SIMBOL X Workshop Bologna May 07 Xray emission

SIMBOL X Workshop Bologna May '07 X-ray emission from GALACTIC very high energy (E>100 Ge. V) gamma-ray sources Dieter Horns University of Tübingen ● ● ● X-Ray/VHE connection Categories of X-ray counterparts of VHE sources Examples: What we will learn from SIMBOL X observations

SIMBOL X Workshop Bologna May '07 VHE/X-ray connection (ke. V-Te. V) SIM-X VHE SIM-X Sturner et al. (1997)

SIMBOL X Workshop Bologna May '07 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)

SIMBOL X Workshop Bologna May '07 Cat I: Gamma-ray & X-ray images from shell type SNRs HESS coll. (2006) RX J 0852. 0 -4622 RX J 1713. 7 -3946 Both sources show a cut-off at Gamma-Ray energies of ~10 -20 Te. V: Maximum energy of the parent proton population ~100 -200 Te. V

SIMBOL X Workshop Bologna May '07 Cat I: MSH 15 -52(PWN) White Contours HESS Colour: ISGRI (not pulsed) Khelifi et al. 2005 Forot et al. 2006 INTEGRAL: cut-off at 160 ke. V?

SIMBOL X Workshop Bologna May '07 Cat I or II? HESS J 1813 -178 PWN/SNR System? (X-ray PWN -candidate, Radio SN shell), VHE source much larger than X-ray PWN candidate No X-ray emission from Radio shell Fx>FVHE RX<FVHE Funk et al. (2007 b)

SIMBOL X Workshop Bologna May '07 Cat I/II: Vela X, prototype “Offset” Nebula DH et al. (2006): ASCA 2 -10 ke. V FOV Position dependent cut-off? Primary particle cooling? Bright but very extended source

SIMBOL X Workshop Bologna May '07 Cat II: PSR J 1826 -1334 (G 18. 0 -0. 7) Aharonian et al. (2005&2006) Gaensler et al. (2003) Very faint X-ray emission (Fx<FVHE) X-ray emission region 6 times more compact than VHE region (different cooling times)

SIMBOL X Workshop Bologna May '07 Cat II: HESS J 1640 -465 PWN/SNR System (X-ray PWN -candidate, Radio SN shell), VHE source much larger than X-ray PWN candidate Funk et al. (2007 a) Fx<FVHE

SIMBOL X Workshop Bologna May '07 CAT II: HESS J 1804 -216 Cui&Konopelko (2006) Bamba et al. (2006) Landi et al. (2006) Kargaltsev et al. (2007) Kargaltsev et al (2007) (white contours ROSAT, black contours 20 cm, colour VHE excess map) Γ=1. 2+/-0. 4 F 2 -10~10 -13 ergs/(cm 2 s)

SIMBOL X Workshop Bologna May '07 Cat II “Rabbit” & “Kookaburra” Aharonian et al. 2006 INTEGRAL detection Hoffmann, DH et al. (2006) Two PWN candidates Very similar in VHE gamma-rays INTEGRAL 20 -40 ke. V RX<RVHE FX<FVHE

Cat II or III? : HESS J 1634 -472=G 337. 2+0. 1 or IGR J 16358 -4726 SIMBOL X Workshop Combi et al. 2006 Hard X-ray spectrum G=1. 8+/-0. 5, f. X~10 -12 ergs cm-2 s-1 Bologna May '07

SIMBOL X Workshop Similar: HESS J 1632 -478 G 336. 4+0. 2 Bologna May '07 DH et al. (2007) XMM-Newton 2 -10 ke. V Hard X-ray spectrum, maybe IC X-rays?

SIMBOL X Workshop Chernyakova et al. (2006) Bologna May '07 CAT III: LS I +61 303 P=26. 5 d Neronov & Chernyakova (2006) CAT III: PSR B 1259 -630 P=3. 4 a

SIMBOL X Workshop Bologna May '07 CAT III: LS 5039 (“runaway Microquasar”) Detection of Orbital modulation (20 -210 ke. V) with INTEGRAL in phase with HESS, Hoffmann et al. (in prep. ) preliminary. SED (adapt. from Paredes et al. 2005)

SIMBOL X Workshop Bologna May '07 CAT IV: Te. V J 2032+4130 ● 1 st unidentified VHE gamma-ray source ● Extended, but unresolved (~6' radius) ● Possible source candidates: ● – Cyg OB 2 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

SIMBOL X Workshop Bologna May '07 MILAGRO Skymap (at ~18 Te. V) HEGRA Skymap Te. V J 2032+4130 (~1 Te. V) Also in Fo. V: ● 3 EG J 2033+4118 ●Cyg X-3 ●Cyg OB 2 ●Ge. V J 2035+4214 ●Ge. V J 2025+4124 ● Extension (circle) and pos. uncertainty (magenta cross) of MGRO J 2031+41

SIMBOL X Workshop Bologna May '07 Detection of extended X-ray emission from Te. V J 2032+4130 Mosaic of XMM-Newton M 1, M 2, 1 -5 ke. V (max. collection area) Blank field background subtracted, vignetting Sources subtracted corrected smoothed with 45” DH et al. 2007 Core of Cyg OB 2 Sources subtracted smoothed with 90” Excess contours from Te. VJ 2032+4130

SIMBOL X Workshop Bologna May '07 Spectral energy distribution and interpretation: Te. V J 2032+4130 a Pevatron?

SIMBOL X Workshop Bologna May '07 Simulation of SIMBOL X response for CAT IV ● ● ● Assuming 50 ksec exposure Power-law model (NH=3. 5 x 1021 cm-2, Γ=1. 5, f 2 -10=7 x 10 -13 ergs (cm 2 s)-1 Stellar component APEC with k. T=1 ke. V, f 2 -12 ergs (cm 2 s)-1 =2 x 10 10 Assuming a 10' diameter homogeneous emission (conservative) Including diffuse XRB, GRUBER_PARMAR bkg model

SIMBOL X Workshop Bologna May '07 Stellar emission vs. non-thermal emission Stellar emission (MPD) J 2032+4130 (CZT) Stellar emission (CZT) ● ● Point source subtraction is difficult (18” HEwidth) E>4 ke. V: Nonthermal component dominates

SIMBOL X Workshop Bologna May '07 Challenge: Background systematics in CZT Background (10' diameter) CZT S/B ~ 5% MPD Background (10' diameter)

SIMBOL X Workshop Bologna May '07 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?

SIMBOL X Workshop Ende! Vielen Dank für die Aufmerksamkeit Bologna May '07