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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 - PowerPoint PPT Presentation
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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'AstrophysiqueCEA Saclay, France
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)
Swift and X-ray transients
Flexible scheduling
Fast pointing
Timing & spectral capabilities
Quasi-simultaneous observations (0.002-150 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 J1752-223
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)
X-ray light curves
MAXI4-10 keV
Swift-XRT0.3-10 keV
Swift-BAT15-150 keV
Identifying the states
Identifying the states: XRT-BAT spectra
Hard (power-law)
Soft/thermal
XRTXRT BATBAT
Spectral parameters & states
ha
rd soft
hard
inte
rmed
iate
X-ray light curves & states
qu
iesc
en
ceh
ard
soft
hard
inte
rmed
iate
MAXI light curves1.5-4 keV
4-10 keV
10-20 keV
Matsuoka et al., 2009
Hardness Intensity Diagrams
Hardness Intensity Diagrams
XRT
BAT/MAXI
Hardness Intensity Diagrams
XRT
BAT/MAXI
Fender et al., 2004
XRT power spectra
XRT power spectra
Hard state (average)RMS ~54%
Soft state (average)RMS <12%
XRT power spectra: RMS
ha
rd soft
hardin
term
edia
te
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?
Hysteresis: excess emission
due to hard state jet?
Counterpart colour?
UVOT u-b-v
Colour: 0 < β < 4
Counterpart colour?
XTE J1752-223: 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 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