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IC 10 X-1: A Long Look with XMM-Newton

IC 10 X-1: A Long Look with XMM-Newton. Tod Strohmayer: NASA ’ s Goddard Space Flight Center (and JSI). with Dheeraj Pasham (UMD), Richard Mushotzky (UMD). IC 10 X-1: Summary. Dynamically confirmed black hole binary with Wolf-Rayet companion ([MAC92] 17A, WNE spectral type).

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IC 10 X-1: A Long Look with XMM-Newton

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  1. IC 10 X-1: A Long Look with XMM-Newton Tod Strohmayer: NASA’s Goddard Space Flight Center (and JSI) with Dheeraj Pasham (UMD), Richard Mushotzky (UMD)

  2. IC 10 X-1: Summary • Dynamically confirmed black hole binary with Wolf-Rayet companion ([MAC92] 17A, WNE spectral type). • X-ray light curve shows eclipse-like intensity drops with Porb = 34.9 hr (Prestwich et al. 2007; Silverman & Filippenko 2008). • Mass function from optical radial velocity curve: f(M) = 7.64 ± 1.26 M (Silverman & Filippenko 2008)  Mbh > 23 – 34 M-- MOST MASSIVE KNOWN Stellar BH! • Lx ~ 2 – 5 x 1038 ergs/s (d=740 kpc), X-ray spectrum consistent with a comptonized “thermal” StBH disk (~1 keV). Similar to “super-soft” behavior in Cyg X-3, but also 4-5 keV roll-over (like some ULXs)? • Study temporal - spectral properties to compare this massive StBH with Galactic BHs and ULXs and do “eclipse mapping.” Cycle 11 observations of a complete orbit (~35 hr).

  3. One Complete Orbit With XMM-Newton • Very little flaring during observation! Eclipse feature clearly evident and resolved. • Eclipse is asymmetric (steeper ingress), not total (8-9% of off eclipse), but has a “flat” minimum of duration of 5 hr. • Significant variability evident.

  4. New Timing Results: 7 mHz QPO Wang et al. (2004) • 2003 data showed marginal feature at 7 mHz • New Cycle 11 data clearly confirm the QPO! With amplitude (rms) of 5.6%, centroid frequency of 6.75 mHz, and coherence Q~10. • Power-law + Lorentzian (QPO) fits the spectrum.

  5. IC 10 X-1: New QPO Detection • Feature evident in a dynamic spectrum. No obvious frequency drift, but low signal to noise. • Power-law continuum of slope ~1.5, no break detected, but orbital modulations make it tough. Frequency Time • 7 mHz is a low frequency for a StBH! Particularly for a Type – C classification. • Spectral state not obviously like other Type – C QPOs. • GRS 1915+105 may have frequencies this low.

  6. IC 10 X-1: Eclipse Timing and Mass Constraint • Eclipse duration constrains size of WR companion (as seen from BH) and inclination. • “flat” bottom to the eclipse feature evident in soft and hard energy bands. Duration of 5 hr. • Wolf-Rayet winds are optically thick! Need to account (or at least approximate) this effect. • Such winds are a strong function of Luminosity and thus stellar mass. • Use known mass function, eclipse geometry constraint, and Reff (M) to constrain component masses and i

  7. IC 10 X-1: Eclipse Timing and Mass Constraints • Derive Reff using mass loss rates from Nugis & Lamers (2000), and simple approximations from Langer (1989). • The eclipse is “direct” evidence for an optically thick WR wind! • Solutions exist for range of companion masses. Suggest Mbh > 27 M

  8. IC 10 X-1: X-ray Spectrum • Spectrum is relatively “soft,” continuum can be modeled with thermal comptonization (comptb in XSPEC). • Analogy with Cyg X-3 in its “ultra-soft” state. • Evidence for “discrete” features near 1 keV. • Orbit phase related variations in the spectral hardess. • “shallow” egress appears hardest. • Should be able to map column through the WR wind..

  9. IC 10 X-1: Eclipse Spectrum There is significant emission during eclipse. Likely at least partly due to scattering and an emission line spectrum from the photo-ionized wind!

  10. Bonus Slide: RGS Line Emission! 1st order 2nd order Several emission line features clearly detected: 12 Å, consistent with Ne X (2-1) ; at 15 Å, maybe Fe XVII; near 17 Å, perhaps OVII; at 26 Å plausibly C. Carbon, Oxygen Neon are products of He burning, so not unexpected.

  11. Summary • Massive StBH with a low frequency QPO (7 mHz). Frequency lower than in some claimed IMBH candidates. Mass estimates from frequency scalings are possible, but must compare “apples with apples.” • SEE POSTER 126.43 for related work in M82 X-1  • Complete eclipse observed (resolved) for the first time. Eclipse duration constrains size of the WR companion. Direct evidence for optically thick WR wind. Mass and inclination constraints follow. • Spectrum consistent with comptonized BH disk emission. Variations evident with orbital phase, more detailed modeling in progress. • Rich line spectrum in RGS, probes the composition and properties of photoionized wind. Again, more details to come.

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