First Fermi-LAT resultson AGNsand
SNRs/PWNe

Hideaki Katagiri
Hiroshima University
On behalf ofFermi LAT Collaboration

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20091

Introduction⎛u⎞Emax ~ 10 Z ⎜ ⎟ BμG L pc (eV )⎝c⎠15

Origin of cosmic rays
• AGN
– UHECR origin?
(ex. AUGER’s result)• SNRs/PWNe– The main objects toaccelerate the bulk of
the Galactic cosmic
rays?
(Recent results of
TeV, X-ray, etc.)

Hillas (1984)
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20092

Thanks to Gino (AGN),
Stefan (SNRs/PWNe)
and all members of the FERMI team!

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20093

Blazars
A class of AGNs
relativistic jetspointing close to the line of sight characteristics
 Compact radio core, flat or inverted spectrum, often superluminal
motion Extreme variability at all frequencies
 High optical and radio polarization
 2 broad classes
 FSRQs : bright broad (>2000 km/s) emission lines often evidences forthe “blue bump” (acc. disc) BL Lac: weak (EW<5 Å) emission lines no signatures of accretion
 Not major galaxy ~ 0.1-0.01%
1-10% (AGN) x 10% (radio loud) x 1-10% (beamed)
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20094

Gamma-ray loud Blazars
Although blazars comprise only a few per cent of the overall AGN
population, they dominate the extragalactic high-energy sky

3C454.3

1991

Year

1995

•

The Energetic Gamma Ray Experiment Telescope (EGRET)
discovered about 70 (3rd Catalog, Hartman et al 1999; >100
Sowards-Emmerd et al. 2003,2004) blazars emitting gammarays• About 20 sources were detected at E>200 GeV by the ACTs

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20095

Blazar Spectral Energy Distribution (SED)
The broadband continuum spectra of blazars are dominated by nonthermal emission and consist of two distinct, broad components.

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20096

Open questions about Blazar Physics
•
•
•
•
•
•
•
•
•
•
•

How are jets made by accreting black
holes?
How and where are jets accelerated (whythey have high Lorentz factors)?
How are jets focused to opening angles
less than a few degrees?
How do shocks, turbulence, instabilities,
jet bending and precession arise?
What is the jet matter content (electronproton vs. pair plasmas)?
How are the relativistic electrons
accelerated?
Which is the jet emission mechanism ?
How and where jets emit gamma-ray ?
What are the mechanisms producing
blazar variability?
Which is the blazar duty-cycle?
Etc…

Fermi-LAT is starting to give an answer to most of these questions
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20097

Fermi LAT & Blazars••

Sky Survey as primary operating mode
– Full sky observed every 2 orbits (3 hours)– Uniform exposure, with each region of the sky viewed for ~30 minutes
every 2 orbits (20% of the sky in the LAT FOV at any time)– EGRET sensitivity reached in days
Huge energy range, including largely unexplored band 10 GeV - 100 GeV.

LAT

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20098

Flaring Sources detection and Source Monitoring••

Automated Science Processing (ASP)– Transient detection: Uses source detection (pgwave) to find all
point sources in data from each epoch (6hr, day, week)– Follow-up monitoring: Runs full likelihood analysis on list fromsource detection step + “Data Release Plan” (DRP) sources– 2 × 10−6 ph cm−2 s−1 threshold (daily) for public release of non-DRP
Flare Advocates:– LAT scientists from Galactic and Extragalactic groups examine
output from ASP pipeline and perform follow-up analyses,
produce ATels, and propose ToOs
3C 454.3

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20099

ATels on Flaring Sources
DATE
ATel#
Title
2009-02-19 1933 Fermi LAT detection of Increased Flux from new gamma-ray blazar PKS 0250-225
2009-02-18 1932 Fermi LAT detection of a GeV flare from new gamma-ray blazar PKS 1118-056
2009-01-29 1919 Fermi-LAT detection of increased gamma-ray activity from the blazar PKS 0727-115
2009-01-22 1905 Fermi-LAT detection of renewed activity from the blazar PKS 1502+106
2009-01-19 1902 Fermi LAT detection of a high gamma-ray state from high-redshift blazar 0917+449
2009-01-12 1898 Fermi LAT detection of increasing gamma-ray activity of blazar PKS 0454-234
2009-01-09 1897 Fermi-LAT detection of another rapid GeV flare from the blazar PKS 1510-089
2009-01-08 1894 Fermi-LAT detection of a GeV flare from a source positionally consistent with PKS 1244-255
2009-01-04 1888 Fermi-LAT and Swift detection of a large GeV and optical flare from J123939+044409
2008-12-17 1877 Fermi LAT detection of a gamma-ray source positionally consistent with QSO B0133+47
2008-12-06 1864 Fermi LAT detections of increasing gamma ray activity of blazar 3C 279
2008-11-21 1850 Fermi LAT Observations of the Cygnus Region
2008-10-17 1788 Fermi LAT Detection of a New Gamma-ray Transient in the Galactic Plane: J0910-5041
2008-10-15 1784 Fermi/LAT detection of strong activity on short timescales of the blazar AO 0235+164
2008-10-08 1771 Fermi LAT Detection of Brightening of the Galactic Plane Source 3EG J0903-3531
2008-10-03 1759 Fermi LAT detections of gamma ray activity in three blazars: 3C 66A, PKS 0208-512, PKS 0537-441
2008-09-26 1744 Fermi LAT strong detection of blazar AO 0235+164 during outburst at Optical-to-Radio Wavelengths
2008-09-26 1743 Fermi LAT observations of the PKS 1510-089 outburst
2008-09-08 1707 Fermi LAT detection of 3C 273 in flaring state
2008-09-05 1701 Fermi LAT detection of a possible new gamma-ray flaring blazar: PKS 1454-354
2008-08-08 1650 GLAST LAT detection of a possible new gamma-ray flaring blazar: PKS 1502+106
2008-07-24 1628 GLAST-LAT detection of extraordinary gamma-ray activity in 3C 454.3

Public light curves for most of the detected flaring sources
are available at:
http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/
Hideaki Katagiri
第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200910

Flaring Blazars: 3C454.3(Abdo et al. 2009, ApJ, submitted)
Preliminary• Well-known blazar, at z = 0.859.
Detected by EGRET, AGILE. Very active(bright, rapidly variable) since 2000
•Fermi-LAT data show rapid, quasisymmetric, flares on a time scale of ~3days => With VLBI, optically thin to pairabsorption
Preliminary•First observation of a spectral break inthe spectrum of a high luminosity
blazar above 100MeV.
A possible interpretattion of the breakis that it is the direct signature of an
intrinsic
break
in
the
energydistribution of the radiating particles.
(Contact authors:G. Madejski & B. Lott)
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200911

Flaring Blazars:
PKS 1454−354

Contours:
EGRET
95,99%

Fermi -LAT data
demonstate that PSK 1454354 (z=1.424) is the mostprobable counterpart of theunidentified EGRET source
3EG J1500-3509•

The source showed afactor ∼5 increase of >100
MeV flux in 12 hours;
achromatic flux variations•

Typical FSRQ?
Large errors in X-ray leave
open different possibilities.

Hideaki Katagiri

Index

•

Flux

(Abdo et al. 2009,arXiv:0903.1713)

1day(Contact authors:L. Foschini)

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200912

Flaring Blazars: PKS 1502+106(Abdo et al. 2009, in preparation)•PKS 1502+106 (z=1.839) was not detected by EGRET•Extremely rapid flare, possibly the highest ΔL/Δt detected to date at
E>100 MeV.
•Time-asymmetric flare

Preliminary

20day•A MW Campaign started soon after its detection: Swift, INTEGRAL,
VLBA(MOJAVE),OVRO, Effelsberg, RATAN and Kanata observatories(Contact author:S. Ciprini)
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200913

Planned MW Campaign:PKS 2155-304 in low state(Abdo et al. 2009, arXiv:0903.2924)•

PKS 2155-304: HBL, z=0.116– 11 nightly obs. using HESS, ATOM, RXTE (+ Swift)– First multiwaveband observations of a blazar SED using Fermi and an ACT– Study correlated variability between various bands.

•Single zone SSC model fits
the time-averaged SED, butvariability patterns present
some challenges.
Electron energy distributionE^2 dN/dE
PRELIMINARY

E
Hideaki Katagiri(Contact authors: J. Chiang & B. Giebels)

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200914

Planned MW Campaign:PKS 2155-304•X-rays show large spectral variations,consistent with strong radiative cooling,
while > 0.2 TeV emission shows no evidenceof spectral variation despite factor ∼2changes in flux ⇒ Electrons producing the
X-rays are at higher energies than those
producing the 0.2-10 TeV emission.

HESS
Preliminary

FERMI•Optical-TeV correlation and ΔΓVHE < 0.2
strongly suggest optical is driving the TeV
variability.

X-ray•Lack of HE flux variability implies opticalphotons are produced by a distinct
population of electrons (multizone SSC)

Optical•X-ray flux correlation with HE spectral index(along with other correlations) defies easy
explanation in any model.
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200915

Other Multiwavelength Campaigns•

3C 454.3: radio, opt, UV, Swift•

BL Lac: opt, UV, X-ray•

PKS 0528+134: radio, IR, opt, UV, X-ray•

3C 273: radio, opt, X-ray•

3C279: radio, opt, X-ray•

Mrk 421, Mrk 501, 1ES 1959+654: radio, opt, X-ray, TeV (VERITAS,
MAGIC)•

3C66A, AO0235+16: radio, opt, X-ray<= Hayashida (SLAC)

Fermi-LAT synergies with other All-Sky monitor instruments like
MAXI will be of great importance for the MW study of Blazars
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200916

Observation with optical/NIR“KANATA” telescope
Detector: TRISPEC 3band (V, J, Ks)
simultaneousSpectroscopic&
PolarimetricObservation

Monitoring FERMI bright 30 blazars
3C454.3, AO0235+164, 3C66A, PKS1502+106 etc.
Sasada’s poster
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200917

3-month Survey: 205 LAT Bright Sources (LBS)(Abdo et al. 2009, arXiv:0902.1340)•205 sources with significance > 10σ (EGRET found 31).
•Typical 95% CL error radius is <10 arcmin. ∼1/3 show variability.
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200918

LAT Bright AGN Sample (LBAS)(Abdo et al. 2009, arXiv:0902.1559)•

125 non-pulsar sources at |b|>10°•

106 high-confidence (P>90%)
associations with AGNs: (LBAS)•

10 lower-confidence associations•

FSRQs: 57•

BLLacs: 42•

Uncertain class: 5•

Radiogalaxies: Cen A, NGC1275•

40% BLLacs (23% for EGRET)•

7 HBLs (3+1 for EGRET)•

9 unidentified (3EG: 96/181 at |b|>10°)

Contact Author:
Fukazawa
N

accidental

Contact Author:
Kataoka(Contact authors: LAT AGN Science Group)
Hideaki Katagiri

57 FSRQ
42 BLLac
5 of Uncertain class
2 Radio Galaxies

Preliminary

1

4Angular separation (sigma)
Θ95% ~0.14° (EGRET sample ~0.62°)

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200919

Key properties of the LBAS: Flux vs index
Preliminary
TS=100b=20, 80 deg.

FSRQ
BLLac
Uncertain
Radio Galaxies

TS=100b= 20 deg.

E< 3 GeV

Dim hard-spectrum sources are favored to be detected with the FermiLAT compared to EGRET
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200920

Key properties of the LBAS: Photon index
Preliminary
FSRQs

FSRQs

νFν

Number of sourcesall<Γ>= 2.33±0.01

BLLacsBL Lacs<Γ>=1.99±0.01

Photon index
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 2009

ν21

Key properties of the LBAS: Gamma-ray Spectra
Preliminary

3C454.3 (FSRQ)

AO 0235+165 (IBL)

Mkn501 (HBL)

Significant departures from pure power-law distributions for bright blazars!

If the spectral softening observed around fews GeV in flaring FSRQs will be
confirmed also for weaker sources, the fraction of BL Lac objects detectedby Fermi-LAT will be even greater than now over longer times.
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200922

Key properties of the LBAS: Luminosity vs redshift

Preliminary

FSRQ
BLLac
Uncertain
Radio galaxies

3

redshift

This distribution is similar to the EGRET one, but we are now see more
low-redshift BL Lac objects.
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200923

Blazar evolution by a reduction of the blackhole accretion power with time?
τ: optical depth of
reprocessed accretiondisk radiation incircumnuclear gas anddust, determined byaccretion rate

FSRQ

BL LacSequence Evolution from FSRQ to BL Lac
objects in terms of a reduction of fuel fromsurrounding gas and dust?
Hideaki Katagiri

Böttcher and Dermer (2002)

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200924

Key properties of the LBAS: Redshift distributions
Preliminary

N/NtotPhoton index

0.18

FSRQs
BZCat
LAT
Fermi−FSRQ
BZCat−FSRQ

Normalized Number of sources

0.16
0.14
0.12

3

0.10

2

0.08

FSRQ
BLLac
Uncertain
Radio galaxies

0.06
0.04
0.02
0.00
0.0

0.5

1.0

1.5

N/Ntot2.0
redshift

2.5

3.0

3

3.5

3

redshift

Preliminary

redshift

0.40

BL Lacs
BZCat
LAT
BZCat−BL Lac
Fermi−BL Lac

Normalized Number of sources

0.35
0.30
0.25

3

0.20

2

0.15
0.10
0.05
0.00
0.0

0.5

Hideaki Katagiri

1.0

1.5

2.0
redshift

2.5

3.0

3

3.5

redshift

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 20093
redshift25

Key properties of the LBAS: Log N - Log S
Preliminary• Euclidian space: slope=2.5

Blazar class

FSRQs
N(>S)[deg2]• « sky coverage » enables thelog N-LogS to be computed

slope
2.50±0.12

FSRQs

2.55 ±0.12

BLLacs2.32 ±0.15

10-7

S[cm-2 s-1]

BL Lacs
N(>S)[deg2]

All

10-7
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 2009

S[cm-2 s-1]
26

Conclusions (1)•These early results from the first months of the science missionof the Fermi- LAT demonstrate its exceptional capabilities toprovide important new knowledge about gamma-ray emission
from active galactic nuclei and blazars.

•

Current set of results are just the tip of the iceberg. As the FermiLAT data accumulate:– many more AGNs at lower flux levels will be detected– many more flaring AGNs will be detected

All this will help to improve our understanding ofsupermassive black holes.

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200927

SNRs/PWNe

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200928

SNRs in TeV view

Hadronicmodel2002～
PSF<0.1度
SNR RX J0852.0-4622 (Vela Jr.)

π0 bump

1GeV～2o

Leptonic
model

Aharonian et al. 2006

Surely accelerated
particles > TeV exist.
How about mechanism?

1GeV
29

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 2009

29

EGRET observation of SNRs
EGRET
Spark chamber onboard
CGRO(1991-1996）
Position determination
accuracy ～1deg.

5 2EG candidates（Esposito et al. 1996）
22 3EG candidates（Romero et al. 1999）

γ Cygni(>1GeV)30
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200930

S. Funk
FERMI First Symposium@TIT

LAT SNRcandidates(Abdo et al. 2009,arXiv:0902.1340)

•

•

•

Hideaki Katagiri

Positional coincident
sources with SNRs and
PWNe such as:– SNR W28, W44, W51,
IC443, Kookabrra,
MSH10-53 …
As seen for CTA1 andmany others, the LAT
detects many pulsars.
Pulsed emission andextension analysis
crucial for association.

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200931

An example – W28
NANTEN CO(J=1‐0)
10‐20km (2.5 – 4 kpc)

NANTEN2 CO(J=2‐1)
10‐20km (2.5 – 4 kpc)

0.8 deg.
Radio boundary
FERMI

GRO J1801‐
2320(EGRET
reanalysis)

3EG J1800‐2338

HESS(4, 5, 6 sigma)

Katagiri, Fukui

But the position and extension must
be carefully investigated…
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200932

S. Funk
FERMI First Symposium@TIT

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200933

S. Funk
FERMI First Symposium@TIT
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200934

S. Funk
FERMI First Symposium@TIT

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200935

Conclusion (2)• Several sources in the bright source catalog arepotentially associated with SNRs/PWNe.
• Bright TeV sources might not be bright GeV
sources (and vice versa)– Young SNRs not in bright source list
– Many pulsars, need extension measurement
for association

Exciting times ahead of us!
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200936

Backup slides

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200937

Fermi LAT & Blazars
Prompt
Blazars

detectionofflaringDaily sampled LC can be easily
obtained for most of the brightest
blazarsÆ
Variability
ontimescales >= 1 day can be wellinvestigated.
Intra-day (hours) variations canbe detected for the very bright
gamma-ray blazars.
Detailedspectralvariation
analysis and intra-bands delays
studies may be performed
Population Studies
Hideaki Katagiri(Atwood at al. 2009, arXiv:0902.1089)

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200938

Radio-Galaxies: NGC 1275
(Abdo et al. 2009, sub. to ApJ)••

NGC 1275, a.k.a. 3C84 or
Perseus A, is a nearby radiogalaxy containing a flatspectrum, compact (VLBIscale) blazar-like, variable
radio source
It has been detected in the
Fermi LAT data, at a muchhigher level than the upper
limit from EGRET. ⇒ variable,i.e., not cluster emission.

QuickTime™ e undecompressore TIFF (Non compresso)
sono necessari per visualizzare quest'immagine.

Please ask him!

(Contact Author: J. Kataoka)
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200939

Narrow‐Line Quasar PMN J0948+0022( Abdo et al., 2009, Submitted to ApJ)
Optical spectrum of narrow‐line Seyfert 1 type (usually
radio quiet). It shows only narrow permitted lines:
FWHM(Hβ) ~ 1500 km/s,
while all FSRQ have FWHM(Hβ) > 2000 km/s.
Radio emission is strongly variable
and with flat spectrum ‐> suggests Doppler boosting,now confirmed by LAT.

First γ‐ray detection of such an object
SED modeling shows this is a typical FSRQ, althoughwith a relatively low power.
Many questions open:•Is this a new type of γ‐ray emitting AGN?
•Are there other sources of this type?
•What is the impact of narrow‐lines?
(Contact authors:L. Foschini)
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200940

PKS1502+106 (OR103)
Aug 7thASP

LATV-bandopticalflux(10-11erg/sec/cm2)

V-bandpol-deg(%)

V-bandpol-ang(deg)July 31
Hideaki Katagiri

MET

Aug 10
we have also J,K-band data

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200941

Key properties of the LBAS: Flux distributions
Preliminary
mean
flux

Fermi
EGRET

weeklypeak
flux

EGRET mean flux
« 1234 VP»
EGRET peak flux:
maximum in 2-w VPs
peak/mean
flux ratio

Fermi mean flux:
3-m averaged
Fermi peak flux:
maximum in 1-w periods

Hideaki Katagiri

mean vspeak flux

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200942

Key properties of the LBAS: LBAS Sources in 3EG
EGRET vs FERMI photon index

33 AGNs/116 LAT-sources (30%)
in 3EG catalog with a comparable

Preliminary

Others are found at lower fluxes
FSRQs: 20
BLLacs: 11
Uncertain: 3
Radio galaxy:1
FSRQ
BLLac
Uncertain
Radio galaxies
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200943

Key properties of the LBAS: Evolution of Blazars<V/Vmax>: ratio between the comoving volume within which the source was
detected and the maximum volume available for its detection
Population uniformly distributed in Euclidian space, non evolving:<V/Vmax> ~ 0.5
Preliminary
Sample#objects<V/Vmax>

FSRQs

57

0.645±0.043

BLLacs420.473±0.046

All with z>0920.512±0.031

Positive evolution for FSRQs (more FSRQs in the past)Compatible with no evolution for BLLacs
Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200944

And more…
(Abdo et al. 2009, arXiv:0902.1340)

Hideaki Katagiri

第９回高宇連研究会「宇宙ジェットの多様性と普遍性」 愛媛大学; March 16-18, 200945