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Рентгеновские галактические двойные в жестких лучах

A .Лутовинов , M. Ревнивцев , M. Гильфанов , Р.Кривонос, П.Штыковский, Р . Сюняев Институт Косм ических Исследований РАН , Москва Max-Plank Institute for Astrophysics, Garching E-mail: aal@hea.iki.rssi.ru. Рентгеновские галактические двойные в жестких лучах. LMXBs and HMXBs with compact

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Рентгеновские галактические двойные в жестких лучах

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  1. A.Лутовинов, M.Ревнивцев, M.Гильфанов, Р.Кривонос, П.Штыковский,Р.Сюняев Институт Косм ических Исследований РАН, Москва Max-Plank Institute for Astrophysics, Garching E-mail: aal@hea.iki.rssi.ru Рентгеновские галактические двойные в жестких лучах

  2. LMXBs and HMXBs with compact objects are the brightnest X-ray emitters in the Galaxy Their properties intimately depends on properties of stars in the Galaxy: 1) Spatial distribution <- SFR or mass density 2) Luminosity function <- evolution of binaries 3) Spectra <- physical properties around stars X-ray binaries – nice tool to explore the Galaxy Grimm et al. 2002

  3. 1) Compact X-ray sources in binaries HMXB • young population (x107 yr) • Mc > 10 Msun • type: late O–B(e) classes • strong stellar wind • intrinsic absorption • trace the SF regions • Vela X-1, 4U1700-37, GX301-2, Cyg X-1, most X-ray pulsars LMXB • old population (~109 yr) • Mc ~ 1 Msun • type: K – M classes • no stellar wind • no intrinsic absorption • trace stellar mass • 1E1740-294, GRS1915+105, X-ray bursters Different properties, different spectra, different spatial distributions

  4. 2) Spectra: A lot of HMXBs have high photoabsorption High energy range and imaging (INTEGRAL) is crucial! Properties of significant part of new sources: strong intrinsic photoabsorption; harboring NS; most part are X-ary pulsars; Lutovinov et al. 2005

  5. Spectra: X-ray pulsars with INTEGRAL 35 X-ray pulsars were investigated in total, spectra of 8 of them were obtained in a first time. No obvious correlations between sources spectral parameters The shapes of spectra of many new strongly absorbed sources are very similar to spectra of X-ray pulsars (see Fig.). Filippova et al. 2005

  6. 3) The Galaxy inner part • Energy band: 20-60 keV -> no absorption! • Flux limited sample (1.5 mCrab) • Totally detected 90 sources: 49 LMXB, 23 HMXB, 2 AGN, SNRs and single pulsars, 10 – unidentified Lutovinov et al. (2005)

  7. List of detected HMXB Criteria of HMXB: 1) optical identification 2) pulsations 3) strong intrinsic absorption

  8. Distribution of the absorption column value observed in X-ray spectra of HMXB Number-flux function of HMXB, obtained with INTEGRAL. Dashed line represents a shape of this function obtained by Grimm et al. (2002) with Г=0.64 19 of 23 HMXB sources have high (>5x1022 cm-2) intrinsic absorption

  9. 4) The whole Galaxy with INTEGRAL • Energy band: 20-60keV • 403 sources in total • Near the Galactic plane (|b|<5) - 228 sources (|b|<2) - 143 sources Total exposure > 30 Msec New sources (IGRJ…) ~ 150

  10. Number of detected sources Galaxy Total 403 sources HMXB 74 sources LMXB 87 sources Krivonos et al. (2007) Galactic plane (b<|5|, LMXB scale) Total 228 sources HMXB 50 sources (only 3BHC!, 32 X-ray pulsars) LMXB 55 sources Galactic plane (b<|2|, HMXB scale) Total 143 sources HMXB 41 sources (1BHC, 23 X-ray pulsars) LMXB 33 sources

  11. 5) Angular distributions of sources Sgr+Sc Crux Norm+Per Carina Cyg Magenta line – all sources Red line – LMXB/2 (concentrated to Galactic center) blue line – HMXB (concentrated to spiral galactic arms) KS-test: HMXB vs uniform > 99.9% HMXB vs LMXB > 99.9%

  12. 6) Disc and arms components of the Galaxy White arrows show the expected directions of the enhanced number of HMXBs. Very similar to the observed picture! Bahcall & Soneira (1980) Density of distributions of HMXB and LMXB Grimm et al. (2002)

  13. 7) HMXB distribution (face-on view) The inner part of Galaxy The whole Galaxy Lutovinov et al. 2005 Lutovinov et al. (2007) HMXB peaked away of the Galactic Center and concentrated towards the spiral arms, but not one-to one

  14. Conclusions and future work 1. INTEGRAL increased sample of Galactic HMXB; reasons – large sky coverage and absorbed sources 2. Majority of HMXB are significantly photoabsorbed; spectra most of them very like to spectra of X-ray pulsars; 3. HMXB are concentrated towards spiral arms, LMXB – to the Galactic Center; subtle details are not clear now. 4. Spatial distribution. Measurements of spiral arms in further part of the Galaxy – needs identifications of more sources and distance measurements

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