X-ray emission from very high energy gamma-ray sources [Horns]

Bologna May '07SIMBOL X Workshop

X-ray emission from GALACTIC very high energy (E>100 GeV)

gamma-ray sources

Dieter HornsUniversity of Tübingen

● X-Ray/VHE connection ● Categories of X-ray counterparts of VHE

sources● Examples: What we will learn from SIMBOL

X observations


VHE/X-ray connection(keV-TeV)

Sturner et al. (1997)

SIM-X

SIM-X

SIM-X

SIM-X

VH

E

SIM-X

SIM-X


X-ray counterparts of VHE sources

● Current catalogue of VHE sources >40 sources (more to come).

● Suggested categories of X-ray counterparts

I. Fx/FVHE>1, RX/RVHE ~ 1(shell type SNR, PWNe)

II.Fx/FVHE<1, RX/RVHE<1 (PWNe & candidates)

III.Fx/FVHE>1, point-like, variable (e.g. XRBs, Blazars)

IV.Fx/FVHE<1, RX/RVHE~1 (unknown)


Cat I: Gamma-ray & X-ray images from shell type SNRs

RX J0852.0-4622RX J0852.0-4622

HESS coll. (2006) HESS coll. (2006)

RX J1713.7-3946RX J1713.7-3946

Both sources show a cut-off at Gamma-Ray energies of ~10-20 TeV:

Maximum energy of the parent proton population ~100-200 TeV


Cat I: MSH 15-52(PWN)White Contours HESSColour: ISGRI (not pulsed)

Forot et al. 2006

Khelifi et al. 2005

INTEGRAL: cut-off at 160 keV?


Cat I or II? HESS J1813-178PWN/SNR System? (X-ray PWN -candidate, Radio SN shell),VHE source much larger than X-ray PWN candidateNo X-ray emission from Radio shell F

x>F

VHE

RX<F

VHE

Funk et al. (2007b)


Cat I/II: Vela X, prototype “Offset” Nebula

DH et al. (2006): ASCA 2-10 keV

FOVPosition dependent cut-off?Primary particle cooling?Bright but very extended source


Very faint X-ray emission (Fx<F

VHE)

X-ray emission region 6 times more compact than VHE region (different cooling times)

Cat II: PSR J1826-1334 (G18.0-0.7)

H.E.S.S. 0.25-30 TeV

XMM 2-10 keV

20 pc

Aharonian et al. (2005&2006)Gaensler et al. (2003)


Cat II: HESS J1640-465

PWN/SNR System (X-ray PWN -candidate, Radio SN shell),VHE source much larger than X-ray PWN candidate

Funk et al. (2007a)F

x<F

VHE


CAT II: HESS J1804-216Cui&Konopelko (2006)Bamba et al. (2006)Landi et al. (2006)Kargaltsev et al. (2007)

Kargaltsev et al (2007)

Γ=1.2+/-0.4F

2-10~10-13 ergs/(cm2 s)

(white contours ROSAT, black contours 20 cm, colour VHE excess map)


Cat II “Rabbit” & “Kookaburra”Aharonian et al. 2006

INTEGRAL detection

Hoffmann, DH et al. (2006)

Two PWN candidatesVery similar in VHE gamma-rays

RX<R

VHE

FX<F

VHEINTEGRAL 20-40 keV

Bologna May '07SIMBOL X Workshop Cat II or III?: HESS J1634-472=G337.2+0.1 or

IGR J16358-4726Combi et al. 2006Hard X-ray spectrum G=1.8+/-0.5,f

X~10-12 ergs cm-2 s-1


Similar:HESS J1632-478G336.4+0.2

DH et al. (2007)XMM-Newton 2-10 keV

Hard X-ray spectrum, maybe IC X-rays?


CAT III:PSR B1259-630

P=3.4 a

Neronov & Chernyakova (2006)

CAT III: LS I +61 303

P=26.5d

Chernyakova et al. (2006)


CAT III: LS 5039 (“runaway Microquasar”)

Detection of Orbital modulation (20-210 keV) with INTEGRAL in phase with HESS, Hoffmann et al. (in prep.)

preliminary.

SED (adapt. from Paredes et al. 2005)


CAT IV: TeV J2032+4130● 1st unidentified VHE gamma-ray source● Extended, but unresolved (~6' radius)● Possible source candidates:

– Cyg OB2 stellar cluster (slightly offset) – Termination shocks of possible radio lobes of Cyg X-3– Hidden (background?) pulsar wind nebula system

● Multiwavelength search for counterparts:– Radio (VLA) Paredes et al. (2006)– Chandra (5+50 ksec), Butt et al. 2002,2006,2007,

Mukherjee (2005,2006)– XMM-Newton (50 ksec), DH et al. 2007

Bologna May '07SIMBOL X WorkshopMILAGRO Skymap (at ~18 TeV)

●HEGRA Skymap TeV J2032+4130 (~1 TeV)Also in FoV:●3EG J2033+4118●Cyg X-3●Cyg OB2●GeV J2035+4214●GeV J2025+4124

Extension (circle)and pos. uncertainty (magenta cross) of MGRO J2031+41


Detection of extended X-ray emission from TeV J2032+4130

Mosaic of XMM-Newton M1,M2, 1-5 keV (max. collection area)Blank field background subtracted, vignetting corrected

Sources subtractedsmoothed with 45”

Sources subtractedsmoothed with 90”Excess contours from TeVJ2032+4130

Core of Cyg OB2

DH et al. 2007


Spectral energy distribution and interpretation:

TeV J2032+4130 a Pevatron?


Simulation of SIMBOL X response for CAT IV

● Assuming 50 ksec exposure

● Power-law model (NH=3.5x1021 cm-2, Γ=1.5, f2-

10=7x10-13 ergs (cm2 s)-1

● Stellar component APEC with kT=1 keV, f2-

10=2x10-12 ergs (cm2 s)-1

● Assuming a 10' diameter homogeneous emission (conservative)

● Including diffuse XRB, GRUBER_PARMAR bkg model


Stellar emission (MPD)

J2032+4130 (MPD) J2032+4130

(CZT)

Stellar emission (CZT)

Stellar emission vs. non-thermal emission

● Point source subtraction is difficult (18” HEwidth)

● E>4 keV: Non-thermal component dominates


Challenge: Background systematics in CZT

CZT S/B ~ 5%

MPD Background(10' diameter)

CZT Background(10' diameter)


Summary

● Tandem of VHE & SIMBOL X: Exploring the non-thermal Universe– Cat I: Probe IC/Bremsstrahlung branch– Cat II: Probe IC Branch, spatially resolved

radiative cooling– Cat III: Probe/Sample fast cooling electrons – Cat IV: Secondary electrons vs. primary

electrons?


Ende!Vielen Dank für die Aufmerksamkeit

X-ray emission from very high energy gamma-ray sources [Horns]

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