Fermi_CTAmeeting_2011-09.ppt

Fermi GeVガンマ線衛星
GeVガンマ線衛星による3による3年間の成果
Sep. 30, 2011@ICRR(Multi-Messenger Astrophysicsand CTA)
T. Mizuno(広島大学 理学部理学部->>宇宙科学センター)
On behalf of the Fermi-LATcollaboration
T. Mizuno et al.

1 /27

Fermi_CTAmeeting_2011-09.ppt

Fermi GammaGamma-ray Space Telescope• Fermi = LAT + GBM• LAT = “GeV”“G V” G
Gamma-ray SpaceSTTelescopel(20 MeV ~ >300 GeV )2008.06 launch2008.08 Sci. Operation

3c454.3

Cape Canaveral,Florida

T. Mizuno et al.

1873 sources
Abdo+, ApJS submitted
arXiv:1108.1435

2 /27

Fermi--LAT Performance
Fermi

Fermi_CTAmeeting_2011-09.ppt• New Dataset and Response (Pass7)– Improved Aeff in low Energy– In-orbit calibration of PSF
http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm
pp gg
p
Effective Area

PSF

comparable to PSF of IACT(>10 GeV)
1 year Integral Sensitivity (>10GeV): ~0.05 Crab (Atwood+09)
T. Mizuno et al.

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Fermi--LAT Publications
Fermi

Fermi_CTAmeeting_2011-09.ppt• Publications by Fermi-LAT members(C t I(CatI+II+III,II III as off mid-Sep.
id S2011)
2008

20092010

2011~200 papers alreadypublished
6 7 papers/month
6-7/thT. Mizuno et al.

http://www-glast.stanford.edu/cgi-bin/pubpub

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Fermi_CTAmeeting_2011-09.ppt

2FGL: Second Source Catalog• 1873 sources (~4σ significance)– 127 firm identifications and 1170 reliable associations– 576 unassociated with known γ-ray source classplease pay attention to flags (e.g., 126 possibly confusedwith diffuse emission)

Abdo+, ApJS submitted
arXiv:1108.1435

T. Mizuno et al.

Preliminary

5 /27

Kifune Plot

Fermi_CTAmeeting_2011-09.ppt• # of sources exponentially increases in GeV• Future: 1000 sources in TeV by CTA!?

(200 publications)

HEE γ-rays

VHE γ-rays

T. Mizuno et al.

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Source Classes in 2FGL

Fermi_CTAmeeting_2011-09.ppt• # of known blazars and pulsars continue to grow• 12 spatially extended sources (LMC/SMC,(LMC/SMC SNR andPWN)
Pulsars6%
Non-blazar
AGN 1%

Unknown
31%

SNR
4%

GC, HMB,normal gal. etc.
1%

Blazars
Bl57%>=50% are blazars
T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

Source Classes in FermiFermi-LAT Publications• Publications by Fermi-LAT members(C t I(CatI+II+III,
II III as off mid-Sep.
id S2011)

Well balanced# of papers:
AGN~Galactic
Diffuse~GRB~DMNP

T. Mizuno et al.

http://www-glast.stanford.edu/cgi-bin/pubpub

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Fermi_CTAmeeting_2011-09.ppt

Source Classes in FermiFermi-LAT Publications• Publications by Fermi-LAT members(C t I(CatI+II+III,
II III as off mid-Sep.
id S2011)Well balanced
covered bythis talk# of papers:
AGN~Galactic
Diffuse~GRB~DMNP

T. Mizuno et al.

http://www-glast.stanford.edu/cgi-bin/pubpub

9 /27

Fermi_CTAmeeting_2011-09.ppt

Diffuse Emission Seen by LAT• Local diffuse emission is compatible withdirectly measured CRs• “dark gas” is confirmed byFFermi-LAT
i LAT datad t• More CRs than expected inouter Galaxy
Abdo+10, ApJ 710, 133
Ackermann+11, ApJ 726, 81• Freshly-accelerated CRs in
Cygnus region
Abdo+09, PRL 103, 251101(CA: Johannesson, Porter, Strong)
T. Mizuno et al.

10 /27

Fermi_CTAmeeting_2011-09.ppt

The Cygnus Region (MILAGRO)• Very rich region of massive-star formation at 1.4 kpc• Two sources + diffuse emission at TeV (MILAGRO)– correlation with matter density– diffuse flux exceeds the prediction by local CR
MGRO J2031+41

EGRET

MILAGRO

MGRO J2019+37

T. Mizuno et al.

Abdo+07, ApJL 658, 33
Abdo+08, ApJ 688, 1078

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Fermi_CTAmeeting_2011-09.ppt

The Cygnus Region (VERITAS)• Very rich region of massive-star formation at 1.4 kpc• Cyg OB1 association seen by VERITAS– CTB87 resolved– plus complex region, likely powered by multiple sources(Good PSF is essential)

MGRO J2031+41

VERITAS

MGRO J2019+37

T. Mizuno et al.

Abdo+07, ApJL 658, 33
Abdo+08, ApJ 688, 1078

Aliu+11(ICRC2011)12 /27

Fermi_CTAmeeting_2011-09.ppt

The Cygnus Region (Fermi)• Very rich region of massive-star formation at 1.4 kpc• Detailed study by Fermi-LAT– GeV diffuse (on average) consistent with local CR spectrum,
despite the conspicuous star formation activity
Total > 10 GeV

MGRO J2031+41(Gamma-ray Image)

MGRO J2019+37

Preliminaryeay
Glonet (deg)85
T. Mizuno
al.

80

Ackermann+11 submitted

75 (CA: Tibaldo, Grenier)13 /27

Fermi_CTAmeeting_2011-09.ppt

The Cygnus Region (Fermi)• Very rich region of massive-star formation at 1.4 kpc• Known sources and diffuse gammas subtracted– Extended hard (>10 GeV) excess revealed in OB2 association– Spatial relation with infrared suggests the interstellar origin
point sources, γ Cygni
and diffuse emission
removedMGRO J2031+41(Gamma-ray Image)

MGRO J2019+37

PreliminaryeayGlonet (deg)85
T. Mizunoal.

80

Ackermann+11 submitted

75 (CA: Tibaldo, Grenier)14 /27

Fermi_CTAmeeting_2011-09.ppt

Energy Spectrum• CRs with local spectrum are too weak or too soft
• Hard,Hard freshly accelerated CRs are required– E-2.4 (hadron) or E-2.7 (lepton)– their origin and propagation to be studied by GeV/TeV obs.
γ-rays (10-100 GeV)γ Cygni

LAT

Preliminary(G(Gamma-raySSpectrum)t)

MILAGRO(Gamma-ray Image)IC fromLocal CR

HII x
Local CR

Cyg OB2

Preliminary
T. Mizuno et al.

15 /27

Starburst Galaxies

Fermi_CTAmeeting_2011-09.ppt• High gas density and star-formation rate
• Detected by H.E.S.S.
H E S S (NGC 253) and VERITAS (M82)
in TeVM82 (VERITAS)

T. Mizuno et al.

Acciari+09, Nature 462, 770

NGC253 (H.E.S.S.)(H E S S )Acero+09, Science 326, 1080

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Starburst Galaxies

Fermi_CTAmeeting_2011-09.ppt• High gas density and star-formation rate
• Detected by H.E.S.S.
H E S S (NGC 253) and VERITAS (M82)
in TeV• Hard spectrum by Fermi+IACT

Γ=2.2

Γ=1.95(Fermibest fit PL)

Abdo+10, ApJL709, 152
T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

SB + Local Group Galaxies• LMC, SMC and M31 detected by Fermi-LAT• Correlation between SFR and Lγ over wide range ingalaxy properties.
• Lγ less correlated with gas mass.

Lγ ~ SFRα
L
α=1.4+/-0.3

Abdo+10, A&A 523, L2(CA: Bechtol, Knodlseder, Martin)
T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

Recent Update••

A sample of 69 is examined: confirm the relation between
star-formation rate and Lγ
SFR-Lγ relation and hard spectrum implies hadron calorimetry– NB MW is escape limited– need theoretical work and future obs.
N1068
N4945

M31
M3

M82
N253
MW
LMC
SMC

T. Mizuno et al.

Preliminary

Ackermann+11 submitted(CA: Bechtol, Cillis, Funk, Torres)

19 /27

Fermi_CTAmeeting_2011-09.ppt

Fermi GRBs as of 20112011-0808-01• In 3 years~0 6/day~0.6/day– 682 GBM GRBs (345 in LAT FOV)– 32 LAT GRBs (19 with >10 photons >100 MeV) ~0.6/month
fewer than
expected(Band+09)

Preliminary
T. Mizuno et al.

20 /27

Summary of LAT GRBs•

aaa

Fermi_CTAmeeting_2011-09.ppt• 32 GRBs by LAT,
19 with >10 γsaboveb
100 MeV
M V• Most of GRBs show
delayed HE onset
andnd HE afterglow
ftl

~3030

• Some bursts havean extra spectral
component

Preliminary
eay

T. Mizuno et al.

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Common feature of GRBs••

Delayed HE onset andtemporary extended emission
are commonly seen
Some GRBs show extra spectral
component (090510, 090902B,090926A)

Fermi_CTAmeeting_2011-09.ppt

GRB 080916C (long)
Abdo et al. 2009, Science 323, 1688

LAT(>100MeV)
GBM

Delay in HE onset: 4-5 s

T. Mizuno et al.

• LAT Aeff ~ 0.8m2 (<10-4 of CTA Aeff)• Large Aeff is of great benefit to study extra component,extended emission and quantum Gravity.
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Prospect of GRB with CTA

Fermi_CTAmeeting_2011-09.ppt• ~1 GRB/yr• Energy threshold is important

Bouvier+11(ICRC2011)

lower Eth and larger Aeff
T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

Caution on Detection Rate Estimate• 10% of GBM GRBs in LAT FOV are detected by LAT– lower than expected (single PL), particularly in GeV– GBM+LAT joint fit leads to softer β
30 GBM-bright samples
undetected
dd bby LAT

Preliminary
GBM+LAT
GBM
LAT

GBM

19/3yr(>10 γs >100MeV)
4 superbursts

Connaughton+11 (ICRC2011)
T. Mizuno et al.

Band+09, ApJ 701, 1673

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SNRs seen by Fermi
Fermi--LAT••Fermi_CTAmeeting_2011-09.ppt

ten 2FGL sources are now identified as, or associated with SNR(# of possible association ~60)
Hadronic scenario is usually favored

T. Mizuno et al.

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RXJ1713.7--3946
RXJ1713.7••

GeV γ-ray excess above diffuse
emission correlates with TeV γsBroadband spectrum favors leptonic
origin as the emission mechanism

Fermi_CTAmeeting_2011-09.ppt

hadronicleptonic
LAT

T. Mizuno et al.

Abdo+11, ApJ 734:28(CA: Ackermann, Funk, Uchiyama)

H.E.S.S.

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Summary

Fermi_CTAmeeting_2011-09.ppt• フェルミは順調に観測. 高い生産性.
• 最近の成果をいくつか紹介– 加速されたばかりの宇宙線 in Cygnus Region– 星生成銀河のSFR-Lγ星生成銀河のSFR L 関係
– SNRのGeV/TeVスペクトルと放射機構• いずれもTeVのデータが重要ず
デ• GRBもCTAへの期待大. 見積もりには注意.

Thank you for your Attention
T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

Backup Slides

T. Mizuno et al.

28 /27Morphology•

Fermi_CTAmeeting_2011-09.ppt

γ-ray excess fills the cavities carved by stellar
winds and ionization fronts– likely interstellar origin

γ-rays (10-100 GeV)

Infrared (8 um)(Gamma-ray Image)(Infrared Image)Preliminary
T. Mizuno et al.

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The Cygnus Region (Fermi)

Fermi_CTAmeeting_2011-09.ppt• Extended excess (>10 GeV) is revealed
Total > 10 GeV

removepoint sources
ISM emission(Gamma-ray Image)

Extended γ Cygni
removed(Gamma-ray Image)(Gamma-ray Image)Preliminary

T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

M31 Morphology and Spectrum

BG-subtracted
BG
subtracted LAT image
Contour: IRIS 100 um
M31 Spectrum vs.
normalized
li d modeld l off MW

possible contribution
from 1ES 0037+405

T. Mizuno et al.

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FIR--radio Relation
FIR

Fermi_CTAmeeting_2011-09.ppt• FIR vs. Radiocorrelation

Condon92

T. Mizuno et al.

SFR as primary factor
controlling radio andFIR luminosities

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Fermi_CTAmeeting_2011-09.ppt

CR--induced Luminosity of MWCR••

MW is nearly a CR electron
calorimeter, if IC is taken
into accountConversion eff.
~1% for protons

protonalphaπ0-decay

Synchrotron

electron

InverseComptonBrems

T. Mizuno et al.

Strong+1033 /27

Fermi_CTAmeeting_2011-09.ppt

The Fermi Observatory (2008(2008-)

LAT : 対生成型ガンマ線望遠鏡トリガ、位置決定、スペクトル取得
ガ 位置決定ペク
取得
20 MeV – 300 GeV

GBM :広視野バ:広視野バーストモニタ
ストモ タ
12 NaI
トリガ、位置決定、スペクトル8 keV – 1 MeV
2 BGO
スペクトル
150 keV – 40 MeV~2.4 sr~8 sr

T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

Simulated CTA Performance• Objective

Bouvier+11(ICRC2011)

T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

LAT view of W44

Abdo+10, Science 327, 1103
CA: Tanaka, Uchiyama, Tajima

x印はパルサーの位置
緑のコントアは衝撃波に励起された分子雲• 高密度の分子雲からγ線が放射T. Mizuno et al.

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Fermi_CTAmeeting_2011-09.ppt

LAT Spectrum & modeling

100 MeV

10 GeV

1 TeV• スペクトルは陽子起源が良く合う

T. Mizuno et al.

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