New Galactic Black Hole Candidate XTE J1752223 N Shaposhnikov 123 J Swank 3 C Markwardt 123 H Krimm 234 The Astrophysical Journal 723 21817 1 University of Maryland Astronomy Department ID: 490176
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Slide1
Discovery and Evolution of aNew Galactic Black Hole CandidateXTE J1752-223
N. Shaposhnikov1,2,3, J. Swank3, C. Markwardt1,2,3, H. Krimm2,3,4The Astrophysical Journal, 723, 2,1817
1
University of Maryland, Astronomy Department
2
Center for Research and Exploration in Space Science & Technology (CRESST)
3NASA/Goddrd Space Flight Center4Universities Space Research Association
4
th
MAXI Workshop
2010,
Tokyo, November 29,
2010Slide2
Discovery
XTE J1752-223RXTE/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 =0.47×10
22 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
4
th
MAXI Workshop 2010, Tokyo, November 29, 2010
Shaposhnikov, Swank,
Markwardt
&
Krimm
Slide3
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 Slide4
Data modeling:
Energy spectral modelComptonization (BMC)Gaussian for the iron line at ~6.5 keVModified by interstellar absorption (measured by Swift/XRT)High energy cutoff
Power Density SpectraPower law or broken power law for the broad band variability
Loretzians for
QPOs
RXTE
Data Spectral Analysis
4
th
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,2010Slide5
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
I
S
LHSSlide6
Low Hard State in XTE J1752-2234th
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 SpectraSlide7
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 State
GX 339-4Slide8
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
S
IMS
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.
Slide9
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!).Slide10
What can we learn from spectral data?Nature of the power
law
E
-
Thermal
Comptonization
:
,
(
Rubicki
&
Lightman
, 79)
Bulk Motion
Comptonization
:
(S
&
Titarchuk
, 2009)
4
th
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)Slide11
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
LuminositySlide12
On the Nature of the Extreme LHS4th MAXI Workshop 2010, Tokyo, November 29, 2010
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223
Shaposhnikov, Swank,
Markwardt
&Krimm
Power Spectrum
Energy Spectrum
Generic
Comptonization
(BMC XSPEC model)
f
c
–
Comptonized
fraction
C(v’,v
) – Green’s function
B(v
) – black body
Perturbation propagation in a bounded medium:
t
*
- perturbation diffusion time
PDS response to an exponential shot:
(
Lyubarskii,1997
)
(
Titarchuk
, S &
Arefiev
, 2007)
RMS
Spectrum
Source of modulation is located outside t
he X-ray forming region and the
response to the modulation is the same for all energies
Slide13
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
LHS
HIMS
Thermal
Comtonization
is variable, BM
Comptonization
is not!Slide14
Correlation scaling: BH mass estimate
4
th
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
s
v
= 0.88
s
n
=0.41
GX 339-4: M=12.5 M ,d=5.7 kpc (S &
Titarchuk
2009)
M
1752
≅11M
d
≅3.5
kpc
S &
Titarchuk
2009,
ApJ
s
v
= 1.5
s
n
=0.96
GRO J1655-40:
M=12.5 M
,
d
=5.7
kpc
(
Hjellming
&
Rupen
1995)
M1752≅9.5M d≅3.8 kpcSlide15
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
s
v
=
1.62 +/- 0.04
GX 339-4:
M=12.5 M
,
d
=5.7
kpc
(S &
Titarchuk 2009)M1659≅20+/-3 M
Hardness-Intensity DiagramSlide16
SUMMARY
On October 21 RXTE discovered a new X-ray transient source XTE J1752-223Spectral 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 s
ources 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 BHsWe 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
4
th
MAXI Workshop 2010, Tokyo, November 29, 2010
Shaposhnikov, Swank,
Markwardt
&
Krimm