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

……and X-ray and X-ray cavities,cavities,

Allen+, 2006, Allen+, 2006, Balmaverde+, Balmaverde+, 20082008

Power of Power of jets in jets in blazarsblazars

Tavecchio+ Tavecchio+ 20002000

Celotti, GG 2001Celotti, GG 2001

Power of Power of jets in jets in blazarsblazars

PPr r = radiation= radiation

PPe e = relat. = relat.

electronselectronsPPp p = protons= protons

PPB 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

Pje

t

10x

100x

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

• PPBB 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)

• PB = B Pjet B propto R-1

• Pe = e Pjet

1/2

•PB = B Pjet B propto R-1

•Pe = 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)

• PB = B Pjet B propto R-1

• Pe = 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)

• PB = B Pjet

• Pe = 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.)

PPjetjet propto propto

LLdiskdisk

1/21/2

PPjet 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 Ldiskdisk Red Red

quasarquasar

High M, Low LHigh M, Low Ldiskdisk Blue Blue

quasarquasar

Simple consequencesSimple consequences

• Small M, small PSmall M, small Pjetjet, large B, red, large B, red

BLRBLR UUBLRBLR ~ the same ~ the same

Large Large UUBB

Synchrotron peak frequencySynchrotron peak frequency

Inverse Compton peak Inverse Compton peak frequencyfrequency

Compton dominance Compton dominance

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

Reproducing the Reproducing the “old” sequence“old” sequence

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