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

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Presentation transcript:

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

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

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

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

XTE J Discovered by RXTE on 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)

X-ray light curves MAXI 4-10 keV Swift-XRT keV Swift-BAT keV

Identifying the states

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

Spectral parameters & states hard soft hard intermediate

X-ray light curves & states quiescence hard softhard intermediate

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

Hardness Intensity Diagrams

XRT BAT/MAXI

Hardness Intensity Diagrams XRT BAT/MAXI

XRT power spectra

Hard state (average) RMS ~54% Soft state (average) RMS <12%

XRT power spectra: RMS hard soft hard intermediate

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

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

Optical counterpart

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

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

Optical light curve variability

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

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

Counterpart colour? UVOT u-b-v

Colour: 0 < β < 4 Counterpart colour?

XTE J : Further work Multi-wavelength spectral fits Radio – nIR/optical/UV – XRT – RXTE – Fermi Multi-wavelength spectral fits Radio – nIR/optical/UV – XRT – RXTE – Fermi

Conclusions Swift observations of the first known outburst of XTE J 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 J support its candidacy as a black hole in the Galactic centre region