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The Fermi blazars divide. Gabriele Ghisellini Osservatorio Astronomico di Brera In collaboration with L. Maraschi and F. Tavecchio. Bright Fermi blazars. >100 with >10 s detection 57 FSRQs and 42 BL Lacs Redshift for all FSRQs and for 30 BL Lacs. FSRQs. TeV. - PowerPoint PPT Presentation
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The Fermi blazars The Fermi blazars dividedivide
Gabriele GhiselliniGabriele GhiselliniOsservatorio Astronomico di Brera
In collaboration with L. In collaboration with L. Maraschi and F. TavecchioMaraschi and F. Tavecchio
Bright Fermi blazarsBright Fermi blazars• >100 with >10>100 with >10 detection detection• 57 FSRQs and 42 BL Lacs57 FSRQs and 42 BL Lacs• Redshift for all FSRQs and for 30 Redshift for all FSRQs and for 30
BL LacsBL Lacs
Ghi
selli
ni, M
aras
chi,
Tave
cchi
o G
hise
llini
, Mar
asch
i, Ta
vecc
hio
2009
2009There is
a sequence
…
There is a se
quence…
-ra
y en
ergy
spe
ctra
l ind
ex
BL LacsBL Lacs
FSRQsFSRQs
TeV
Ghi
selli
ni, M
aras
chi,
Tave
cchi
o G
hise
llini
, Mar
asch
i, Ta
vecc
hio
2009
2009……desp
ite
despite
dramatic
dramatic
varia
bility
varia
bility
BL LacBL Lac
FerFermimi
454.3454.3
FerFermimi
AgilAgilee
05205288
FerFermimi
279279
FerFerm
im
i
MAGICMAGIC
Foss
ati e
t al
. 199
8; D
onat
o et
al.
Foss
ati e
t al
. 199
8; D
onat
o et
al.
2001
2001
TheThe “blazar“blazar sequence”sequence” FSRQsFSRQs
BL LacsBL Lacs
SteepSteep
FlatFlat
LL
Steep Steep FSRQsFSRQs
Flat BL Flat BL LacsLacs
The divideThe divide
The
blaz
ar d
ivid
eTh
e bl
azar
div
ide
~100~100
~100~100
PPjetjet~M~Maccraccrcc2 2 L Ldiskdisk>>~~
Celo
tti &
GG
200
8Ce
lott
i & G
G 2
008
Celo
tti &
GG
200
8,
Celo
tti &
GG
200
8, M
aras
chi+
200
8M
aras
chi+
200
8
Celo
tti &
GG
200
8,
Celo
tti &
GG
200
8, M
aras
chi+
200
8M
aras
chi+
200
8
GG
, Tav
ecch
io &
Ghi
rlan
da in
pre
p,
~100~100
LLdiskdisk~M~MEddEddcc22
LLdiskdisk~0.01M~0.01MEddEdd
cc22
PPjetjet~M~Maccraccrcc2 2 L Ldiskdisk>>~~
Ledl
ow &
Ow
enLe
dlow
& O
wen
Ghi
selli
ni &
Cel
otti
G
hise
llini
& C
elot
ti
2000
2000
Ghi
selli
ni &
Cel
otti
G
hise
llini
& C
elot
ti
2000
2000
Ledl
ow &
Ow
enLe
dlow
& O
wen
Disk accretion rate (Eddington Disk accretion rate (Eddington units)units)
LLdi
skdi
sk
PPje
tje
tJet power vs disk Lum.Jet power vs disk Lum.
e-p e-p decouplindecoupling g
Photon Photon trappingtrappingBL Lacs,
FSRQ
FRI,
FRII
~10~10-2-2
PP jetjet
LL diskdisk
Torus ~1-10 Torus ~1-10 pcpc
RRBLRBLR ~ L ~ Ldisk disk
UUBLRBLR= = constconst
1/21/2
RRTorusTorus~ L~ Ldisk disk
UUIRIR= const= const
1/21/2
strong coolingstrong coolingExternal ComptonExternal Compton
BLRBLRStandard
Standard
diskdisk
M>0.01MM>0.01MEdEd
dd
Far IRFar IR
MeVMeV
BLR <<0.2 BLR <<0.2 pcpc
RRBLRBLR ~ L ~ Lioniz ioniz
~No BLR ~No BLR (or very (or very small)small)
1/21/2
weak weak coolingcooling
SSC onlySSC onlyM<0.01MM<0.01MEE
dddd
TeVTeV
XX
TeVTeV
““ADAF disk”
ADAF disk”
Evolution? Evolution? (e.g. Cavaliere & D’Elia 2002)
• M should increase with redshiftM should increase with redshift• In the past more FSRQs (and In the past more FSRQs (and
FRII): positive evolution? FRII): positive evolution? • Now more BL Lacs (and FRI): Now more BL Lacs (and FRI):
negative evolution?negative evolution?• And taken together…? Similar to And taken together…? Similar to
radio-quiet or not?radio-quiet or not?
Conclusions/PredictionsConclusions/Predictions• The most powerful Fermi blazars The most powerful Fermi blazars
should be accreting near should be accreting near Eddington, and have the largest Eddington, and have the largest black hole massesblack hole masses
• Also radio-quiet should have much Also radio-quiet should have much weaker broad lines for M<0.01Mweaker broad lines for M<0.01MEddEdd
• As the survey goes on, including As the survey goes on, including weaker sources….weaker sources….
~forbidden
~forbidden
exce
pt
exce
pt
extra
ordinary
extra
ordinary
and ra
re sta
tes
and ra
re sta
tes
smaller M0948
Conclusions/PredictionsConclusions/Predictions• The most powerful Fermi blazars The most powerful Fermi blazars
should be accreting near should be accreting near Eddington, and have the largest Eddington, and have the largest black hole massesblack hole masses
• Also radio-quiet should have much Also radio-quiet should have much weaker broad lines for weaker broad lines for M<0.01MM<0.01MEddEdd
From Ho, 2008, ARAA.. For radio-quiet:From Ho, 2008, ARAA.. For radio-quiet:
“8. Low luminosity AGNs are not simply scaled-down versions of powerful AGNs. Their central engines undergo fundamental changes when the accretion rate << Eddington. In this regime, the BLR and obscuring torus disappear…
9. Below L~0.01% Eddington, the canonical accretion disk transforms into an inner vertically thick and radiatively inefficient accretion flow….”
MM22
MM
ADAFADAF (Narayan et (Narayan et al.)al.)
LLjetjet propto propto LLdiskdisk
1/21/2LLjet jet propto propto LLdiskdisk
By By modeling, modeling, we find we find physical physical parameters parameters in the in the comoving comoving frame.frame.
peakpeak is the is the energy of energy of electrons electrons emitting at emitting at the peak of the peak of the SEDthe SED
EGRET EGRET blazarsblazars
Low power slow cooling large peak
Big power Big power fast fast cooling cooling small small peakpeak
ttcoolcool 1/( 1/(peakpeak U) = R/c U) = R/c
peakpeakU = U = constconst
22
Power of jetsPower of jets
LLr r = radiation= radiationLLe e = relat. = relat. electronselectronsLLp p = protons= protonsLLB B = B-field= B-field RR
The power of blazar jetsThe power of blazar jets
~1017 cm
If one p per e-If one p per e-
Relat. Relat. electronselectrons
Magnetic FieldMagnetic Field
RadiationRadiation
Celo
tti &
Ghi
selli
ni
Celo
tti &
Ghi
selli
ni
2007
2007
High High powerpower
Powerful jets a
re not
Powerful jets a
re not
magnetically
dominated
magnetically
dominated
If one p per e-If one p per e-
Relat. Relat. electronselectrons
Magnetic FieldMagnetic Field
RadiationRadiation
Celo
tti &
Ghi
selli
ni
Celo
tti &
Ghi
selli
ni
2007
2007
Low powerLow power