Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys.,...
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![Page 1: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/1.jpg)
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.
![Page 2: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/2.jpg)
1
Comparison of survey volumes
Galaxy Quasar
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We can investigate > 100Mpc/h structure.
![Page 3: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/3.jpg)
EH
・ Eisenstein & Hu matter transfer function (1998)
Theoretical matter 2PCF
zero crossing
baryon bumpQuickTime˛ Ç∆
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![Page 4: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/4.jpg)
B dependence
Predicted Ωb-dependence
Ωb↑・ slope↓・ zero-crossing scale↑
![Page 5: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/5.jpg)
Λ dependence
Predicted ΩΛ-dependence
ΩΛ↑・ slope↓・ zero-crossing scale↑
We can derive constraints on Ωb and ΩΛ from these dependence.
![Page 6: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/6.jpg)
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
![Page 7: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/7.jpg)
sample
The quasar sample
NQSO = 20303
2D distribution
Mi’r
cN
redshift
![Page 8: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/8.jpg)
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.
![Page 9: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/9.jpg)
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
![Page 10: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/10.jpg)
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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![Page 12: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/12.jpg)
Chi2 h60
Δχ2 (h=0.60)
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2.6Ωb + ΩΛ = 0.9
h-dependence is weak.
![Page 13: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/13.jpg)
Chi2 h70
Δχ2 (h=0.70)
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2.6Ωb + ΩΛ = 0.9
h-dependence is weak.
![Page 14: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/14.jpg)
Chi2 h80
Δχ2 (h=0.80)
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2.6Ωb + ΩΛ = 0.9
h-dependence is weak.
![Page 15: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/15.jpg)
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.
![Page 16: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/16.jpg)
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.
![Page 17: Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.](https://reader034.fdocuments.in/reader034/viewer/2022042615/56649f555503460f94c79554/html5/thumbnails/17.jpg)
END
End
(Next: Dust Extinction)