The clustering of galaxy groups in the 2dFGRS (2PIGG) The clustering of 2PIGGs Project zero: CDM...
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Transcript of The clustering of galaxy groups in the 2dFGRS (2PIGG) The clustering of 2PIGGs Project zero: CDM...
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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:
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Clustering dependence on group mass from the 2PIGG
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Clustering dependence on group mass from the 2PIGG
2PIGG Subsamples:
Padilla & the 2dFGRS Team – Astro-ph/0402577
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Indicators of amplitude of clustering:
Relative bias:
s) = b2 ’(s)
Padilla & the 2dFGRS Team – Astro-ph/0402577
Clustering dependence on group mass from the 2PIGG
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Clustering length:
(s0) = 1
Indicators of amplitude of clustering:
Clustering dependence on group mass from the 2PIGG
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Clustering dependence on group mass:
Comparison withother cluster results
Padilla & the 2dFGRS Team – Astro-ph/0402577
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Project zero: CDM predictions and parameter constraints
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Clustering dependence on
group mass: Comparison with
CDM
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Clustering dependence on group mass: CDM predictions
mh0
h0
b/m
8
v
1. Choose mh0 and h0. Calculate = 1 - m
2. Calculate dc using luminosity function and geometry
3. Pick b/m
4. Calculate linear mass power spectrum Plin,mass(k)
5. Choose value of 8
6. Calculate b(M), n(M), dc, theory(M) dc, theory(b) or b(dc, theory)
7. Choose v
8. Choose dc
9. Calculate non-linear halo power spectrum Pnl,halo(ks) for this dc
10. Fourier transform power spectrum nl,halo(s) s0,theory
Model predictions for dc-s0
Padilla & Baugh, MNRAS, 2002, 329, 431.
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Clustering dependence on group mass: CDM predictions
6/6. Cosmology
Reference model:
mh0=0.21
h0=0.7
b/m=0.2
8=0.95
v=3.5
dc-s0 for 2PIGG Constraints
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Clustering dependence on group mass: Constraints from s0
6/6. Cosmology
mh0 b/m
8 v/100kms-1
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Clustering dependence on group mass: Constraints from s0
6/6. Cosmology
mh mh
Percival et al. 2002
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Project one: matching the clustering of groups with non-gaussian initial fluctuations
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Project two: use non-gaussian simulations to studyhigher order correlations and compare to
results from the 2dFGRS
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NETWORK-WIDE PROJECT
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Telescopes:
ESO: Paranal and La Silla
CTIO
GEMINI
CARNEGIE: Magellan Las Campanas