Supernova Remnants interac1ng with molecular clouds as seen with H.E.S.S.
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1 Supernova Remnants interac1ng with molecular clouds as seen with H.E.S.S. MaJ DALTON, Peter EGER, Diane FERNANDEZ, Hélène LAFFON, Jérémie MEHAULT, Stefan OHM, Igor OYA, MaJhieu RENAUD on behalf of the H.E.S.S. collabora1on Rencontres de Moriond Very High Energy Phenomena in the Universe March 916, 2013 La Thuile, Italy
2 Features of SNRs interac1ng w/ MCs: SNRs interac1ng w/ MCs: W28N, W49B, W51C, IC443, W44 Luminous GeV & weak TeV sources Spectral break at a few GeV, steep at VHE FermiLAT D. Willasch h IC 443 Op1cal image SNR ΔIndex Ebreak (GeV) W28N 0.65± ±0.2 W49B 0.72± ±1.6 IC ± ±0.6 W ±0. 1.9±0.2 W51C 1.3± ± GeV Abdo et al., 2009 Abdo et al., 20 Aleskic et al., 2012 Ackermann et al., 2013 D. FERNANDEZ March 916,
3 H.E.S.S. Galac1c Plane Survey D. FERNANDEZ March 916,
4 3 H.E.S.S. sources associated to a SNRMC interac1on W51C W49B W28 D. FERNANDEZ March 916,
5 3 H.E.S.S. sources coincident w/ SNRMC interac1on but PWN emission possibly dominant W51C W49B Kes78 W28 W30 CTB 37A D. FERNANDEZ March 916,
6 4 new H.E.S.S. sources possibly associated to a SNRMC interac1on HESS J HESS J W51C W49B Kes78 W28 W30 CTB 37A RaDec HESS J HESS J D. FERNANDEZ March 916,
7 J : Discovered with the HESS survey (Aharonian et al., 2005) MAGIC dedicated paper (Albert et al., 2006) Images at the same scale MAGIC HESS Δ CCO SNR (NRAO, 20 cm) 13 CO (GRS, 7482 km/s) Black contours: 12 CO 90 cm VLA radio contours MAGIC tracking posi1ons MAGIC analysis source region D. FERNANDEZ March 916,
8 HESS J HESS J HESS J HESS J : Δ CCO SNR (NRAO, 20 cm) 13 CO (GRS, 7482 km/s) 2 H.E.S.S. components from the center of the remnant: Ptlike (coincident w/ CCO) + Extended (Ø=21 ) components k coincident w/ SNR G (W41): 4.2 kpc, 6x 4 yrs, Ø=27 f coincident w/ 12 CO (Dame et al., 1986) & 13 CO (Jackson et al., 2006) 13 CO peak density not compa1ble w/ VHE emission Possible OH maser (Green et al., 1996) but not confirmed f Xray CCO at the center of the remnant, no pulsa1ons Nonthermal Xray diffuse emission => PWN candidate (Misanovic et al., 2011; Mukherjee et al., 2009) coincident w/ a FermiLAT extended source (compa1ble w/ CCO) PL spectrum ( no exp. cutoff) D. FERNANDEZ March 916,
9 HESS J HESS J HESS J HESS J : 2 H.E.S.S. components from the center of the remnant: Ptlike (coincident w/ CCO) + Extended (Ø=21 ) components k coincident w/ SNR G (W41): 4.2 kpc, 6x 4 yrs, Ø=27 f coincident w/ 12 CO (Dame et al., 1986) & 13 CO (Jackson et al., 2006) 13 CO peak density not compa6ble w/ VHE emission Possible OH maser (Green et al., 1996) but not confirmed f Xray CCO at the center of the remnant, no pulsa6ons Nonthermal Xray diffuse emission => PWN candidate (Misanovic et al., 2011; Mukherjee et al., 2009) Δ CCO SNR (NRAO, 20 cm) 13 CO (GRS, 7482 km/s) coincident w/ a FermiLAT extended source (compa1ble w/ CCO) PL spectrum ( no exp. cutoff) D. FERNANDEZ March 916, 2013 Against SNR shell emission Against SNR MC emission Against PSR scenario 9
10 HESS J HESS J HESS J HESS J : Δ CCO SNR (NRAO, 20 cm) 13 CO (GRS, 7482 km/s) Possible PWN emission 2 H.E.S.S. components from the center of the remnant: Ptlike (coincident w/ CCO) + Extended (Ø=21 ) components k coincident w/ SNR G (W41): 4.2 kpc, 6x 4 yrs, Ø=27 f coincident w/ 12 CO (Dame et al., 1986) & 13 CO (Jackson et al., 2006) 13 CO peak density not compa6ble w/ VHE emission Possible OH maser (Green et al., 1996) but not confirmed f Xray CCO at the center of the remnant, no pulsa6ons Nonthermal Xray diffuse emission => PWN candidate (Misanovic et al., 2011; Mukherjee et al., 2009) Possible SNRMC shock coincident w/ a FermiLAT extended source (compa1ble w/ CCO) PL spectrum ( no exp. cutoff) D. FERNANDEZ March 916, 2013
11 HESS J : HESS J SNRMC interac=on scenario: Fermi + HESS extended region spectra Hadronic emission: W CR ~ 50 erg Broad GeV plasorm: 10GeV => E break ~ 0 GeV Δ CCO SNR (NRAO, 20 cm) 13 CO (GRS, 7482 km/s) PWN scenario : HESS central region spectrum Spin down power : erg/s SNRMC and PWN scenario : Fermi + 2 HESS components spectra Γ=2.15±0.16 Γ=2.60±0.07 Γ=2.67±0.11 Φ extended (130 TeV) 5% Crab Φ central (130 TeV) 2% Crab D. FERNANDEZ March 916,
12 Integrated 13 CO antenna temperature (arbitrary units) HESS J HESS J Cloud a: 2.3kpc 2631 km/s HESS J : Cloud b: 4.5kpc 7381 km/s HESS excess contours (801 γ) White: radio contours H.E.S.S. source: pointlike or extension 0.09 (99% CL) close to the G radio rim coincident with 2 clouds : 13 CO (J=0>1) (Jackson et al., 2006) Xray pointlike source 1 away from the H.E.S.S. source bestfit posi1on (No pulsa1ons No extended emission) No counterpart with FermiLAT (Nolan et al., 2012) HESS J D. FERNANDEZ March 916,
13 Integrated 13 CO antenna temperature (arbitrary units) HESS J HESS J Against SNRMC scenario Against PSRPWN scenario Cloud a: 2.3kpc 2631 km/s HESS J : H.E.S.S. source: pointlike or extension 0.09 (99% CL) close to the G radio rim coincident with 2 clouds : 13 CO (J=0>1) (Jackson et al., 2006) Xray pointlike source 1 away from the H.E.S.S. source bestfit posi1on (No pulsa6ons No extended emission) No counterpart with FermiLAT (Nolan et al., 2012) HESS J Cloud b: 4.5kpc 7381 km/s HESS excess contours (801 γ) White: radio contours Possible SNRMC shock Possible PSR PWN scenario D. FERNANDEZ March 916,
14 HESS J s -1 ] -2 dn/de [erg.cm 2 E FermiLAT H.E.S.S. Γ=2.5±0.3 HESS J Against SNRMC scenario Against PSRPWN scenario -13 HESS J : H.E.S.S. source: pointlike or extension 0.09 (99% CL) close to the G radio rim coincident with 2 clouds : 13 CO (J=0>1) (Jackson et al., 2006) Xray pointlike source 1 away from the H.E.S.S. source bestfit posi1on (No pulsa6ons No extended emission) No counterpart with FermiLAT (Nolan et al., 2012) -2 Φ(>1TeV) 1% Crab -1 1 E [TeV] Possible SNRMC shock Possible PSR PWN scenario Assuming a SNRMC interac=on : kkk D. FERNANDEZ March 916,
15 4 new H.E.S.S. sources possibly associated to a SNRMC interac1on HESS J HESS J W51C W49B Kes78 W28 W30 CTB 37A RaDec HESS J HESS J D. FERNANDEZ March 916,
16 E > 4TeV HESS excess map: HESS best fit posi1on HESS extension: Ø=9 HESS J HESS J : Radio contours O HESS J O FermiLAT source bestfit posi1on O XMM: PWN candidate Extended H.E.S.S. source Coincident w/ the northern part of the G SNR shell: D 8kpc or D 13kpc (Lemière et al., 2009; Davies et al., 2012), Ø=8 HII region between SNR G & SNR G Nearby stellar cluster Mc81 Coincident w/ an extended Xray source (Funk et al., 2007) + Ptlike Xray source (Lemière et al., 2009) Coincident w/ a FermiLAT source (Slane et al., 20) D. FERNANDEZ March 916,
17 E > 4TeV HESS excess map: HESS best fit posi1on HESS extension: Ø=9 HESS J HESS J : Radio contours O HESS J O FermiLAT source bestfit posi1on O XMM: PWN candidate Extended H.E.S.S. source Coincident w/ the northern part of the G SNR shell: D 8kpc or D 13kpc (Lemière et al., 2009; Davies et al., 2012), Ø=8 HII region between SNR G & SNR G Nearby stellar cluster Mc81 Coincident w/ an extended Xray source (Funk et al., 2007) + Ptlike Xray source (Lemière et al., 2009) Coincident w/ a FermiLAT source (Slane et al., 20) First interpreted as PSRPWN scenario (Lemière et al., 2009; Slane et al., 20) D. FERNANDEZ March 916,
18 dn/de [erg.cm -2.s -1 ] FermiLAT Γ=2.3±0.1 HESS excess map: HESS best fit posi1on HESS extension: Ø=9 E -12 H.E.S.S. Γ=2.15±0. Ecut = 7.3 TeV Φ(>1TeV) 8% Crab -3 u E [TeV] HESS J : Extended H.E.S.S. source Coincident w/ the northern part of the G SNR shell: D 8kpc or D 13kpc (Lemière et al., 2009; Davies et al., 2012), Ø=8 HII region between SNR G & SNR G Nearby stellar cluster Mc81 Coincident w/ an extended Xray source (Funk et al., 2007) + Ptlike Xray source (Lemière et al., 2009) Coincident w/ a FermiLAT source (Slane et al., 20) Radio contours O HESS J O FermiLAT source bestfit posi1on O XMM: PWN candidate The new H.E.S.S. results and MWL data suggest that at least part of the TeV emission is likely of hadronic origin. Total energy in interac1ng protons of up to W p n H 4x 52 (d/kpc) erg cm 3 D. FERNANDEZ March 916,
19 E > 4TeV All events HESS J E > 4TeV HESS J HESS J : H.E.S.S. source: ptlike or small extension (Ø=3.6 ) Coincident w/ SNR G : D 11kpc (Kothes & Dougherty, 2007) Ø=9 (Green, 2009) or Ø=5 (Whiteoak et al.,1996) HII region between SNR G & SNR G Nearby stellar cluster Mc81 No evident Xray counterpart No GeV counterpart D. FERNANDEZ March 916,
20 E > 4TeV All events HESS J E > 4TeV HESS J HESS J : H.E.S.S. source: ptlike or small extension (Ø=3.6 ) Coincident w/ SNR G : D 11kpc (Kothes & Dougherty, 2007) Ø=9 (Green, 2009) or Ø=5 (Whiteoak et al.,1996) HII region between SNR G & SNR G Nearby stellar cluster Mc81 No evident Xray counterpart No GeV counterpart SNR shell much larger than VHE source: PWN scenario? Against PSRPWN scenario D. FERNANDEZ March 916,
21 E > 4TeV Radio image (843MHz) 5,6,7,8σ contours (E>4TeV) G Jy/beam HII Region G Γ=1.99±0.13 Φ(>1TeV) 1.7% Crab HII Region G HESS J HESS J : HESS J FGL J SNR G H.E.S.S. source: ptlike or small extension (Ø=3.6 ) Coincident w/ SNR G : D 11kpc (Kothes & Dougherty, 2007) Ø=9 (Green, 2009) or Ø=5 (Whiteoak et al.,1996) HII region between SNR G & SNR G Nearby stellar cluster Mc81 No evident Xray counterpart No GeV counterpart HII bridge + similari1es between the 2 SNRs: Emission from same hadronic origin? D. FERNANDEZ March 916,
22 H.E.S.S. sources associated and possibly associated to a SNRMC interac1on HESS J HESS J W51C W49B Kes78 W28 W30 CTB 37A HESS J HESS J D. FERNANDEZ March 916,
23 Comparison of integrated GeV and TeV fluxes for different kind of TeV sources coincident w/ a SNR.s -1 ] -2 I(1-0GeV) [cm W49B W28N W51C W30 IC443 CTB37A W41 J1640 J1641 CasA J1832 J1731 SN06 Tycho RCW86 VelaJr RXJ1713 TeV emission from: SNRMC shock Possible SNRMC shock Isolated SNR -13 1% Crab I(1-0TeV) [cm.s -1 ] D. FERNANDEZ March 916,
24 Ra1o of integrated GeV and TeV fluxes vs SNR age for different kind of TeV sources coincident w/ a SNR I(1-0GeV)/I(1-0TeV) CasA W49B CTB37A Tycho SN06 RCW86 VelaJr J1640 J1731 IC443 W51C W30 W41 W28N TeV emission from: SNRMC shock Possible SNRMC shock Isolated SNR RXJ Age [yrs] D. FERNANDEZ March 916,
25 Conclusion and outlook (1/2) : Some trends between the two popula1ons of SNRs (SNRMC & isolated SNRs) are apparent in the data : SNRs interac=ng w/ MCs: W28, W51C, W49B, IC443 I GeV >> I TeV : Steepening of the spectra around E γ = 1 GeV Isolated SNRs: Vela Jr, HESS J , RCW 86, RX J , SN06 Young SNRs I GeV /I TeV much lower than for SNRMC systems: Hard GeV & strong TeV sources H.E.S.S. new sources possibly interac=ng w/ MCs : HESS J , HESS J , HESS J , HESS J I GeV vs I TeV : sources between the two popula1ons of SNRs I GeV /I TeV vs Age: sources between the two popula1ons of SNRs D. FERNANDEZ March 916,
26 Conclusion and outlook (2/2) : H.E.S.S. II: lower energy threshold Improved sensi1vity and resolu1on FermiLAT HESS II HESS I W44: a SNRMC undetected at VHE Will be further explored with H.E.S.S. II Ackermann et al., 2013 D. FERNANDEZ March 916,
27 Thank you for your ajen1on. D. FERNANDEZ March 916,
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