A Multiwavelength Study of Cygnus X-1: the First mid-ir Spectroscopic Detection of Compact Jets
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1 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
2 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)
3 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
4 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 () constrain the spectral break (physical conditions within jet) (2) origin of midir continuum (variations?) (3) dust (spectroscopic features, excess?)
5 Spectral States & Radio Activity ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD
6 Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod MJD 5353
7 Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD HS jet.6.5 SL2 Nod SL2 Nod2 SL Nod SL Nod2 LL2 Nod LL2 Nod2 LL Nod LL Nod MJD 5353
8 Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD HS jet 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 Nod MJD 5353 MJD 53528
9 Spectral States & Radio Activity.6.4 ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD HS jet IS jet 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 Nod MJD 5353 MJD 53528
10 Spectral States & Radio Activity ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD HS jet IS jet 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 Nod MJD 5353 MJD MJD 53553
11 Spectral States & Radio Activity ASM HR2 ASM Counts/s RXTE RXTE Flux (mjy) MJD HS jet IS jet HS no jet 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 Nod MJD 5353 MJD MJD 53553
12 Dereddened midir Spectra.4.3 Obs IS with jet HS with jet Wavelength (microns) HS without jet
13 Dereddened midir Spectra Same level.4.3 Obs IS with jet HS with jet Wavelength (microns) HS without jet Due to the companion star photosphere at nearir and short midir wavelengths
14 Dereddened midir Spectra Same level.4.3 Obs Variable midir continuum IS with jet HS with jet 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
15 Dereddened midir Spectra Same level.4.3 Obs Variable midir continuum IS with jet HS with jet 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
16 HS without Jet(s) O9.7Iab star Res (Jy) 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
17 HS without Jet(s) / 9.7Iab photosphere with BB, T=28 K and R/D free, but excess
18 HS without Jet(s) 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)
19 HS without Jet(s) 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
20 HS with Jet(s) 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
21 HS with Jet(s) / Photosphere parameters (T, R/D) and bremsstrahlung index (ß) fixed
22 HS with Jet(s).5 O9.7Iab star Bremsstrahlung Compact jets 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
23 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) 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
24 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))
25 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)
26 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
27 IS with Jet(s).5 O9.7Iab star Bremsstrahlung Compact jets 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)
28 Wind Clumpiness Massloss rate including wind clumpiness (Lamers & Waters 984) If =, then
29 Wind Clumpiness Massloss rate including wind clumpiness (Lamers & Waters 984) If =, then 3 to 4x higher than in Gies et al. (23) => f =.9.
30 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.
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