the 7-year view of the accreting x-ray binaries with integral
DESCRIPTION
The 7-year view of the accreting X-ray binaries with INTEGRAL. R.Krivonos, M.Revnivtsev, S.Tsygankov, E.Churazov, R.Sunyaev MPA Garching, Germany; IKI, Moscow, Russia. Galactic Center region, 20 Ms, 17-60 keV. Limiting flux ~0.26 mCrab 3.7e-12 erg/s/cm 2 - PowerPoint PPT PresentationTRANSCRIPT
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The 7-year view of the accreting X-ray binaries with INTEGRAL
R.Krivonos, M.Revnivtsev,S.Tsygankov, E.Churazov, R.Sunyaev
MPA Garching, Germany; IKI, Moscow, Russia
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Galactic Center region, 20 Ms, 17-60 keV
Limiting flux ~0.26 mCrab 3.7e-12 erg/s/cm2
Luminosity 4e+34 erg/s at the distance of GC
The Milky Way is a unique galaxy where we can detect X-ray objects with the lowest possible luminosities.
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Stellar density field
Galactic Center region, 20 Ms, 17-60 keV
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Low-Massive X-ray Binaries in Bulge
Revnivtsev et al., 2008
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Low-Massive X-ray Binaries in Bulge
d log N / d log L = -0.96 +/- 0.20 at log(L) < 37
Break in dM/dT distribution?
Change in Lx – dM/dT relation?
Recent: the break is due to different classes of companion stars:
Gilfanov 2004
Revnivtsev et al., 2010
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Galactic ridge X-ray emission with INTEGRAL
It is shown that the Ridge is due to point sources at energies <10 keV (Revnivtsev et al. 2006, 2007, 2008, 2009)`
What is in hard X-rays?
Cataclysmic Variables: first approach
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INTEGRAL view of the GRXE
NIR contours
Krivonos et al. 2006, 2009
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Galactic ridgeemission in hardX-rays consists ofemission of millionsof CVs!
Shape of cutoffaverage mass of WDs
<Mwd>~0.5-0.6 Msun
INTEGRALRXTE
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The dominant class of INTEGRAL CV is intermediate polars
Revnivtsev et al., 2008
INTEGRAL provides one of the largest unbiased sample of luminous intermediate polars existing today (37 in the 7-year survey)
The survey is serendipitous with respect to CVs
Cataclysmic Variables
INTEGRAL
Cataclysmic Variables: second approach
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Cataclysmic Variables
Scale height of Galactic disk population is 130 (+90-50) kpc
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Luminosity function of hard X-ray emitting CVs only from INTEGRAL all sky survey!
Revnivtsev et al. 2008
Cumulative emissivity of CVs
in 17-60 keV
Ridge value in 17-60 keV
INTEGRALpoints
RXTE points
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Revnivtsev et al. 2008
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Density of HMXBs In the Galactic plane
INTEGRAL surveySimple toy model
Lutovinov et al. 2005, 2007
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The position of spiral arms(ignored)
Shtykovskiy & Gilfanov 2007
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Method:Integrate the galactic disk model with a given luminosity function, given survey sensitivity map, and measure the probability to have the observed distribution of sources.
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-- measured-- not ID-- predicted
High-Massive X-ray Binaries distribution over the Galactic longitude
Crux Carina
Norma
Cyg
Sgr
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Disk without hole
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r_disk = 2.2 (+0.6-0.4) kpc
Disk size
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dN/dL ~L
Probing the LF (single) slope over Log(L) 33-38
-Gamma
Gamma = 1.3 (+0.3-0.2)Voss & Ajello 2010
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Maximum Likelihood HMXB Luminosity Function
delta Likelihood < 1.0
Log
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Unrealistic LF shape:Overprediction at low luminosities
Log
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Unrealistic LF shape:Underprediction at low luminosities
Like “Propeller effect”
Log
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dN/dL~L^1.5Absolutely unrealistic LF shape:
Log
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The perfect sky imaging with IBIS/ISGRI is possible:
IKI/RSDC http://hea.iki.rssi.ru/integral
MPA http://www.mpa-garching.mpg.de/integral
Concluding remarks (1)
• 7-year Galactic Bulge Map• Galactic Plane Survey • Galactic Bulge Monitoring• Catalog of sources with spectra and lightcurves
INTEGRAL/IBIS 7-year All-Sky Hard X-Ray Survey. Part I: Image Reconstruction A&A (arXiv:1006.2463)
INTEGRAL/IBIS 7-year All-Sky Hard X-Ray Survey. Part II: Catalog of Sources A&A (arXiv:1006.4437)
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Flat end of luminosity function at Log (L) < 37
The cumulative angular distribution in the Galactic center region traces the cumulative number of stars (bulge and nuclear stellar disk components)
Concluding remarks (2)LMXB in Bulge
=> Break in dM/dT distribution?
=> Change in Lx – dM/dT relation?
=> Different classes of companions
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The scale height of the Galactic disk 130 (+90-50) kpc
Luminosity Function
Luminosity density is consistent with that measured from unresolved emission (“Rigde”)
Concluding remarks (3)Cataclysmic Variables
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Spatial distribution of HMXB allows one to constrain lower and upper limits for luminosity function regardless distance information
Probe of flattening at Log (L) < 34 “Propeller effect”
Concluding remarks (4)HMXB