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Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223 Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223.

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Presentation on theme: "Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223 Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223."— Presentation transcript:

1 Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223 Discovery and Evolution of a New Galactic Black Hole Candidate XTE J1752-223 N. Shaposhnikov 1,2,3, J. Swank 3, C. Markwardt 1,2,3, H. Krimm 2,3,4 The Astrophysical Journal, 723, 2,1817 1 University of Maryland, Astronomy Department 2 Center for Research and Exploration in Space Science & Technology (CRESST) 3 NASA/Goddrd Space Flight Center 4 Universities Space Research Association 4 th MAXI Workshop 2010, Tokyo, November 29, 2010

2 Discovery XTE 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 N H =0.47×10 22 cm -2 (Atel #2261) 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 N H =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

3 XTE J1752-223 Evolution XTE J1752-223 Evolution 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 Hardness – Intensity Diagram

4 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 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 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,2010

5 XTE J1752-223 Variability Evolution 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 LHS HIMSSIMSHSS ISLHS

6 Low Hard State in XTE J1752-223 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 XTE J1752-223 GX 339-4 Power Spectra

7 Fourier Resolved Spectroscopy (FRS) 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 XTE J1752-223 Low Hard State GX 339-4

8 Fourier Resolved Spectroscopy (continued) 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 State Transition HIMSSIMS 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.

9 Fourier Resolved Spectroscopy (HIMS) 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 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!).

10 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)

11 Thermal versus Bulk motion Comptonization 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 (S & Titarchuk 2010) XTE J1550-564 Thermal BMC High Energy Cutoff Evolution Thermal BMC XTE J1550-564 (1998 ouburst) Index vs Luminosity

12 On the Nature of the Extreme LHS 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 Power SpectrumEnergy 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 the X- ray forming region and the response to the modulation is the same for all energies

13 On the behavior of RMS spectrum 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 LHS HIMS Thermal Comtonization is variable, BM Comptonization is not!

14 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) M 1752 ≅ 9.5M  d ≅ 3.8 kpc

15 MAXI J1659-152 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 EvolutionIndex – 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) M 1659 ≅ 20+/-3 M  Hardness-Intensity Diagram

16 SUMMARYSUMMARY 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 4 th MAXI Workshop 2010, Tokyo, November 29, 2010 Shaposhnikov, Swank, Markwardt &Krimm

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