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