Current status and future plans of TeV gamma-ray observations

Current status and future plans of TeV gamma-ray observations

Hidetoshi Kubo (Kyoto University)

Outline

• TeV gamma-ray telescopes

• Observations Results– Galactic

• HESS plane survey• G.C., Diffuse emission• PWN, SNR, etc.

– Extragalactic sources• AGN, Starburst galaxy

• Future plans

• Summary

TeV gamma-ray observation• Cherenkov shower pool

• Better angular resolution=0.20.07/

• Better energy resolution E/E=30%15%

• E>100GeV at present

• Higher E threshold at larger zenith angle

• 1%Crab for 25hrs(HESS)

• FOV ＜ 5, ＜ 3 (FWHM)

Altitude 10 ～ 20km

~300m

+Water Cherenkov telescope, Air Shower Array

CANGAROO-III

T2 T4 T3 T1

T2

114 80cm FRP mirrors

427ch (4 FOV)

STACEE

MILAGRO

TIBETARGO-YBJ

PACT

GRAPES

TACTIC

VERITAS

MAGIC

HESS CANGAROO

TIBETMILAGRO

STACEE

TACTIC

TeV gamma-ray telescopes

R.Ong (2005)

HESS Galactic Plane Survey in 2004

Survey Region

PSR B1259HESS J1303

MSH 15-52RXJ 1713

GC

RXJ 0852

Vela X

• 30°in longitude, 3° in latitude• 230hrs(95 hrs scanning + follow-up observations)• E > 200GeV• Flux > 2%Crab Aharonian et al. (2005)

Detections with CANGAROOBefore the HESS survey Gal. Centre

330°

30° 0°

RX J1713.7-3946

359° 330°

HESS Survey: New sources

HESS J1804-216 Gal. Centre HESS J1837-069

330°

G0.9+0.1 HESS J1813-178 HESS J1825-137

HESS J1834-087

30° 0°

RX J1713.7-3946 HESS J1640-485HESS J1616-508

HESS J1614-518

359° 330°

Sources > 6 sigma (10 new, 12 total)

Aharonian et al. (2005)

LS 5039

HESS Survey: New Sources

HESS J1702-420HESS J1713-381 HESS 1632-478

330°

RX J1713.7-3946 HESS J1640-465HESS J1616-508

HESS J1614-518

359°

HESS J1708-410 HESS J1634-472HESS J1745-303

LS 5039

HESS J1804-216 Gal. Centre HESS J1837-069

G0.9+0.1 HESS J1813-178 HESS J1825-137

HESS J1834-087

30° 0°

Sources > 6 sigma (10 new, 12 total)Sources > 4 sigma (6 new)


HESS GP Source Associations

PWN

PWN

PWN/UID

XRB/SNRSNR/UID

SNRSNR

XRB

SNR

SNRUID

UIDSNR/BH

SNR/PWN

J1826-148 LS5039 XRB

○

○○○

○○◎

◎

◎

◎

◎◎◎◎◎◎

◎

◎ >6 ○ >4


The VHE Sky - 1995

Mrk421

Mrk501

Crab

R.A.OngAug 2005

Pulsar Nebula

SNR

AGN

Other, UNID

The VHE Sky - 2003

Mrk421 H1426

Mrk501

1ES1959

1ES 2344

PKS 2155

Cas A

RXJ 1713

CrabTeV 2032

M87

GC

R.A.OngAug 2005

Pulsar Nebula

SNR

AGN

Other, UNID

12 sources

The VHE Sky - 2005

Mrk421 H1426

Mrk501

1ES1959

1ES 2344

PKS 2155

Cas A

RXJ 1713

CrabTeV 2032

M87

PKS 2005

PSR B1259

RXJ 0852

MSH 15-52

SNR G0.9

HessJ1303

GC

R.A.OngAug 2005

Pulsar Nebula

SNR

AGN

Other, UNID

H2356

1ES 1218

1ES 1101

LS 5039Vela X

+ 8-15 add. sourcesin galactic plane.

CygnusDiffuse

33 sources

TeV gamma-ray sources

Source Type* 2003 2005

Pulsar Wind Nebula (e.g. Crab, MSH 15-52 …) 1 6

Supernova Remnants (e.g. Cas-A, RXJ 1713 …) 2 6

Binary Pulsar (B1259-63) 0 1

Microquasar (LS 5039) 0 1

Diffuse (Cygnus region) 0 1

AGN (e.g. Mkn 421, PKS 2155 …)

Starburst galaxy (NGC253)

7

0

11

1

Unidentified 2 6

TOTAL 12 33

Based on R.A.Ong ICRC2005

SGR A

Galactic Center

CANGAROO(E>300GeV)

EGRET(E>500MeV) r<0.2

Tsuchiya et al.(2004)

Mayer-Hasselwander et al.(1998)

VLA@5GHz

HESS (E>125GeV)

Contour: Radio

Consistent with SGR A* to 6’’±10”stat±20”sysPoint like core + slightly extended tail

Aharonian et al.(2004),Rolland et al.(2005)

Yusef-Zadeh & Morris(1987)

Galactic Center– Unbroken power-law.– Hard spectrum = 2.2

(HESS).– No evidence for

variability

π0→2γ

CANGAROO-III(stereo)under analysis

HESS

Galactic Center Region

CS

gamma rays(subtracted)

HESS

2.29±0.07±0.20

CS

gamma rays

Harder than Diffuse model

Hinton et al.(2005)

CS

Galactic Diffuse emission

E-2.51±0.05

EGRET longitude latitude R1 　 40-100°±5° R2 　 140-200°±5°

Milagro 　 (2000 ～ 2002)

Sinnis et al.(2005)

Milagro4.5

-1.3

x1/100

CANGAROO-II ULl=+13,b=0, l=-19.5,b=-3,0,+3Ohishi et al.(2005)

Cygnus region

+20

+40

+60

+100

+80

Milagro (2000 ～ 2005)

Excess >5°(1.55Crab for E>2TeV) from Cygnus region

PSF

Contour: 1420MHz

HEGRA unIDTeV 2032+4130

Smith et al.(2005)

HESS (440GeV<E<10TeV)Consistent with point source(PSF 　 σ ～ 0.14°)Error 5”(stat)±20”(sys)

Crab ー standard candle in VHE ー PWN(1/5)

Gravity of the X-ray emissionWeisskopf et al.(2000)

Masterson et al.(2005)

UL for pulse

Continuum

Aharonian et al.(2004)

=2.6

E>100GeV

SNR MSH-52(PSR B1509-58) PWN(2/5)


Contours: X-ray(ROSAT)

HESS

PSF

Photon index2.27 ± 0.03 ± 0.20

Gray:RadioContours:ROSAT

Chandra

B ～ 17GDust=2.3eV/cm3

Major axis 6.4’±0.7’Minor 2.3’±0.5’

Vela pulsar

ROSATcontours

Khelifi et al.(2005)

Preliminary

HESSNo emission from Vela pulsar position, butExtented hard spectrum ≈1.9 or ≈1.5 cutoffextends to50 TeV

Vela PWN(3/5)

HESS

CANGAROO-IIalso detected

Enomoto et al.(2005)

HESS J1825-137(4/5)

TeV

17%Crab(E>200GeV)


Offset by 11’ south to PSR B1823-13(101ms) in PWN G18.0-0.7

SNRG0.9+0.1

Radio

Radio (90 cm)

HESS・ Consistent with point source at core, not SN shell・ 2% Crab flux(E>200GeV)

PWN in SNR G0.9+0.1(5/5)

HESS


G.C.

6G

=2.40±0.11±0.20

Chandra Gaensler et al.(2001)Hard spectrum Point Src(No pulsed emission)Newton Porquet al.(2003)Softening of spectrum with increasing distance from the center

GLAST 1yr

Berge et al.(2005)

Shell structureclearly resolved.Morphology does not change with energy.

RXJ 1713.7-3946 SNR(1/4)From the NW rim, non-thermal X-ray emission detected with ASCA (Koyama et al.1997) TeV - detectionE>1TeV CANGAROO-I in 1998E>400GeV CANGAROO-II in 2000+1Enomoto et al.(2002)

HESS

Spectral index:little variation across SNR

RXJ 0852.0-4622 “Vela Jr.” SNR(2/4)

Katagiri et al.(2005)

CANGAROO-II

4850MHz

ASCA

HESS Aharonian et al.(2005)

Contour: ROSAT

TeV flux ～ Crab

SNR RXJ 0852.0-4622 “Vela Junior”

Bremsstrahlung

Synchrotron

IC

0 decay

Katagiri et al.(2005)

0 decay? Brems.? IC?

GLAST 1yr

Cas A SNR(3/4)

Chandra image

HEGRACenter of TeV excess

Aharonian et al.(2001)IC+Bremsstrahlung?

0 decay?

GLAST 1yr

Earlier detection by CANGAROO-I from NE rim.& HEGRA CT1.

CANGAROO-III

2 U.L.

HESS & CANGAROO-III 　

SN1006 not detected at previous levels.

SN1006 SNR(4/4)Upper limit

ASCA

Tanimori et al.(2005)

PSR B1259-63/SS2883

331 R*


PSR B1259-63 (P=48ms)

around Be star SS2883 in

a highly eccentric 3.4yr orbit

1.4GHz

HESSperia

stro

n


PSR B1259-63/SS2883

electron origin? Hadronic origin?

Kawachi et al.(2004)

GLAST?

Paredes et al. (2002)

RA (mas)

compact 4 (?) M object in eccentric 4 day orbit around 20-30 M starclosest approach ~1012 cm or ~2 stellar radii


Microquasar LS 5039first detection of TeV emission from a microquasar

European VLBI@5GHz

Jets

HESS

2.12 ± 0.15

Flux (E>250GeV)(5.1±0.8stat±1.3sys)x10-12

ph cm-2s-1

2003 XMM

1998 RXTE

L ～ 1033 erg/s at 3kpc

Microquasar LS 5039


Extented with radius 6.2’(±1.2’stat±0.9’sys)

HEGRA observations 1999 ～ 2002

Hard spectrum Γ=1.9±0.1’stat±0.3’sys

Flux (6.2±1.5stat±1.3sys)x10-13

ph cm-2s-1TeV-1@1TeV

unID TEV J2032+4130

3EGJ2033+4118

Higher angular resolution of GLAST canresolve it

Source Redshift Type First Detection Confimation

M87 0.004 FR I HEGRA HESS

Mkn 421 0.031 BL Lac Whipple Many

Mkn 501 0.034 BL Lac Whipple Many

1ES2344+514 0.044 BL Lac Whipple HEGRA

1ES1959+650 0.047 BL Lac Tel. Array Many

PKS 2005-489 0.071 BL Lac HESS

PKS 2155-304 0.116 BL Lac Mark VI HESS

H1426+428 0.129 BL Lac Whipple Many

H2356-309 0.165 BL Lac HESS

1ES1218+304 0.182 BL Lac MAGIC

1ES 1101-232 0.186 BL Lac HESS

TeV –ray detected AGNs

R.Ong (2005)

5014212155

23441426

Costamante & Ghisellini(2002)

2005

1101

2356

HB

LLB

L

Total :11 sources

Extragalactic Background Light


TeV

HESS limits Reference shape

TeV photon + EBL → 　 e+ + e-

More transparent than previously thought

If we assume (electron index>2)for intrinsic spectrum

GLAST

GLAST

Mrk 421 & Mrk 501

Light Curve: 2 min time bins.Mazin et al.(2005)

STACEE

Carson et al.(2005)

Mrk 501 Big Flare in Jul 2005

Rapid variation

Mirzoyan et al.(2005)

4CrabMAGIC

Wide range:300GeV – 30TeV

GLAST

Simulataneous obs. with GLAST is needed

Radio galaxy M87(16Mpc)

Beilicke et al.(2005)

Georganopoulos et al.(2005)

HESS(2003+2004)

5.8

HEGRA

Starburst galaxy NGC253

Multi-band spectrum Itoh et al. A&AL 2002

Crab(65%)

DSS2

CANGAROO

CANGAROO-II

E-1.5e-√E/(0.25±0.01)

• Nearby(2.5Mpc) spiral galaxy

• Radio Halo extending to ~9kpc

First TeV gamma-ray detection from anormal spiral galaxy other than our own

Detected with CANGAROO-II in 2000 and 2001 with 11 (E>0.5TeV)

GLAST 1yr

Future plans of TeV ray observations

Project Site Current Plan From E>

VERITAS USA 12m x 1 12m x 4 2006 　 50GeV

CANGAROO Australia 10m x 3 10m x 4 100GeV

HAGAR India(4.2km) 0.9m x 1 0.9m x 7 2006 60GeV

MACE India(4.2km) 21m x 2 15GeV MAGIC Canary is. 17m x 1 17m x 2 2007 20GeV

HESS Namibia 12m x 4 +28m x 1 2008 20GeV

Ashra Hawaii

HAWC 300mx300m pondLower Energy Threshold at higher altitude

Future plans of TeV ray observations

Cherenkov telescope network

・ Continuous monitoring of time variable objects such as blazars・ Simultaneous observations with GLAST

＋

HAGAR,Mace

Summary

• 33 sources detected in TeV ray region, including newcomers (Pulsar Binary, Microquasar, Starburst Galaxy, unID). Candidates for GLAST detection.

• Improved resolution of TeV(< 0.1/) + GLAST enable us to investigate detail morphology of SNRs, PWNs, etc.

• TeV + GLAST reveal electron or proton origin of ray emission in SNR etc., the intrinsic spectrum of blazars, and the EBL spectrum. 　

• Simultaneous monitoring with Cherenkov telescope network and GLAST for variable sources.

• New telescopes are under construction in order to lower the energy threshold to <100GeV, overlapped with GLAST region.

Documents

Current status and future plans of TeV gamma-ray observations