 The 2MASS Redshift Survey z ≤ 0.01 0.01 < z ≤ 0.025 0.025 < z < 0.05 0.05 ≤ z

5 If we have a perfect 3-dimensional galaxy catalogue with same mass, with no selection effects, no z-distortions and with linear biasing then Linear theory: From CMB: v LG = 627 km/sec towards l=273 o and b=29 o From galaxy cat. Number Weighting Technique

6 The 2MRS Redshift Distribution

7 The Rocket Effect (Kaiser, 1987) cz=H 0 r + (v pec - v(0)).(r/r) cz=H 0 r + (v pec - v(0)).(r/r) LG Gal 1 with d=100 km/sec v pec = 20 km/sec Thus calculated distance=120 km/sec Thus calculated dipole= 44% less than the real dipole Gal 2 with d = 100 km/sec v pec= -20 km/sec Thus calculated distance=80 km/sec Thus calculated dipole = 64 % more than the Real dipole Net effect: A spurious contribution to the LG dipole from All the galaxies.

8 If we have a perfect 2-dimensional galaxy catalogue with no selection effects, constant mass-to- light ratio and with linear biasing then since Flux Weighting Technique

9 Luminosity Weighting Function

10 Notice the Zone of Avodiance Notice the Zone of Avodiance

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13 Shapley Centaurus Hydra Star: CMB Triangle: 2MRS – Lum Weighted Triangle: 2MRS-Num Weighted Circle: 2MASS by Maller etal 2003 Upside down Triangle: IRAS PSCz Dipole Upside down Triangle: 2MASS dipole of PSCz galaxies Triangle: 2MRS – Lum Weighted without Maffei 1, 2, Dwingeloo 1, IC342, M87 Blue square: Dipole from X- Ray Clusters (Kocevski & Ebeling 2005)

14 To summarise…  The flux weighted galaxy dipoles are better.  Most of the LG dipole is caused by the tug-of-war between the GA and Per-Pis. The dipole converges by ~ 60 Mpc/h.  If dipole converged β 2mrs = 0.4±0.1  Small discrepancy between LG and CMB dipoles are due to ZoA, 2nd and 3rd assumptions mentioned in the earlier slide and structure beyond. But no big deal!


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