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Physics of blazar heatingThe intergalactic medium
Galaxy clusters
The Physics and Cosmology of TeV Blazars
Christoph Pfrommer1
in collaboration with
Avery E. Broderick2, Phil Chang3, Ewald Puchwein1, Volker Springel1
1Heidelberg Institute for Theoretical Studies, Germany2Perimeter Institute/University of Waterloo, Canada
3University of Wisconsin-Milwaukee, USA
Aug 30, 2012 / ICM theory/computation workshop, Michigan
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Outline
1 Physics of blazar heatingPropagation of TeV photonsPlasma instabilities in beamsImplications
2 The intergalactic mediumBlazar luminosity densityThermal history of the IGMProperties of blazar heating
3 Galaxy clustersBimodality of core entropiesAGN feedbackChallenges and Conclusions
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
The TeV gamma-ray skyThere are several classes of TeV sources:
Galactic - pulsars, BH binaries, supernova remnants
Extragalactic - mostly blazars, two starburst galaxies
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Propagation of TeV photons
1 TeV photons can pair produce with 1 eV EBL photons:
γTeV + γeV → e+ + e−
mean free path for this depends on the density of 1 eV photons:→ λγγ ∼ (35 . . . 700) Mpc for z = 1 . . . 0→ pairs produced with energy of 0.5 TeV (γ = 106)
these pairs inverse Compton scatter off the CMB photons:→ mean free path is λIC ∼ λγγ/1000→ producing gamma-rays of ∼ 1 GeV
E ∼ γ2ECMB ∼ 1 GeV
each TeV point source should also be a GeV point source
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
What about the cascade emission?
Every TeV source should be associated with a 1-100 GeV gamma-rayhalo – not seen! → limits on extragalactic magnetic fields?
expected cascade
Fermiconstraints
TeV spectra
TeV detections
Neronov & Vovk (2010)
emission
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Missing plasma physics?
How do beams of e+/e− propagate through the IGM?
plasma processes are important
interpenetrating beams of charged particles are unstable
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Two-stream instability: mechanismwave-like perturbation with k ||vbeam, longitudinal charge oscillationsin background plasma (Langmuir wave):
initially homogeneous beam-e−:attractive (repulsive) force by potential maxima (minima)
e− attain lowest velocity in potential minima → bunching up
e+ attain lowest velocity in potential maxima → bunching up
p
Φ
e e− −
p
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Two-stream instability: mechanismwave-like perturbation with k ||vbeam, longitudinal charge oscillationsin background plasma (Langmuir wave):
beam-e+/e− couple in phase with the background perturbation:enhances background potential
stronger forces on beam-e+/e− → positive feedback
exponential wave-growth → instability
p
Φ
e−
e+
e−
+e
e e− −
p
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Two-stream instability: momentum transfer
particles with v & vphase:pair momentum → plasma waves: growing modes/instability
particles with v . vphase:plasma wave momentum → pairs: damping (Landau damping)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Oblique instabilityk oblique to vbeam: real word perturbations don’t choose “easy”alignment =
∑all orientations
greater growth rate than two-stream: ultra-relativistic particlesare easier to deflect than to change their parallel velocities(Nakar, Bret & Milosavljevic 2011)
Bret (2009), Bret+ (2010)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
Beam physics – growth rates
IC
obliq
ue
plasma phenomenaexcluded for collective
Broderick, Chang, C.P. (2012)
consider a light beampenetrating intorelatively dense plasma
maximum growth rate
∼ 0.4 γnbeam
nIGMωp
oblique instability beatsIC by factor 10-100
assume that instabilitygrows at linear rate upto saturation
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Propagation of TeV photonsPlasma instabilities in beamsImplications
TeV emission from blazars – a new paradigm
γTeV + γeV → e+ + e− →
IC off CMB → γGeV
plasma instabilities → heating IGM
absence of γGeV’s has significant implications for . . .
intergalactic B-field estimates
γ-ray emission from blazars: spectra, background
additional IGM heating has significant implications for . . .
thermal history of the IGM: Lyman-α forest
late time structure formation: dwarfs, galaxy clusters
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
TeV blazar luminosity density: today
Broderick, Chang, C.P. (2012)
collect luminosity of all 23TeV blazars with goodspectral measurements
account for the selectioneffects (sky coverage,duty cycle, galacticoccultation, TeV flux limit)
TeV blazar luminositydensity is a scaledversion (ηB ∼ 0.2%) ofthat of quasars!
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
Unified TeV blazar-quasar model
Broderick, Chang, C.P. (2012)
Quasars and TeV blazars are:
regulated by the samemechanism
contemporaneouselements of a single AGNpopulation: TeV-blazaractivity does not lagquasar activity
→ assume that they traceeach other for all redshifts!
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
Evolution of the heating rates
10 5 2 11+z
1020.1
1
10
102
103
HeatingRates[eVGyr
1 ]photoheatingstandard blazarstandard blazar fitoptimistic blazaroptimistic blazar fit
10x larger
heating
blazar heating
HI,HeI−/HeII−reionization
photoheating
Chang, Broderick, C.P. (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
Blazar heating vs. photoheating
total power from AGN/stars vastly exceeds the TeV power of blazars
TIGM ∼ 104 K (1 eV) at mean density (z ∼ 2)
εth =kT
mpc2 ∼ 10−9
radiative energy ratio emitted by BHs in the Universe (Fukugita & Peebles 2004)
εrad = η Ωbh ∼ 0.1× 10−4 ∼ 10−5
fraction of the energy energetic enough to ionize H I is ∼ 0.1:
εUV ∼ 0.1εrad ∼ 10−6 → kT ∼ keV
photoheating efficiency ηph ∼ 10−3 → kT ∼ ηph εUV mpc2 ∼ eV(limited by the abundance of H I/He II due to the small recombination rate)
blazar heating efficiency ηbh ∼ 10−3 → kT ∼ ηbh εrad mpc2 ∼ 10 eV(limited by the total power of TeV sources)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
Thermal history of the IGM
20 10 5 2 11+z
103
104
105T [K
]
only photoheatingstandard BLFoptimistic BLF
Chang, Broderick, C.P. (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
Evolution of the temperature-density relation
no blazar heating with blazar heating
Chang, Broderick, C.P. (2012)
blazars and extragalactic background light are uniform:→ blazar heating rate independent of density→ makes low density regions hot→ causes inverted temperature-density relation, T ∝ 1/δ
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Blazar luminosity densityThermal history of the IGMProperties of blazar heating
Blazars cause hot voids
no blazar heating with blazar heating
Chang, Broderick, C.P. (2012)
blazars completely change the thermal history of the diffuseIGM and late-time structure formation
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Entropy evolution
temperature evolution
20 10 5 2 11+z
103
104
105
T [K
]
only photoheatingstandard BLFoptimistic BLF
entropy evolution
20 10 5 2 11+z
0.1
1
10
102
Ke [keV
cm2]
only photoheatingstandard BLFoptimistic BLF
C.P., Chang, Broderick (2012)
evolution of entropy, Ke = kTn−2/3e , governs structure formation
blazar heating: late-time, evolving, modest entropy floor
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
When do clusters form?
mass accretion history
11 + z
1012
1013
1014
1015
M20
0c [
MO • ]
z0.5 = 0.95
z0.5 = 0.86
z0.5 = 0.70
z0.5 = 0.55
z0.5 = 0.42
mass accretion rates
11 + z
0
1
2
3
4
5
S =
d lo
g M
200c
/ d
log
a (z
)C.P., Chang, Broderick (2012)
most cluster gas accretes after z = 1, when blazar heating canhave a large effect (for late forming objects)!
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Entropy floor in clusters
Cluster entropy profiles
Cavagnolo+ (2009)
ICM entropy at 0.1R200:
Opticallyselected
X−ray selected
Hicks+ (2008)
Do optical and X-ray/Sunyaev-Zel’dovich cluster observationsprobe the same population? (Hicks+ 2008, Planck Collaboration 2011)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Entropy floor in clusters
Cluster entropy profiles
Cavagnolo+ (2009)
Planck stacking of optical clusters
Planck Collaboration (2011)
Do optical and X-ray/Sunyaev-Zel’dovich cluster observationsprobe the same population? (Hicks+ 2008, Planck Collaboration 2011)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Entropy profiles: effect of blazar heating
varying formation time
0.01 0.10 1.00r / R200
10
100
1000
Ke [
keV
cm
2 ]
z = 0z = 0.5z = 1z = 2
M200 = 3 x 1013 MO •
optimistic blazar
varying cluster mass
0.01 0.10 1.00r / R200
10
100
1000
Ke [
keV
cm
2 ]
M200 = 1 x 1014 MO • , z = 0.5M200 = 3 x 1013 MO • , z = 0.5M200 = 1 x 1013 MO • , z = 0.5
optimistic blazar
C.P., Chang, Broderick (2012)
assume big fraction of intra-cluster medium collapses from IGM:
redshift-dependent entropy excess in cores
greatest effect for late forming groups/small clusters
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Gravitational reprocessing of entropy floors
no preheating + floor
preheated
no preheating
K = 25 keV cm0
Borgani+ (2005)
2
Borgani+ (2005)
greater initial entropy K0→ more shock heating→ greater increase in K0over entropy floor
net K0 amplification of 3-5
expect:
median Ke,0 ∼ 150 keV cm2
max. Ke,0 ∼ 600 keV cm2
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Cool-core versus non-cool core clusters
hotcool
Cavagnolo+ (2009)
time-dependent preheating + gravitational reprocessing→ CC-NCC bifurcation (two attractor solutions)
need hydrodynamic simulations to confirm this scenario
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Cool-core versus non-cool core clusters
hotcool
t < tmerger
late forming,
merger coolt > tcool
Cavagnolo+ (2009)
early forming,
time-dependent preheating + gravitational reprocessing→ CC-NCC bifurcation (two attractor solutions)
need hydrodynamic simulations to confirm this scenario
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
How efficient is heating by AGN feedback?
1 10 100
10-2
100
102
104
Eb, 2500(kTX = 0.7 keV)
Eb, 2500(kTX = 1.2 keV)
Eb, 2500(kTX = 2.0 keV)
Eb, 2500(kTX = 3.5 keV)
Eb, 2500(kTX = 5.9 keV)
cool cores non-cool cores
Eca
v=
4PV
tot[1
058er
g]
Ke,0 [keV cm2]
C.P., Chang, Broderick (2011)
AGNs cannot transform CC to NCC clusters (on a buoyancy timescale)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
How efficient is heating by AGN feedback?
1 10 100
10-2
100
102
104
Eb, 2500(kTX = 0.7 keV)
Eb, 2500(kTX = 1.2 keV)
Eb, 2500(kTX = 2.0 keV)
Eb, 2500(kTX = 3.5 keV)
Eb, 2500(kTX = 5.9 keV)
cool cores non-cool cores
Eca
v=
4PV
tot[1
058er
g]
Ke,0 [keV cm2]
C.P., Chang, Broderick (2011)
AGNs cannot transform CC to NCC clusters (on a buoyancy timescale)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
How efficient is heating by AGN feedback?
1 10 100
10-2
100
102
104
Eb, 2500(kTX = 0.7 keV)
Eb, 2500(kTX = 1.2 keV)
Eb, 2500(kTX = 2.0 keV)
Eb, 2500(kTX = 3.5 keV)
Eb, 2500(kTX = 5.9 keV)
cool cores non-cool cores
Eca
v=
4PV
tot[1
058er
g]
Ke,0 [keV cm2]
C.P., Chang, Broderick (2011)
AGNs cannot transform CC to NCC clusters (on a buoyancy timescale)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
How efficient is heating by AGN feedback?
1 10 100
10-2
100
102
104
Eb, 2500(kTX = 0.7 keV)
Eb, 2500(kTX = 1.2 keV)
Eb, 2500(kTX = 2.0 keV)
Eb, 2500(kTX = 3.5 keV)
Eb, 2500(kTX = 5.9 keV)
cool cores non-cool cores
Eca
v=
4PV
tot[1
058er
g]
Ke,0 [keV cm2]
max K0
C.P., Chang, Broderick (2011)
AGNs cannot transform CC to NCC clusters (on a buoyancy timescale)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Challenges to the ChallengeChallenge #1 (unknown unknowns): inhomogeneous universe
universe is inhomogeneous and hence density of electrons change asfunction of positioncould lead to loss of resonance over length scale spatial growthlength scale (Miniati & Elyiv 2012)we have reasons to believe that the instability is not appreciably slowedin the presence of even dramatic inhomogeneities
plasma eigenmodes for the Lorentzian background case
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Challenges to the Challenge
Challenge #1 (unknown unknowns): inhomogeneous universeuniverse is inhomogeneous and hence density of electrons change asfunction of position
could lead to loss of resonance over length scale spatial growthlength scale (Miniati & Elyiv 2012)
we have reasons to believe that the instability is not appreciably slowedin the presence of even dramatic inhomogeneities
Challenge #2 (known unknowns): non-linear saturationwe assume that the non-linear damping rate = linear growth rate
effect of wave-particle and wave-wave interactions need to be resolved
Miniati and Elyiv (2012) claim that the nonlinear damping rate is linear growth rate
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Conclusions on blazar heating
explains puzzles in high-energy astrophysics:
lack of GeV bumps in blazar spectra without IGM B-fieldsunified TeV blazar-quasar model explains Fermi sourcecounts and extragalactic gamma-ray background
novel mechanism; dramatically alters thermal history of the IGM:
uniform and z-dependent preheatingrate independent of density → inverted T–ρ relationquantitative self-consistent picture of high-z Lyman-α forest
significantly modifies late-time structure formation:
group/cluster bimodality of core entropy valuessuppresses late dwarf formation (in accordance with SFHs):“missing satellites”, void phenomenon, H I-mass function
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Simulations with blazar heating
Puchwein, C.P., Springel, Broderick, Chang (2012):
L = 15h−1Mpc boxes with 2× 3843 particles
one reference run without blazar heating
three with blazar heating at different levels of efficiency(address uncertainty)
used an up-to-date model of the UV background (Faucher-Giguère+ 2009)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
The intergalactic medium
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Temperature-density relation
−2 −1 0 1 2 33.0
3.5
4.0
4.5
5.0
5.5
6.0
6.5
7.0
log 1
0(T/K
)
log10
(N HI
N H) =−8
no blazar heating
-7
-6
-5
-4-3 -2
Viel et al. 2009, F=0.1-0.8Viel et al. 2009, F=0-0.9
−2 −1 0 1 2 3
log10(Mpix/(h−1M))
intermediate blazar heating
-8
-7
-6
-5
-4
-3 -2
5 6 7 8 9 10
log10(ρ/〈ρ〉)
Puchwein, C.P., Springel, Broderick, Chang (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
The Lyman-α forest
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
The observed Lyman-α forest
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
The simulated Ly-α forest
0.0
0.2
0.4
0.6
0.8
1.0
tran
smitt
edflu
xfr
actio
ne−
τ
no blazar heatingintermediate b. h.
0 1000 2000 3000 4000velocity [km s−1]
0.00
0.05
0.10
0.15
0.200.25
∆e−τ
Puchwein+ (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Optical depths and temperatures
1.8 2.0 2.2 2.4 2.6 2.8 3.0redshift z
0.1
0.2
0.3
0.4
0.5
effe
ctiv
eop
tical
dept
hτ e
ff
no blazar heatingweak blazar heatingintermediate blazar heatingstrong blazar heatingViel et al. 2004Tytler et al. 2004FG ’08
2.0 2.2 2.4 2.6 2.8 3.0redshift z
2.0
2.5
3.0
3.5
tem
pera
ture
T(∆
)/(1
04 K)
no blazar heatingweak blazar heatingintermediate blazar heatingstrong blazar heatingBecker et al. 2011
Puchwein+ (2012)
Redshift evolutions of effective optical depth and IGM temperaturematch data only with additional heating, e.g., provided by blazars!
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Ly-α flux PDFs and power spectra
10−1
100
101
z = 2.52
no blazar heatingweak blazar heatingintermediate blazar heatingstrong blazar heatingKim et al. 2007
0.0 0.2 0.4 0.6 0.8 1.0transmitted flux fraction
10−1
100
101
z = 2.94
oftr
ansm
itted
flux
frac
tion
tuned UV background
Puchwein+ (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Voigt profile decomposition
decomposing Lyman-α forest into individual Voigt profiles
allows studying the thermal broadening of absorption lines
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Voigt profile decomposition – line width distribution
0 10 20 30 40 50 60b [kms−1]
0.00
0.01
0.02
0.03
0.04
0.05
0.06
0.07
0.08
ofb
[skm−1
]NHI > 1013cm−2
2.75< z< 3.05no blazar heatingweak blazar heatingintermediate blazar h.strong blazar heatingKirkman & Tytler ’97
Puchwein+ (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Lyman-α forest in a blazar heated Universe
improvement in modelling the Lyman-α forest is a direct consequenceof the peculiar properties of blazar heating:
heating rate independent of IGM density → naturally producesthe inverted T–ρ relation that Lyman-α forest data demand
recent and continuous nature of the heating needed to matchthe redshift evolutions of all Lyman-α forest statistics
magnitude of the heating rate required by Lyman-α forest data∼ the total energy output of TeV blazars (or equivalently ∼ 0.2%of that of quasars)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Dwarf galaxy formation – Jeans mass
thermal pressure opposes gravitational collapse on small scales
characteristic length/mass scale below which objects do not form
hotter IGM → higher IGM pressure → higher Jeans mass:
MJ ∝c3
s
ρ1/2 ∝
(T 3
IGM
ρ
)1/2
→ MJ,blazar
MJ,photo≈(
Tblazar
Tphoto
)3/2
& 30
→ depends on instantaneous value of cs
“filtering mass” depends on full thermal history of the gas:accounts for delayed response of pressure in counteractinggravitational collapse in the expanding universe
apply corrections for non-linear collapse
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Dwarf galaxy formation – Filtering mass
106
108
1010
1012
MF
[ h-1
MO • ]
linear theorynon-linear theoryoptimistic blazarstandard blazaronly photoheating
1 + δ = 1, zreion = 10
10 11 + z
1
10
MF,
bla
zar /
MF
non−linear theory
blazar heatingonly photoheating
linear theoryM ~ 10 MF
M ~ 10 MF10
11o
o
C.P., Chang, Broderick (2012)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Peebles’ void phenomenon explained?
mean density
106
108
1010
1012
MF
[ h-1
MO • ]
linear theorynon-linear theoryoptimistic blazarstandard blazaronly photoheating
1 + δ = 1, zreion = 10
10 11 + z
1
10
MF,
bla
zar /
MF
void, 1 + δ = 0.5
106
108
1010
1012
MF
[ h-1
MO • ]
linear theorynon-linear theoryoptimistic blazarstandard blazaronly photoheating
1 + δ = 0.5, zreion = 10
10 11 + z
1
10
MF,
bla
zar /
MF
C.P., Chang, Broderick (2012)
blazar heating efficiently suppresses the formation of void dwarfswithin existing DM halos of masses < 3× 1011 M (z = 0)
may reconcile the number of void dwarfs in simulations and thepaucity of those in observations
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
“Missing satellite” problem in the Milky Way
Springel+ (2008)
Dolphin+ (2005)
Substructures in cold DM simulations much more numerous thanobserved number of Milky Way satellites!
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
When do dwarfs form?
10 Myr
100 Myr
1 Gyr
M110
Dolphin+ (2005)
10 Gyr
isochrone fitting for different metallicities → star formation histories
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
When do dwarfs form?
τ formred: > 10 Gyr, z > 2
Dolphin+ (2005)
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Milky Way satellites: formation history and abundance
satellite formation time
not observed!late forming satellites (< 10 Gyr)
Maccio & Fontanot (2010)
satellite luminosity function
linear theory
non−linear theory
no blazar heating:
Maccio+ (2010)
blazar heating suppresses late satellite formation, may reconcilelow observed dwarf abundances with CDM simulations
Christoph Pfrommer The Physics and Cosmology of TeV Blazars
Physics of blazar heatingThe intergalactic medium
Galaxy clusters
Bimodality of core entropiesAGN feedbackChallenges and Conclusions
Galactic H I-mass functionMo+ (2005)
H I-mass function is too flat (i.e., gas version of missing dwarf problem!)
photoheating and SN feedback too inefficient
IGM entropy floor of K ∼ 15 keV cm2 at z ∼ 2− 3 successful!
Christoph Pfrommer The Physics and Cosmology of TeV Blazars