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Swift observations of black hole candidate XTE J1752-223

Swift observations of black hole candidate XTE J1752-223. Peter A. Curran. with P. Casella. T.J. Maccarone & P.A. Evans. Laboratoire AIM, Irfu /Service d'Astrophysique CEA Saclay, France. Swift and X-ray transients. Gamma-ray burst (GRB) satellite: Burst Alert Telescope

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Swift observations of black hole candidate XTE J1752-223

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  1. Swift observations of black hole candidate XTE J1752-223 Peter A. Curran with P. Casella. T.J. Maccarone & P.A. Evans Laboratoire AIM, Irfu /Service d'Astrophysique CEA Saclay, France

  2. Swift and X-ray transients Gamma-ray burst (GRB) satellite: Burst Alert Telescope (BAT: 15-150 keV) X-ray Telescope (XRT: 0.2-10 keV) Ultraviolet & Optical Telescope (UVOT: UV,U,B,V)

  3. Swift and X-ray transients Flexible scheduling Fast pointing Timing & spectral capabilities Quasi-simultaneous observations (0.002-150 keV)

  4. All emissions regions probed by Swift Accretion Disk: warm/hot thermal (optical-X-ray) Companion Star: cool thermal (nIR-optical-UV) Corona, Jet: non-thermal (radio, X-ray)

  5. Discovered by RXTE on 2009-10-23 Black-hole candidate with radio-observed jet Observed by RXTE, Swift, Fermi, Suzaku, MAXI, & ground-based optical/radio telescopes ~50 Swift observations over 8 months (Curran et al. 2010) XTE J1752-223

  6. X-ray light curves Swift-BAT 15-150 keV MAXI 4-10 keV Swift-XRT 0.3-10 keV

  7. Identifying the states

  8. Identifying the states: XRT-BAT spectra Soft/thermal Hard (power-law) XRT BAT

  9. Spectral parameters & states intermediate hard soft hard

  10. X-ray light curves & states intermediate quiescence hard soft hard

  11. MAXI light curves 1.5-4 keV 4-10 keV 10-20 keV Matsuoka et al., 2009

  12. Hardness Intensity Diagrams

  13. Hardness Intensity Diagrams BAT/MAXI XRT

  14. Hardness Intensity Diagrams Soft – Intermediate - Hard BAT/MAXI XRT Fender et al., 2004

  15. XRT power spectra

  16. XRT power spectra Hard state (average) RMS ~54% Soft state (average) RMS <12%

  17. XRT power spectra: RMS intermediate soft hard hard

  18. XRT power spectra: QPO? QPO? Hard state (average) RMS ~54% Soft state (average) RMS <12%

  19. XRT power spectra: QPO? QPO? Hard state (individual sequence)

  20. Optical counterpart

  21. Counterpart (nIR) IMACS i’ band image Torres et al., 2009

  22. Counterpart & sub-arcsec position UVOT v band image DSS image

  23. Optical light curve variability

  24. Optical – X-ray correlation Early, hard state Soft state & later

  25. Optical – X-ray correlation Early, hard state Hysteresis: excess emission due to hard state jet? Soft state & later

  26. Counterpart colour? UVOT u-b-v

  27. Counterpart colour? Colour: 0 < β < 4

  28. XTE J1752-223: Further work Multi-wavelength spectral fits Radio – nIR/optical/UV – XRT – RXTE – Fermi

  29. Conclusions • Swift observations of the first known outburst of XTE J1752-223 allowed us to: • Confirm and refine the epochs of the canonical X-ray states • Confirm the optical counterpart and produce a sub-arcsecond position • Discover an optical - X-ray correlation and hysteresis effect Furthermore, these discussed properties of XTE J1752-223 support its candidacy as a black hole in the Galactic centre region

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