[PPT] - The cosmological evolution of blazars and the cosmic gamma- ray PowerPoint Presentation

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Yoshiyuki INOUE (Kyoto, JSPS fellow DC1)

Collabolators：Tomonori Totani, Susumu Inoue (Kyoto),

Masakazu. A. R. Kobayashi (NAO),

Jun Kataoka (Waseda), Rie Sato (JAXA)

Fermi Symposium

The cosmological evolution of blazars and the cosmic gamma- ray background in the Fermi era

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keV

Sreekumar et al. 1998

GeV MeV

AGNs Energy (keV) E^2 dJ/dE (keV/cm^2/s/sr)

What’s the origin of the cosmic gamma-ray background?

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1. MeV Background

AGNs (Rogers & Field ’91; Field & Rogers ’93;

Stecker, Salamon, & Done ’01; YI, Totani, & Ueda’08)

Supernovae (Clayton & Ward ‘75; Zdziarski

‘96; Watanabe+‘99)

MeV Dark Matter annihilation (Ahn &

Komatsu ’06, Rasera+‘06; Lawson & Zhitnitsky ‘07 )

MeV Blazars (Ajello+’09)

2. GeV Background

Blazars (Stecker & Salamon ’96; Chiang &

Mukherjee ’98; Mücke & Pohl 00; Narumoto & Totani ’06; Dermer ’07; YI & Totani ’09)

Galaxy Cluster Merger (Loeb & Waxman

‘00; Totani & Kitayama ’00)

GeV Dark Matter annihilation (e.g. Oda

et al. ’05)

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http://www.nasa.gov/

What is BLAZAR?

Inverse Compton

41 42 43 44 45 46 47 48 49

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5 10 Log10 L(erg s-1) Log10 E (eV)

GeV

Synchrotron

Log10 (Energy [eV]) Log10 (νLν [erg/s])

(Fossati+’97,’98; Kubo+’98; Donato +’01, but see also Padovani+’07)

SED Sequence

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Blazar

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Basic assumptions for blazar GLF construction

Blazar SED sequence.
AGN X-ray Luminosity Function (Ueda+’03:hereafter U03).

Assuming “Ljet, bol ∝Ldisk, X “. Constraining GLFs from EGRET data.

Blazar Gamma-ray Luminosity Function

(YI & Totani ’09)

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0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 0.01 0.1 1 dN/d(log10 z) Redshift z U03(q) U03(q,γ1) H05(q) H05(q,γ1) EGRET blazars 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 43 44 45 46 47 48 49 50 dN/d(log10 Lγ) log10 (Lγ [erg s-1]) U03(q) U03(q,γ1) H05(q) H05(q,γ1) EGRET blazars

Redshift z log(Lγ [erg/s]) dN/log(Lγ) dN/log(z)

Redshift Distribution Luminosity Distribution

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10-4 10-3 10-2 10-1 10-2 10-1 100 101 102 103 104 105 106

E2 dN/dE (MeV2 cm-2 s-1 MeV-1 sr-1) Photon Energy (MeV)

EGRET (S98) EGRET (S04a) EGRET (S98+S08) Blazar: U03 (q, γ1) Non-blazar (Γ=3.5): ITU08 Non-blazar (Γ=3.8): ITU08 Blazar + Non-blazar (Γ=3.5) Blazar + Non-blazar (Γ=3.8) HEAO-1 Swift/BAT SMM COMPTEL

X-ray

non-blazar AGNs (YI+08)

YI & TT 09 arXiv:0810.3580

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Cosmic X-ray and Gamma-ray Background before the Fermi era

Above GeV, our model does not reproduce

bservational data.

Blazars ( YI & TT 09)

GeV MeV

Energy (MeV) E2 dN/dE (MeV/cm2/s/sr)

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X-ray

non-blazar AGNs (YI+08) YI & TT 09 arXiv:0810.3580

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Cosmic X-ray and Gamma-ray Background in the Fermi era

10-4 10-3 10-2 10-1 10-2 10-1 100 101 102 103 104 105 106

E2 dN/dE (MeV2 cm-2 s-1 MeV-1 sr-1) Photon Energy (MeV)

Blazar: U03 (q, 1) Non-blazar (=3.5): ITU08 Non-blazar (=3.8): ITU08 Blazar + Non-blazar (=3.5) Blazar + Non-blazar (=3.8) EGRET (S98) EGRET (S04a) EGRET (S98+S08) Fermi

Our prediction matched very well with the Fermi data. Blazars ( YI&TT09)

MeV Fermi Data from TeV conf. on July

Energy (MeV) E2 dN/dE (MeV/cm2/s/sr)

GeV

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Non-blazar AGNs vs. Blazars

Ackermann+’09 at TeV. conf.

<~10 MeV:

smooth connection to

CXB

likely to be non-blazar

AGNs >~10 MeV:

distinct SED from CXB
likely to be blazars
MeV-blazar contribution at

<~10 MeV? (Ajello+09)

fine-tuning required for

SED

distinct blazar population

required between MeV and GeV.

Blazars

Non-blazar AGNs

Energy (MeV) E2 dN/dE (MeV/cm2/s/sr)

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N (>Flux) [(4 π sr)-1] Flux (>100MeV) [photons cm

2 s
1]

EGRET Fermi

Blazar: U03(q,γ1) Non-blazar (Γ=3.5) Non-blazar (Γ=3.8) Blazar + Non-blazar (Γ=3.5) Blazar + Non-blazar (Γ=3.8)

Expected Number of Fermi AGNs

N(>Flux) [(4πsr)-1] Flux(>100MeV) [photons cm-2 s-1] EGRET

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Blazar Fermi Non-blazar AGN

One-year survey
~800 blazars
1~10 non-blazar AGNs
Five-year survey
~1200 blazars
4~50 non-blazar AGNs
Nonthermal gamma-ray

flux from NGC 4151, the brightest Seyfert AGN

Flux(>100 MeV): ~1e-8 γ/cm/s
Photon Index: ~3.5

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10-11 10-10 10-9 10-8 10-7 10-6 10-5 10-15 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 10-6

Fγ dN/d(log10 Fγ) [photons cm-2 s-1 sr-1] Flux (>100MeV) [photons cm-2 s-1]

EGRET Fermi

Blazar: U03 (q,γ1) Non-blazar (Γ=3.5) Non-blazar (Γ=3.8) Blazar + Non-blazar (Γ=3.5) Blazar + Non-blazar (Γ=3.8)

Will Fermi resolve the cosmic gamma-ray background?

FdN/d(log10 F) [photons cm-2 s-1 sr-1] Flux(>100MeV) [photons cm-2 s-1]

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EGRET Fermi

Blazar Non-blazar AGN

Five year survey will

resolve

~99% of the

background flux from blazars (>100 MeV).

~0.01% of the

background flux from non-blazar AGNs (>100 MeV).

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~1 blazar @ z~7 with ~5-year Fermi survey (YI+in prep.). N(>z) z~7 ~5-years survey

0.1 1 10 100 1000 2 4 6 8 10 12 14 z

Flim(>100MeV)=1×10-9 photons/cm2/s

U03(q) U03(q,1) U03(q,1): p2=3.5

Redshift z

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YI&TT09 YI&TT09 +SDSS

Fermi blazar @ z~7

Predictions for z~7

blazar detectability

based on IT09
improved at

high-z based on SDSS quasar LF upto z~6.

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0.1 1 10 100 z=0.1

Optical Depth

z=0.3 z=1.0 z=3.0 0.1 1 10 100 1 10 100 z=5.0 Mitaka model Kneiske+04 S.Inoue+09 1 10 100 z=6.0

Energy (GeV)

1 10 100 z=7.0

z=0.1 z=0.3 z=1.0 z=3.0 z=5.0 z=6.0 z=7.0

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Probing high-z universe through GeV gamma-ray attenuation

γ(>GeV)+γUV→e++e-.

GeV flux attenuated by high-z UV background (Oh ’01,

Gilmore+09, S.Inoue+09).

information of early

star/galaxy formation may be obtained.

Red model: consistent with

z<5 data (e.g. galaxy LF)

Blue model: consistent

with z>5 data (e.g. reionization data)

Optical Depth 1 1

(YI+in prep.)

Kneiske+04 Semi-analytical model S.Inoue+09

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Summary 1

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New blazar GLF (Y. Inoue & Totani ’09, arXiv:0810.3580)
Blazar SED sequence incorporated
Non-trivial prediction for the cosmic gamma-ray

background

Our prediction matched very well with the Fermi data.
AGNs are the primary sources as the origin of cosmic X-

ray/Gamma-ray background.

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Summary 2

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Fermi will find
~800 blazars and 1~10 non-blazar AGNs in 1-year survey,
~1200 blazars and 4~50 non-blazar AGNs in 5-year survey.
Fermi will resolve
~99% of the gamma-ray background from blazars (>100

MeV),

~0.01 % of the gamma-ray background from non-blazar

AGNs (>100 MeV).

~1 blazar @ z~7 may be found by Fermi.
A new key to understanding the high-z cosmic evolution.