extragalactic jets: a new perspective
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Almost every galaxy hosts a BHAlmost every galaxy hosts a BH
99% are silent99% are silent
1% are active1% are active
0.1% have jets0.1% have jets
Extragalactic jets: a new Extragalactic jets: a new perspectiveperspective
G. Ghisellini in coll. with F. Tavecchio INAF-OABreraG. Ghisellini in coll. with F. Tavecchio INAF-OABrera
FRI-FRII & Blazars
SynchrSynchroo
Inverse Inverse ComptonCompton(also possible(also possiblehadronic hadronic models)models)
Radio IR Opt UV X MeV Radio IR Opt UV X MeV GeV GeV
Blazars: Spectral Energy DistributionBlazars: Spectral Energy Distribution
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001
TheThe “blazar“blazar sequence”sequence”FSRQs
BL LacsBL LacsLBLLBL and and HBLHBL
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001
peakpeakBB22
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
TeV BL LacsTeV BL Lacs
Low power slow cooling large peak
Big power Big power fast fast cooling cooling small small peakpeak
Power of Power of jets in jets in blazarsblazars
Power of Power of jets in jets in blazarsblazars
Power of Power of jets in jets in blazarsblazars
LLr r = radiation= radiation
LLe e = relat. = relat.
electronselectronsLLp p = protons= protons
LLB B = B-field= B-field RR
The power of blazar jetsThe power of blazar jets
Rdiss ~1017 cm
Ghisellini, Foschini, Tavecchio, Pian Ghisellini, Foschini, Tavecchio, Pian 20072007
AGILEAGILE!!3C 454.3 3C 454.3
SwifSwiftt
If one p per e-If one p per e-
Relat. Relat. electronselectrons
Magnetic FieldMagnetic Field
RadiationRadiation
Celo
tti &
Gh
isellin
i C
elo
tti &
Gh
isellin
i 2007
2007
High High powerpower
Powerful je
ts are
not
Powerful je
ts are
not
magnetically
dominated
magnetically
dominated
Celotti GG 2008Celotti GG 2008
Celo
tti G
G 2
008,
Mara
sch
i et
al.
C
elo
tti G
G 2
008,
Mara
sch
i et
al.
2008
2008
Disk accretion rate (Eddington Disk accretion rate (Eddington units)units)
LLd
isk
dis
k
PPje
tje
tJet power vs disk Lum.Jet power vs disk Lum.
e-p e-p decouplindecoupling g
Photon Photon trappingtrapping
BL Lacs, F
SRQ, QSO
GRBGRB
ss
PausePause
• Jet power is large. More than LJet power is large. More than Ldiskdisk
• Matter dominated. Not many pairsMatter dominated. Not many pairs
• LLBB is small is small
• Powerful jets Powerful jets mustmust be radiatively be radiatively inefficientinefficient
• Powerful jets do not deceleratePowerful jets do not decelerate
A new blazar sequenceA new blazar sequence
• Old one: based on 1 parameter: the observed luminosity
• Now: info on mass and accretion rate (spin? not yet)
• Info on jet power vs disk luminosity• Info on location of dissipation: must
be at some distance from BH. One zone is dominant (internal shocks?)
The key ideasThe key ideas
• Rdiss proportional to MBH
• RBLR proportional to (Ldisk)
UBLR=cost
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
1/2
Led
low
& O
wen
Gh
isellin
i &
Celo
tti
Gh
isellin
i &
Celo
tti
2001
2001
The key ideasThe key ideas
• Rdiss proportional to MBH
• RBLR proportional to (Ldisk) UBLR=cost
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
• LB = B Pjet B propto R-1
• Le = e Pjet
1/2
•LB = B Pjet B propto R-1
•Le = e Pjet
Celo
tti &
Gh
isellin
i C
elo
tti &
Gh
isellin
i 2008
2008
The key ideasThe key ideas• Rdiss proportional to MBH
• RBLR proportional to (Ldisk) UBLR=cost
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
• LB = B Pjet B propto R-1
• Le = e Pjet
peak propto U-1; U-1/2
1/2
The key ideasThe key ideas• Rdiss proportional to MBH
• RBLR proportional to (Ldisk)
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
• LB = B Pjet
• Le = e Pjet
peak propto U-1; U-1/2
The key ansatzThe key ansatz• Pjet always proportional to M
1/2
MM22
MM
ADAFADAF (Narayan et (Narayan et al.)al.)
LLjetjet propto propto
LLdiskdisk
1/21/2
LLjet jet propto propto
LLdiskdisk
Simple consequencesSimple consequences
• RRdissdiss propto M; R propto M; RBLRBLR propto propto
(L(Ldiskdisk))1/21/2
BLRBLR
Low M, High LLow M, High L Red Red quasarquasar
High M, Low LHigh M, Low L Blue Blue quasarquasar
Simple consequencesSimple consequences
• Small M, small LSmall M, small Ljetjet, large B, red, large B, red
BLRBLR UUBLRBLR ~ the same ~ the same
Large Large UUBB
Give me MGive me MBHBH
and Land Ldiskdisk (or (or
LLBLRBLR) and I will ) and I will
tell you the tell you the SED of the jet SED of the jet and its powerand its power
ConclusionsConclusions
• PPjetjet > L > Ldiskdisk
• Jets are matter dominatedJets are matter dominated• Link between M, M and observed SEDLink between M, M and observed SED• ““Blue” FSRQs may existBlue” FSRQs may exist• ““Red” low power FSRQs may existRed” low power FSRQs may exist• Implications about evolutionImplications about evolution
• GLAST + Swift + M + LGLAST + Swift + M + Ldiskdisk (or L (or LBLRBLR))
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001AGILE AGILE
GLASTGLAST
CTCT
SwifSwiftt
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001AGILE AGILE
GLASTGLAST
CTCT
SwifSwiftt
If one p per e-If one p per e-
Relat. Relat. electronselectrons
Magnetic FieldMagnetic Field
RadiationRadiation
Celo
tti &
Gh
isellin
i C
elo
tti &
Gh
isellin
i 2007
2007
Low powerLow power
TeV BL
Lacs
TeV BL
Lacs
Subluminal motion for all TeV Subluminal motion for all TeV sources?sources?
Mkn 421 appapp~ 0.03 – 0.1 (+-0.06)~ 0.03 – 0.1 (+-0.06)
H1426+428
appapp~ 2.09 (+-0.53)~ 2.09 (+-0.53)
Mkn 501 appapp~ 0.05 – 0.54 (+-0.15)~ 0.05 – 0.54 (+-0.15)
1959+650 appapp~ 0 ~ 0
2155-304 appapp~ 0.93 (+-0.31)~ 0.93 (+-0.31)
2344+514 appapp~ 0 – 1.15 (+-0.5)~ 0 – 1.15 (+-0.5)
Pin
er,
Pan
t &
Ed
ward
s
Pin
er,
Pan
t &
Ed
ward
s
2008
2008
Cospatial fast spine & slow Cospatial fast spine & slow layerlayer
RRll~10~101616 cmcmRRss~10~101414 cm cm
10
10
15
15 c
m c
m
More seed photons for More seed photons for bothboth
’ = layerspine(1-layerspine)
The spine sees an enhanced Urad coming from the layer
Also the layer sees an enhanced Urad coming from the spine
The IC emission is enhanced wrt to the standard SSC model
BL LacBL Lac
RadiogalaxyRadiogalaxy
Ghisellini Tavecchio Chiaberge Ghisellini Tavecchio Chiaberge 20052005
Tavecchio Ghisellini 2008Tavecchio Ghisellini 2008
spinspin
ee
layelayerr
Power of jetsPower of jets
Coordinated variability at Coordinated variability at different different
Mkn 421Mkn 421
TeV
PDS
MECS
LECS
RBLR~1018 cm
=10-20
~1017 cm
Dissipation here?
NO!
Dissipation here?Yes!
Leptonic models:Leptonic models:
Maraschi Ghisellini Celotti 1992Maraschi Ghisellini Celotti 1992
Dermer Schlickeiser 1993Dermer Schlickeiser 1993
Sikora Begelman Rees 1994Sikora Begelman Rees 1994
Blandford Levinson 1995Blandford Levinson 1995
Ghisellini Madau 1996Ghisellini Madau 1996
But see e.g.: But see e.g.: Mannheim 1993; Mannheim 1993; Aharonian 2002; Aharonian 2002; Rachen 2000 for Rachen 2000 for proton modelsproton models
Importance Importance
of of -rays-rays
If If -- important too many X- important too many X-
rays rays x,x,>1 (>10) >1 (>10)
RRblobblob large enough (>10 large enough (>101616 cm), cm),
but tbut tvarvar<1day R<1day Rblobblob <2.5x10 <2.5x101515
ttvarvar cm cm
Blob away from accretion disk X-Blob away from accretion disk X-ray corona (>10ray corona (>101717 cm) cm)Energy transport in inner Energy transport in inner
jet must be jet must be dissipationlessdissipationless
Rava
sio e
t al.
2000
Fossati
et
al.
1998
Fossati
et
al.
1998
Gamma-ray Gamma-ray blazarsblazars
GLASTGLAST
HESS+ HESS+ MAGICMAGIC
EGRET: ~60 blazarsEGRET: ~60 blazars
Cherenkov: 21 blazars (+1 Cherenkov: 21 blazars (+1 Radiogal)Radiogal)
The Universe The Universe becomes becomes opaque at opaque at z~0.1 at 1TeV z~0.1 at 1TeV at z~2 at 20 at z~2 at 20 GeVGeV
The VHE extragalactic gamma-ray sky2020 BL Lacertae (BL Lacertae (18 HBL + + 22 LBLLBL))))11 radiogalaxy (M87, radiogalaxy (M87, 16 Mpc16 Mpc))11 FSRQs (3C279, FSRQs (3C279, z=0.536z=0.536))
Name Redshift
Mkn 421 0.03Mkn 501 0.031ES 2344+514 0.044Mkn 180 0.0451ES 1959+650 0.047PKS 0548-322 0.069BL Lacertae 0.069BL Lacertae 0.069PKS 2005-489 0.071RGB 0152+017 0.080ON231 (W Comae) 0.102ON231 (W Comae) 0.102PKS 2155-304 0.116H1426+428 0.1291ES 0806+524 0.1381ES 0229+200 0.140H2356-309 0.1651ES 1218+30 0.1821ES 0347-121 0.1851ES 1101-232 0.1861ES 1011+496 0.212PG 1553+113 0.25-0.78
Extragalactic Extragalactic jets: a new jets: a new perspectiveperspective
o The blazar sequenceThe blazar sequenceo Power and content of jetsPower and content of jetso A new perspectiveA new perspective
G. Ghisellini in collaboration with F. G. Ghisellini in collaboration with F. TavecchioTavecchio
INAF – Osservatorio Astronomico di BreraINAF – Osservatorio Astronomico di Brera
ttcoolcool 1/( 1/(peakpeak U) = R/c U) = R/c
peakpeakU = U =
constconst
22
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