the d istributions of baryons in the universe and the w arm h ot i ntergalactic medium
DESCRIPTION
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 - PowerPoint PPT PresentationTRANSCRIPT
The Distributions of Baryons in the Universe
and the Warm Hot Intergalactic Medium
Baryonic budget at z=0
Overall thermal timeline of baryons from z=1000 0
Three separate redshift intervals in history
Conclusions
Renyue Cen (Princeton University Observatory)Sept 26, 2013
@Anisotropic Universe: from microwaves to ultrahigh energiesUniversity van Amsterdam
The Bottom 5% in the Standard Model: The Bottom 5% in the Standard Model:
Komatsu et al (2011) WMAP7Planck Collaboration (2013)
Warm-Hot Intergalactic Medium (WHIM) z~0
T=105-7Kelvin &Density=(1-300)
mean density
Cen & Ostriker (1999)
Cosmological Recom-bination
RealDarkAges
Pop III Stars1stgen Galaxies1stgen Quasarsreheating
Lya forestMajority of QuasarsEllipticals
Majority ofGalaxiesClusters
LSS
Redshiftz=1100 30 – 10 6 - 2 2 - 010-6
2nd genGalaxiesQuasarsFinal Reion
Temp103 K
104 K
106 K
102 K
106Msun 1014Msun1012Msun109MsunMass(nonlinear)
Budget, Structure, Thermal Timeline: Budget, Structure, Thermal Timeline: Heating of the Cosmic Baryons by Fusion Heating of the Cosmic Baryons by Fusion
and Gravitational Energy and Gravitational Energy
Baryonbudget
evolution
1. SDSS QSOs: zzriri~6.0~6.0
SDSS 1030+0524z=6.28
Which translates to zzriri=8.2-13.0 (2σ)=8.2-13.0 (2σ)
(assuming a step function like transition from a
totally neutral to totally ionized universe)
2. CMB optical depth=0.088 +- 0.015=0.088 +- 0.015
Fan et al (2002)
Epoch of Reionization Observational Data: z~20 to 6
Komatsu et al (2011) WMAP7
z~20 to 6ab initio theory:
the universecan be
reionizedby 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 inhomogene
ous Trac, Cen, … (2013)
A list of major observational probes of EoR
CMB: probing ionized hydrogen (bubbles)
21cm in radio: probing neutral hydrogen
Ground based infrared surveys: probing Ly 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
Cen et al (1994)
z=3
zem3.6 QSOWomble et al (1996)
• The standard model + gravitational instability + photoionization +
hydrodynamics A successful model for Ly
observed forest A powerful method to
determine Pk on small scales (~1Mpc), complementary to CMB and others
Photoionization heated, T~104K Lyforest:
z~6 to 2
Gravitational re-heating of the universe: z~2 to 0
Cen & Ostriker (1999)
The process is complexbut the essential physics
is rather simple:H(z) L(z) vshock
z~20 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)
A list of major observational probes of z=2 to 0 IGM
QSO absorption lines (H, He, metals)
Emission lines (Ly, 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
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
Conclusions