フェルミ衛星による活動銀河核からのガンマ線観測
林田将明(KIPAC/SLAC, Stanford Univ. & 京都大学)
for the Fermi-LAT collaboration

Supernova Remnants - Spatially Resolved

Note: LAT does not resolve Cas A
Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)

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The Fermi LAT 1FGL

Extragalactic Sky

2697 extragalactic sources among 1451 source (630 unID)

mostly AGNs, mostly blazar
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Credit: Fermi Large Area Telescope Collaboration

outline• Blazar– Fermi view of blazar– jet structure– blazar emission model• radio galaxies (“misaligned” blazar)– gamma-ray emission from ~pc to ~100 kpc• UHECR from AGNs?

Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)

4Over half the bright sources seen with LAT appear to
be associated with Active Galactic Nuclei (AGN)!
• Power comes frommaterial falling
toward asupermassive
black holee+ep+

• Some of thisenergy fuels a jetof high-energy
particles thattravel at nearly the
speed of light• Fermi LAT sees
primarily blazars,
for which the jet ispointed towardEarth.

5strong variability!!
(Abdo et al. 2010)(Abdo et al. 2010)
3C 273Asymmetry

Plateau

Green: 3-hour
Blue: 6-hour
Red: 1-day

3C 454.3

Doubling timescale is ~3 hours
From the requirement that !-! opacity(e.g., Dondi+95), there should be

relativistic beaming effect!!

<variability timescale>(3 hours)<minimum Doppler factor>(> 13)
Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)

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broad band emission
Mkn 421 (real simultaneous data)

boosting
factor : "#Inverse
ComptonE = !E’

Synchrotron

L = !(3+")L’strong flux andflat spectrum
in radiopreliminaryradio
Nov, 2010 CTA-Japan meetingTeV
林田将明 (KIPAC/SLAC, Kyoto)

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Blazar sequence
Flux (E>100 MeV)

photonindex between! Inverse
correlation

Epeak and luminosity
Mean: 2.40+/-0.02(Fossati et al. 1998)

FSRQ (Flat Spectrum Radio Quasar)
BL Lac objects
2
3
Selection/incompletenessbiases(Giommi et al. 1999;
Padovani et al. 2003,FSRQs
Padovani 2007)
BL Lacs! Origin of the sequence!

– Galaxy evolution throughreduction of fuel from
Unknown typesurrounding gas and dust
(Böttcher and Dermer 2002)
32(Abdo et al. 2010, 1LAC)

10-910-5.5

BL Lacs

photon index vs, z
012redshift (z)38in the HEAD meeting (in March 2010) by Roger Blandford(Sikora et al. 1994)

particles (e+/e-) are accelerated
in the collimated jet(bulk speed: $ > 10)• geometry-> one-zone model is still valid?

far (~pc) ?

• What is the seed photon for!-ray?

near ( < sub-pc) ?
Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)9

!-ray (LAT)!-ray photonindex (LAT)
X-ray

Light curves between
July 2008 to June 2009(~ 1 year)

optical-UV光学偏光度(PD)光学偏光角(EVPA)
Near-Infrared
RadioNature, Abdo et al. (2010) 463, 919–
Contact authors : 林田将明, G.Madejski

10Complex jet structure
ration of polarization angle lasts 20 days
20 daysemission zone locates
5! pc scale (~10 rg) from the BH
opt.

helical magnetic field?

PDEVPAbent jet!?
similar behaviors were observed in•PKS 1510-089 (Marscher et al. 2010, ApJ)
•3C 454.3 (Sasada et al., 2010, COSPAR)

emission zone in blazar
Energy densities as function ofdistance from BH (Sikora et al. 2009)0.01

0.1

r [pc]

110(model: $=20, Ldisk=1046 erg/s, Lsyc=1047 erg/s,
magnetic flux LB=1046 erg/s, MBH=109Msolar)

Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)

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The GeV Spectral Break in 3C 454.3!"!#$%&########'()*++,+-.++-/,#####################'()*++-01.++211#"34#5#6789#8%:7;&9#<=>?@4%A##(Abdo et al. 2010)

Peculiarly Constant!!

No strong evolution of Eb is found%$ > 0.5 -> should not bea simple cooling break
13 2010 CTA-Japan meeting
Nov,林田将明 (KIPAC/SLAC, Kyoto)

Model for spectral break
Finke and Dermer (2010)

KN effect due to Compton-Scattered Intrinsic electron spectral break
Ly & Radiation?
with both disk and broad line region radiation-> unlikely,,

14 2010 CTA-Japan meetingNov,

林田将明 (KIPAC/SLAC, Kyoto)

AGN are not all pointing toward us…

Centaurus A – AGN, Radio Galaxy
Composite image with Chandra (blue, X-rays),
APEX (Radio, red), ESO/WFI (true)15

Radio galaxies (RG)
FR-II :

FR-I :

bright hotspot
higher powerCore dominant
Lower power

Unified model:
Blazar: FSRQ --- BL Lac
RG:
FR II --- FR I I

difference only in the relativistic beaming effect ?
Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)

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Radio galaxies as “misaligned” blazar?
Abdo et al. (2010) (MAGN)

7 FR I and 4 FR II

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emission from core
NGC1275 (Abdo et al. 2009)

One-zone SSC model
works, but with smallbulk speed jet ($ = 1.8)

blazarradio galaxies

different originslayer
between(slow) GeV and TeV
spinelayermodel ?
Spine and layer

Cen A (Abdo et al. 2010)
Fermi
HESSspine (fast)layer (slow)(Tavecchio(e.g.,& Ghisellini,2008)
Ghiselliniet al.2005)

Resolving Giant Lobes with LAT
22 GHz!waves: Synchrotron

Cen A(Abdo et al. 2010,Science)E > 200 MeV

LAT PSF
Gamma-Rays: Inverse Compton

extended ~ 10 deg
Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)

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particle acceleration in 100’s kpc scale• LAT detected !-ray emission
requires 0.1-1 TeV electron in100’s kpc-scale lobes.

high-energy particleaccelerationin very large scale!!
（2nd order “Fermi”?)
Nov, 2010 CTA-Japan meeting(Moskalenko et al. 2009)35ox35o of 408 MHz image with directionsof Auger UHECR events (E > 57 EeV)
indicated (r=3.2d)

林田将明 (KIPAC/SLAC, Kyoto)20Ultra-high energy cosmic-ray from AGNs ?
(PAO, 2010, PRL)

Hillas diagramwith GZK cut off

AGN(PAO, 2010, PRL)

correlation with AGNs?

proton or Fe ?
(PAO, 2010, APh)black dot: E > 55 EeVBlue : AGNs < 75 Mpc (VVC)L - $ diagram•Sources with jet Lorentz
factor $ must have jet power
L exceeding heavy solid anddot-dashed curves toaccelerate p and Fe
respectively, to E = 1020 eV.

•Upper limits to L vs. $defined by competition
between synchrotron losses
and acceleration time (dashedlines), and synchrotron losses
and available time (dottedlines).

(Dermer & Razzaque, airXiv:1004.4249)
林田将明 (KIPAC/SLAC, Kyoto)

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Luminosity Density of !-ray Galaxies from Fermi Data•

1LAC AGNs

!

––

FSRQs
BL Lac––Misaligned Radio Galaxies
Starburst (and Star-forming)

Need adequate
luminosity density and ! Fermi data favors high-Z
ion acceleration by BL
number of sources
Lacs/FR1 radio galaxies
within GZK radius

Dermer & Razzaque (2010)(Dermer & Razzaque, airXiv:1004.4249)
林田将明 (KIPAC/SLAC, Kyoto)23Summary of AGNs
• Fermi-LAT detect 682 AGNs in the 1st catalog– blazar sequence looks OK!
• Location of !-ray emission :– blazar : not only at sub-pc, but also at pc scale– Radio Galaxies : not only at core (pc), but also at lobe (Mpc)

Gamma-ray can also be generated far from BH !!
• Geometry :– complex jet structure (bent jet? helical magnetic field?)– classical one-zone model is too simple!!
– multi-zone? (spine and layer?)• Gamma-ray emission mechanism :– Inverse-Compton with either UV or IR photons
depending on the location of emission region• dddd• sss

Nov, 2010 CTA-Japan meeting

林田将明 (KIPAC/SLAC, Kyoto)28