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The D istributions of Baryons in the Universe and the W arm H ot I ntergalactic Medium

The D istributions of Baryons in the Universe and the W arm H ot I ntergalactic Medium. Renyue Cen (Princeton University Observatory) Sept 26, 2013 @Anisotropic Universe: from microwaves to ultrahigh energies University van Amsterdam. Baryonic budget at z=0

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The D istributions of Baryons in the Universe and the W arm H ot I ntergalactic Medium

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  1. The Distributions of Baryons in the Universe and the Warm Hot Intergalactic Medium Renyue Cen (Princeton University Observatory) Sept 26, 2013 @Anisotropic Universe: from microwaves to ultrahigh energies University van Amsterdam • Baryonic budget at z=0 • Overall thermal timeline of baryons from z=1000  0 • Three separate redshift intervals in history • Conclusions

  2. The Bottom 5% in the Standard Model: Komatsu et al (2011) WMAP7 Planck Collaboration (2013)

  3. Warm-Hot Intergalactic Medium (WHIM) z~0 T=105-7Kelvin & Density=(1-300) mean density 100 Mpc/h Cen & Ostriker (1999)

  4. Power Spectrum in the Standard Model WHIM n=0.96, s8 = 0.8, Wxh2 = 0.126, H0 = 70 WHIM

  5. Budget, Structure, Thermal Timeline: Heating of the Cosmic Baryons by Fusion and Gravitational Energy  Redshift z=1100 30 – 10 10-6 6 - 2 2 - 0 Cosmological Recom- bination Real Dark Ages Pop III Stars 1stgen Galaxies 1stgen Quasars reheating 2nd gen Galaxies Quasars Final Reion Lya forest Majority of Quasars Ellipticals Majority of Galaxies Clusters LSS 1014Msun Mass(nonlinear) 106Msun 109Msun 1012Msun 106 K Gravitational shock heating Photo heating 104 K Photo heating 103 K Expansion cooling Temp 102 K Baryon budget evolution

  6. Epoch of Reionization Observational Data: z~20 to 6 1. SDSS QSOs: zri~6.0 2. CMB optical depth t=0.088 +- 0.015 Fan et al (2002) Which translates to zri=8.2-13.0 (2σ) (assuming a step function like transition from a totally neutral to totally ionized universe) SDSS 1030+0524 z=6.28 Komatsu et al (2011) WMAP7

  7. z~20 to 6 ab initio theory: the universe can be reionized by stars (mostly Pop II stars), producing optical depth that is consistent with WMAP7, but the process is NOT a step function like and spatially very inhomogeneous Trac, Cen, … (2013)

  8. A list of major observational probes of EoR • CMB: probing ionized hydrogen (bubbles) • 21cm in radio: probing neutral hydrogen • Ground based infrared surveys: probing Lya emission of galaxies • HST & JWST: probing rest-frame optical-UV continuum • High-z QSOs: absorption • High-z GRBs: absorption as well as SFR • IR radiation background

  9. Photoionization heated, T~104K Lyaforest: z~6 to 2 Cen et al (1994) • The standard model + gravitational instability + photoionization + • hydrodynamics • A successful model for Lya observed forest • A powerful method to determine Pk on small scales (~1Mpc), complementary to CMB and others z=3 zem3.6 QSO Womble et al (1996)

  10. Gravitational re-heating of the universe: z~2 to 0 The process is complex but the essential physics is rather simple: H(z) L(z)  vshock Cen & Ostriker (1999)

  11. z~20 ab initio theory: the universe is heated by waves breaking due to gravitational collapse of large-scale structure at moderate to low redshift Cen (1999)

  12. Capitalistic development of baryonic universe: z=2 to 0 Cen & Ostriker (1999)

  13. A list of major observational probes of z=2 to 0 IGM • QSO absorption lines (H, He, metals) • Emission lines (Lya, C IV, OVI, …) • X-ray emission from groups/clusters (lines and continuum) • SZ effects • Soft X-ray background (intensity, correlation function) • Cosmic rays produced in shocks  radio emission

  14. Conclusions • The intergalactic medium in the observable universe have three characteristic redshift ranges • z=100  20: universe expansion cooling • z=20  2: universe being heated by photoionization from star formation (nuclear energy) from 10 to 104K • z=2  0: universe being heated by hydrodynamic shock waves produced by gravitational collapse of large-scale structure from 104 to 106K --- IGM “measure” the temperature of the universe

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