Ofer Lahav
Ofer Lahav Ofer Lahav
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30.06.2013
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The halo model – the ‘new biasing’ P(k) = P lin +P halo Truncates NFW fit with C=2.4§ 0.2 Using 2dF Groups Collister & Lahav, astro-ph/0412516
Clustering of Red vs. Blue 2dF galaxies Madgwick, Hawkins, Lahav & 2dFGRS team, astro-ph/0303668
- Page 1 and 2: Large Scale Structure at Low Redshi
- Page 3 and 4: LSS at low z • 2MRS/6dF The LG di
- Page 6 and 7: 2MASS Galactic chart F
- Page 8 and 9: 2MASS and follow-ups • 2MASS: 1.5
- Page 10 and 11: Dipole - weighting schemes by Numbe
- Page 12 and 13: Kocevski, Mullis & Ebeling, astro-p
- Page 14 and 15: The expected rms bulk motion h V 2
- Page 16 and 17: The revival of peculiar velocities
- Page 18 and 19: 7 Abell clusters 77 groups (>8) 20
- Page 20 and 21: From 2dF+CMB (6 parameter fit): Col
- Page 22 and 23: Brief History of ‘Hot Dark Matter
- Page 24 and 25: Data 2dFGRS Neutrino mass from Cosm
- Page 28 and 29: Correlation Function per Type dP /
- Page 30 and 31: Imaging CFHTLS Supernovae SDSS Spec
- Page 32 and 33: Input: magnitudes ANNz Collister &
- Page 34 and 35: DES + VISTA griz+YJHKs filters 10σ
- Page 36: Conclusions - in the Trio’s own w
The halo model – the ‘new biasing’<br />
P(k) = P lin +P halo<br />
Truncates NFW fit with C=2.4§ 0.2<br />
Using 2dF Groups<br />
Collister & <strong>Lahav</strong>, astro-ph/0412516
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