Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys.,...
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Transcript of Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys.,...
Baryonic signature in the large-scale clustering of SDSS quasars
Kazuhiro Yahata <[email protected]>
Dept. of Phys., University of Tokyo.
Issha Kayo, Yasushi Suto, Matsubara Takahiko, Andy Connolly, Daniel Vanden Berk and others.
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Comparison of survey volumes
Galaxy Quasar
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We can investigate > 100Mpc/h structure.
EH
・ Eisenstein & Hu matter transfer function (1998)
Theoretical matter 2PCF
zero crossing
baryon bumpQuickTime˛ Ç∆
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B dependence
Predicted Ωb-dependence
Ωb↑・ slope↓・ zero-crossing scale↑
Λ dependence
Predicted ΩΛ-dependence
ΩΛ↑・ slope↓・ zero-crossing scale↑
We can derive constraints on Ωb and ΩΛ from these dependence.
Quasar sample selection
・ DR3 spectroscopic sample. ・ point source
・ Northern sky (80 ≦ α ≦ 300)
・ 15.0 ≦ mi,rc ≦ 19.1
・ 0.16 ≦ z ≦ 2.24
Quasar sample selection
sample
The quasar sample
NQSO = 20303
2D distribution
Mi’r
cN
redshift
2PCF
2PCF of SDSS quasars (Ωm=0.3,ΩΛ=0.7,h=0.7)
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It seems that the baryon bump exists in quasar 2PCF.
・ binning
We derive constraints on Ωb fromSDSS QSO clustering.
Fitting Proc
Fitting procedure
・ h = 0.7, (0.6, 0.8)
・ spatially flat: Ωb + ΩΛ + Ωd =1
・ scale independent bias: bQSO(z)
→fitting parameters: Ωb , ΩΛ
・ compute 2PCF (theory and observation) for grids of Ωb and ΩΛ. at linear regime, s ≧ 10Mpc/h
・ compute χ2
z evolution
Redshift evolution
・ Light-cone effect (Hamana, et al. 1998)
・ The Kaiser effect
・ evolution of scale independent bias
All above effects are scale independent.Thus we can introduce effective quasar bias:
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Chi2 h70
Result Δχ2
Approximate fit: 2.6Ωb + ΩΛ = 0.9
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Contours: 68%, 95%, 99.7%
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Chi2 h60
Δχ2 (h=0.60)
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2.6Ωb + ΩΛ = 0.9
h-dependence is weak.
Chi2 h70
Δχ2 (h=0.70)
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2.6Ωb + ΩΛ = 0.9
h-dependence is weak.
Chi2 h80
Δχ2 (h=0.80)
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B
2.6Ωb + ΩΛ = 0.9
h-dependence is weak.
Degeneracy
Due to the huge errors of large scale bins, the zero-crossing scale is not well constrained yet.
Future data are important in improving the constraints.
The 2PCFs preferred from the current analysis.
Summary
Summary
We derived constraints on Ωb and ΩΛ fromSDSS QSO 2PCF.
The result is approximately fitted to 2.6Ωb + ΩΛ=0.9±0.1
Future quasar data will constrain the zero crossing scale well. We willbreak the degeneracy between Ωb and ΩΛ.
END
End
(Next: Dust Extinction)