Smithsonian Astrophysica A Multiwavelength Study of Cygnus X: the First midir Spectroscopic Detection of Compact Jets F. Rahoui, Harvard University & CfA J.C. Lee, S. Heinz, D.C. Hines, K. Pottschmidt, J. Wilms & V. Grinberg Rahoui et al, 2, ApJ, 736, 63 Celebrating 5 years since the discovery of Sco X, July th 22
Cygnus X BH, HMXB, 9.7Iab companion star (Walborn 973) D.86 kpc (Xiang et al. 2 Xray scattering halo; Reid et al. 2 parallax) Focusedwind accretion, intermediate between BondiHoyle and RLO (Gies et al. 986, 23; Hanke et al. 29) 2/3 in the HS with many failed transitions to SS (IS, Wilms et al. 26)
Cygnus X BH, HMXB, 9.7Iab companion star (Walborn 973) D.86 kpc (Xiang et al. 2 Xray scattering halo; Reid et al. 2 parallax) Focusedwind accretion, intermediate between BondiHoyle and RLO (Gies et al. 986, 23; Hanke et al. 29) 2/3 in the HS with many failed transitions to SS (IS, Wilms et al. 26) OBS # (25) SPITZER/IRS PCA+HEXTE RYLE@5 GHz 5353.3998 5353.5444 5353.4333 5353.2425 5353.3986 5353.5463 2 53528.95922 53528.97367 53528.9698 53529.24333 53528.95935 53528.97375 3 53553.299 53553.2746 53552.9796 53553.9888 53553.36 53553.2756
Cygnus X BH, HMXB, 9.7Iab companion star (Walborn 973) D.86 kpc (Xiang et al. 2 Xray scattering halo; Reid et al. 2 parallax) Focusedwind accretion, intermediate between BondiHoyle and RLO (Gies et al. 986, 23; Hanke et al. 29) 2/3 in the HS with many failed transitions to SS (IS, Wilms et al. 26) OBS # (25) SPITZER/IRS PCA+HEXTE RYLE@5 GHz Goals 5353.3998 5353.5444 5353.4333 5353.2425 5353.3986 5353.5463 () constrain the spectral break (physical conditions within jet) 2 53528.95922 53528.97367 53528.9698 53529.24333 53528.95935 53528.97375 (2) origin of midir continuum (variations?) 3 53553.299 53553.2746 53552.9796 53553.9888 53553.36 53553.2756 (3) dust (spectroscopic features, excess?)
Spectral States & Radio Activity ASM HR2 ASM Counts/s.6.4.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD
Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.4.3.2...4.42.44.46.48.5.52.54 MJD 5353
Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD HS jet.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.4.3.2...4.42.44.46.48.5.52.54 MJD 5353
Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD HS jet.6.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.4.4.3.2.3.2.....4.42.44.46.48.5.52.54.96.962.964.966.968.97.972.974 MJD 5353 MJD 53528
Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD HS jet IS jet.6.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.4.4.3.2.3.2.....4.42.44.46.48.5.52.54.96.962.964.966.968.97.972.974 MJD 5353 MJD 53528
Spectral States & Radio Activity ASM HR2 ASM Counts/s.6.4.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD HS jet IS jet.6.6.7.5.4 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.5.4 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.3.2.3.2.4.3.2......4.42.44.46.48.5.52.54.96.962.964.966.968.97.972.974 MJD 5353 MJD 53528..2.4.6.8.2.22.24.26.28 MJD 53553
Spectral States & Radio Activity ASM HR2 ASM Counts/s.6.4.2.8 5 4 3 2 RXTE RXTE Flux (mjy) 27 24 2 8 5 2 9 6 3 535 535 5352 5353 5354 5355 5356 5357 MJD HS jet IS jet HS no jet.6.6.7.5.4 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.5.4 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod2.3.2.3.2.4.3.2......4.42.44.46.48.5.52.54.96.962.964.966.968.97.972.974 MJD 5353 MJD 53528..2.4.6.8.2.22.24.26.28 MJD 53553
Dereddened midir Spectra.4.3 Obs. 2 3.2..9.8.7.6.5.4 IS with jet HS with jet 6 7 8 9 2 3 Wavelength (microns) HS without jet
Dereddened midir Spectra Same level.4.3 Obs. 2 3.2..9.8.7.6.5.4 IS with jet HS with jet 6 7 8 9 2 3 Wavelength (microns) HS without jet Due to the companion star photosphere at nearir and short midir wavelengths
Dereddened midir Spectra Same level.4.3 Obs. 2 3.2..9.8.7.6.5.4 Variable midir continuum IS with jet HS with jet 6 7 8 9 2 3 Wavelength (microns) HS without jet Due to the companion star photosphere at nearir and short midir wavelengths Variations at longer midir wavelengths may be due to: Synchrotron emission from compact jets Bremsstrahlung from stellar winds
Dereddened midir Spectra Same level.4.3 Obs. 2 3.2..9.8.7.6.5.4 Variable midir continuum IS with jet HS with jet 6 7 8 9 2 3 Wavelength (microns) Due to the companion star photosphere at nearir and short midir wavelengths Variations at longer midir wavelengths may be due to: Synchrotron emission from compact jets Bremsstrahlung from stellar winds HEATED DUST J.C. Lee et al, in prep HS without jet
HS without Jet(s) O9.7Iab star Res (Jy).4.3.2..5.4.3.5.5 e+3 2e+3 3e+3 4e+3 5e+3 Frequency (Hz) / 9.7Iab photosphere with BB, T=28 K and R/D free, but excess
HS without Jet(s) / 9.7Iab photosphere with BB, T=28 K and R/D free, but excess
HS without Jet(s).4.3.2..5.4.3 O9.7Iab star Bremsstrahlung Res (Jy).5.5 e+3 2e+3 3e+3 4e+3 5e+3 Frequency (Hz) / 9.7Iab photosphere with BB, T=28 K and R/D free, but excess 2/ Add S ν α ν ß and ß=.55±.7.6, value for bremsstrahlung from a spherically expanding stellar wind (Wright&Barlow 975, Panagia&Felli 975)
HS without Jet(s).4.3.2..5.4.3 O9.7Iab star Bremsstrahlung Res (Jy).5.5 e+3 2e+3 3e+3 4e+3 5e+3 Frequency (Hz) / 9.7Iab photosphere with BB, T=28 K and R/D free, but excess 2/ Add S ν α ν ß and ß=.55±.7.6, value for bremsstrahlung from a spherically expanding stellar wind (Wright&Barlow 975, Panagia&Felli 975) No jet => midir continuum due to photosphere and stellar winds
HS with Jet(s).5.25..5 Optically thick O9.7Iab star Bremsstrahlung Compact jets.2 Res (Jy).2.2 e+ e+ e+2 e+3 / Photosphere parameters (T, R/D) and bremsstrahlung index (ß) fixed 2/ Add PL to mimic synchrotron emission of compact jet => similar bremsstrahlung as HS w/o jet Frequency (Hz) => flat PL consistent with optically thick synchrotron from jet
HS with Jet(s) / Photosphere parameters (T, R/D) and bremsstrahlung index (ß) fixed
HS with Jet(s).5 O9.7Iab star Bremsstrahlung Compact jets.25..5 Optically thick Optically thin.2 Res (Jy).2.2 e+ e+ e+2 e+3 Frequency (Hz) / Photosphere parameters (T, R/D) and bremsstrahlung index (ß) fixed 3/ Add broken PL to mimic compact jet optically thicktothin synchrotron emission (Blandford&Königl 979) Bremsstrahlung normalization fixed to Obs 3 and broken PL free Bremsstrahlung normalization fixed to value for simple PL and broken PL free Bremsstrahlung normalization free to and opticallythin index fixed to.6
HS with Jet(s).5 O9.7Iab star Bremsstrahlung Compact jets ν b 2.7x 3 Hz => B 2x 4 G (model in Chaty et al. 2).25..5 Optically thick Optically thin.2 Res (Jy).2.2 e+ e+ e+2 e+3 Frequency (Hz) / Photosphere parameters (T, R/D) and bremsstrahlung index (ß) fixed 3/ Add broken PL to mimic compact jet optically thicktothin synchrotron emission (Blandford&Königl 979) Bremsstrahlung normalization fixed to Obs 3 and broken PL free Bremsstrahlung normalization fixed to value for simple PL and broken PL free Bremsstrahlung normalization free to and opticallythin index fixed to.6 } Similar Results Improvement
Radio to Xray SED during HS with Jet O9.7Iab star Bremsstrahlung Compact jet IRS/MIR... /5Ghz RXTE/Xray. e5 e6 e+ e+2 e+4 e+6 e+8 e+2 e+22 Log(Frequency (Hz))
Radio to Xray SED during HS with Jet O9.7Iab star Bremsstrahlung Compact jet IRS/MIR... /5Ghz RXTE/Xray. e5 ISGRI/ e6 e+ e+2 e+4 e+6 e+8 e+2 e+22 Log(Frequency (Hz)) IR slope consistent with INTEGRAL polarized emission in Laurent et al. (Science, 2)
Radio to Xray SED during HS with Jet O9.7Iab star Bremsstrahlung Compact jet IRS/MIR... /5Ghz RXTE/Xray. e5 ISGRI/ e6 e+ e+2 e+4 e+6 e+8 e+2 e+22 Log(Frequency (Hz)) IR slope consistent with INTEGRAL polarized emission in Laurent et al. (Science, 2) IR slope underestimates RXTE => both the jet and corona contribute to Xrays but corona dominates below 2 kev
IS with Jet(s).5 O9.7Iab star Bremsstrahlung Compact jets.25..5.2 Res (Jy).2.2 e+ e+ e+2 e+3 Frequency (Hz) / Bestfit suggests break shifted to higher frequency, as expected 2/ Bremsstrahlung level 34% lower than HS ( with and w/o jets): => lower massloss rate of stellar winds => consistent with anticorrelation massaccretion/massloss rates (Gies et al. 23, 28)
Wind Clumpiness Massloss rate including wind clumpiness (Lamers & Waters 984) If =, then
Wind Clumpiness Massloss rate including wind clumpiness (Lamers & Waters 984) If =, then 3 to 4x higher than in Gies et al. (23) => f =.9.
Summary & Conclusion Significant contribution of compact jets to midir spectrum first spectroscopic measurement of the jet spectral break in a microquasar (Rahoui et al. 2) but photometric breaks have been detected for GX 3394 (Corbel & Fender 22, Gandhi et al. 2) Cygnus X: ν b =2.7 3 Hz µm => B 2x 4 G Jet consistent with polarized γray detected by INTEGRAL but not with Xrays detected by RXTE Presence of a coronadominated Xray emission Significant stellar wind bremsstrahlung Massloss rate anticorrelated to massaccretion rate Stellar winds likely clumpy with f.