discovery and evolution of a new galactic black hole candidate xte j1752-223
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Discovery and Evolution of aNew Galactic Black Hole Candidate
XTE J1752-223
N. Shaposhnikov1,2,3, J. Swank3, C. Markwardt1,2,3, H. Krimm2,3,4
The Astrophysical Journal, 723, 2,1817 1University of Maryland, Astronomy Department2Center for Research and Exploration in Space Science & Technology (CRESST)3NASA/Goddrd Space Flight Center4Universities Space Research Association
4th MAXI Workshop 2010, Tokyo, November 29, 2010
DiscoveryXTE J1752-223
• RXTE/PCA Galactic Bulge Scans showed an unidentified new source on October 21, 2009. Scans on October 23 fully confirmed a new source (Atel #2258)
• Subsequent Swift/XRT observation showed bright point source with very hard non-thermal spectrum with index Γ = 1.2 and NH =0.47×1022 cm-2 (Atel #2261)
October, 21 2009
October 20, 2009
October, 23 2009
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
4th MAXI Workshop 2010, Tokyo, November 29, 2010Shaposhnikov, Swank, Markwardt &Krimm
XTE J1752-223 Evolution
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
Hardness – Intensity Diagram
Data modeling:Energy spectral model• Comptonization (BMC)• Gaussian for the iron line
at ~6.5 keV• Modified by interstellar
absorption (measured by Swift/XRT)
• High energy cutoff
Power Density Spectra• Power law or broken
power law for the broad band variability
• Loretzians for QPOs
RXTE Data Spectral Analysis
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
QPO
Shaposhnikov et al. ApJ,2010
XTE J1752-223 Variability Evolution
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
LHS HIMS SIMS HSS IS LHS
Low Hard State in XTE J1752-223
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
XTE J1752-223
GX 339-4
Power Spectra
Fourier Resolved Spectroscopy (FRS)
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
XTE J1752-223
Low Hard StateGX 339-4
Fourier Resolved Spectroscopy (continued)
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
State Transition
HIMS SIMS
Lowest QPOs during the beginning of the transition are softer than the time averaged spectrum. As the transition evolves they quickly become harder (Sobolewska & Zycki 2006). QPO spectrum is always harder that
the broad band noise.
Fourier Resolved Spectroscopy (HIMS)
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
FRS normalized by total spectrum
FRS normalized by the non-thermal
spectral component
(Shaposhnikov et al. 2010)
Disk black body spectral component is stable!RMS ratio normalized on the power law component alone is decreasing
from the level of 50% (LHS!).
What can we learn from spectral data?Nature of the power law
E- Thermal Comptonization:
€
Nsc ~ τ 2,
€
η =4kT /mec2
€
~ [(4kT /mec2)2τ 2]−1
(Rubicki & Lightman, 79)
Bulk Motion Comptonization:
(S & Titarchuk, 2009)
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
(Laurent & Titarchuk 2010)
€
η∝τ −1, Nsc ∝ τ ⇒ α ≈ const
Thermal versus Bulk motion Comptonization
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
(S & Titarchuk 2010)
XTE J1550-564
Thermal
BMC
High Energy Cutoff Evolution
Thermal
BMC
XTE J1550-564 (1998 ouburst) Index vs Luminosity
On the behavior of RMS spectrum
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm €
F(v) = (1− fC )B(v) + fC ⋅ B(v')0
∞
∫ C(v ',v)dv'
LHS HIMS
€
C = Cthermal
€
C = Cthermal + CBMC
Thermal Comtonization is variable, BM Comptonization is not!
Correlation scaling: BH mass estimate
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
Scaling Laws GX 339-4 vs XTE J1752-223 GRO J1655-40 vs XTE J1752-223
sv = 0.88 sn=0.41GX 339-4:
M=12.5 M ,d=5.7 kpc (S & Titarchuk 2009)
M1752≅11M d≅3.5 kpc
S & Titarchuk 2009, ApJ
sv = 1.5 sn=0.96GRO J1655-40:
M=12.5 M, d=5.7 kpc (Hjellming & Rupen 1995)M1752≅9.5M d≅3.8
kpc
MAXI J1659-152
4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank, Markwardt &Krimm
Evolution Index – QPO Frequency during the rise episode
sv = 1.62 +/- 0.04GX 339-4:
M=12.5 M ,d=5.7 kpc (S & Titarchuk 2009)
M1659≅20+/-3 M
Hardness-Intensity Diagram
SUMMARY • On October 21 RXTE discovered a new X-ray transient source
XTE J1752-223• Spectral and variability properties and the evolutionary
pattern are consistent with other Galactic BH candidates• XTE J1752-223 exhibited a uniquely stable prolonged low-
hard state• RXTE data allows spectral, timing analysis and Fourier
resolved spectroscopy revealing a new phenomenology. This helps to identify sources of different types of variability (noise, QPOs). QPO seems to be produced in the Compton Corona.
• Bulk Motion Comptonization in the converging flow provides a very promising framework for explaining different observational aspects of accreting BHs
• We estimated BH masses in XTE J1752-223 and MAXI J1659-152 of about 10 and 20 solar masses correspondingly
• The presented results are entirely due to unique RXTE capabilities, large collection area, high time and moderate spectral resolution and unmatched monitoring capabilities.
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
4th MAXI Workshop 2010, Tokyo, November 29, 2010Shaposhnikov, Swank, Markwardt &Krimm
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