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

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

  1. 1. Bologna May '07SIMBOL X Workshop X-ray emission from GALACTIC very high energy (E>100 GeV) 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
  2. 2. Bologna May '07SIMBOL X Workshop VHE/X-ray connection (keV-TeV) Sturner et al. (1997) SIM-XSIM-X SIM-XSIM-X VHE SIM-XSIM-X
  3. 3. Bologna May '07SIMBOL X Workshop 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)
  4. 4. Bologna May '07SIMBOL X Workshop 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
  5. 5. Bologna May '07SIMBOL X Workshop Cat I: MSH 15-52(PWN) White Contours HESS Colour: ISGRI (not pulsed) Forot et al. 2006 Khelifi et al. 2005 INTEGRAL: cut-off at 160 keV?
  6. 6. Bologna May '07SIMBOL X Workshop Cat I or II? HESS J1813-178 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. (2007b)
  7. 7. Bologna May '07SIMBOL X Workshop Cat I/II: Vela X, prototype “Offset” Nebula DH et al. (2006): ASCA 2-10 keV FOV Position dependent cut-off? Primary particle cooling? Bright but very extended source
  8. 8. Bologna May '07SIMBOL X Workshop Very faint X-ray emission (Fx <FVHE ) 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)
  9. 9. Bologna May '07SIMBOL X Workshop 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) Fx <FVHE
  10. 10. Bologna May '07SIMBOL X Workshop CAT II: HESS J1804-216 Cui&Konopelko (2006) Bamba et al. (2006) Landi et al. (2006) Kargaltsev et al. (2007) Kargaltsev et al (2007) Γ=1.2+/-0.4 F2-10 ~10-13 ergs/(cm2 s) (white contours ROSAT, black contours 20 cm, colour VHE excess map)
  11. 11. Bologna May '07SIMBOL X Workshop Cat II “Rabbit” & “Kookaburra” Aharonian et al. 2006 INTEGRAL detection Hoffmann, DH et al. (2006) Two PWN candidates Very similar in VHE gamma-rays RX <RVHE FX <FVHEINTEGRAL 20-40 keV
  12. 12. Bologna May '07SIMBOL X Workshop Cat II or III?: HESS J1634-472=G337.2+0.1 or IGR J16358-4726 Combi et al. 2006 Hard X-ray spectrum G=1.8+/-0.5, fX ~10-12 ergs cm-2 s-1
  13. 13. Bologna May '07SIMBOL X Workshop Similar:HESS J1632-478 G336.4+0.2 DH et al. (2007) XMM-Newton 2-10 keV Hard X-ray spectrum, maybe IC X-rays?
  14. 14. Bologna May '07SIMBOL X Workshop 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)
  15. 15. Bologna May '07SIMBOL X Workshop 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)
  16. 16. Bologna May '07SIMBOL X Workshop 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
  17. 17. Bologna May '07SIMBOL X Workshop MILAGRO 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
  18. 18. Bologna May '07SIMBOL X Workshop 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 subtracted smoothed with 45” Sources subtracted smoothed with 90” Excess contours from TeVJ2032+4130 Core of Cyg OB2 DH et al. 2007
  19. 19. Bologna May '07SIMBOL X Workshop Spectral energy distribution and interpretation: TeV J2032+4130 a Pevatron?
  20. 20. Bologna May '07SIMBOL X Workshop 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
  21. 21. Bologna May '07SIMBOL X Workshop 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
  22. 22. Bologna May '07SIMBOL X Workshop Challenge: Background systematics in CZT CZT S/B ~ 5% MPD Background (10' diameter) CZT Background (10' diameter)
  23. 23. Bologna May '07SIMBOL X Workshop 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?
  24. 24. Bologna May '07SIMBOL X Workshop Ende! Vielen Dank für die Aufmerksamkeit

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