` Крупномасштабная структура ближней Вселенной по данным обсерватории ИНТЕГРАЛ Р. Кривонос, М. Ревнивцев, А.Лутовинов С.Сазонов, Е.Чуразов, Р. Сюняев ИКИ. - презентация

1 ` Крупномасштабная структура ближней Вселенной по данным обсерватории ИНТЕГРАЛ Р. Кривонос, М. Ревнивцев, А.Лутовинов С.Сазонов, Е.Чуразов, Р. Сюняев ИКИ РАН, Москва / MPA, Garching

2 Обзор всего неба кэВ Обнаружено 403 источника на всем небе 217 галактических, 137 внегалактических 49 неизвестной природы 12% sky – 1 mCrab 80% sky – 5 mCrab Эффективная глубина обзора Мпк для источника со светимостью эрг/с

3 500 Mpc Large Scale Structure of the Local Universe 100 Mpc

4 Local Group Large Scale Structure of the Local Universe Peebles, 1993 Kraan-Korteweg & Lahav, Sci. Am D < 40 Мпк 40 < D < 80 Мпк

5 268 o 27 o NP AGN surface density contrast 11:1

6 AGN volume density (D erg/s 40 AGNs

7 Virgo Hydra Centaurus Pavo Perseus n = 1.4 x / Mpc 3, L > erg/s 40 AGNs AGN volume density (D

8 ~5,000 IR galaxies: (IRAS PSCz survey) Volume density excess of nearby (

9 X-Ray AGN bias factor We use IRAS PSCz survey as matter tracer ( b IR1 ) b=

10 X-Ray AGN bias factor => AGNs – good matter tracers on Mpc scale => SMBH activity independent from density of galaxies b AGN = 0.80 ± 0.13 b AGN = 1.0

11 HEAO1 A2 Survey INTEGRAL survey Historic remark: HEAO 1 / A2 survey Piccinotti et al Krivonos et. al. 2007

12 Космические лучи сверхвысоких энергий

13 Summary => Already now INTEGRAL is able to probe Large Scale Structure of the local Universe => Density fluctuations of matter can be linearly translated into the density fluctuation of Hard X-ray emitting AGNs at zero redshift. => SMBH activity independent from density of galaxies on scales Mpc

14 Galactic and extragalactic source counts ASCA, Sugizaki et al., (2001) INTEGRAL gal. Sources |b|

15 Survey Sensitivity: 12% sky – 1 mCrab 80% sky – 5 mCrab Effective depth of the survey Mpc for a source with typical luminosity 10^43 erg/s Coded-mask based telescope IBIS: FOV 30х30 degrees. Angular resolution 12 Detector ISGRI: Survey energy range keV 1 mCrab = 1.4 х erg/s/cm 2 All-sky survey / keV

16 IRAS PSCz Redshift Survey n = 1.4 x / Mpc 3, L > erg/s 40 AGNs 15,000 gal. AGN volume density (D

17 Nearby Active Galactic Nuclei (|b|>5) 66 non-blazar AGNs 3 clusters of galaxies

18 Luminosity Function 1) Volume density (L>10 42 ) 2 x / Mpc 3 2) Volume emissivity (L>10 41 ) 12 х erg/s/ Mpc 3 Consistent with: Beckmann et al keV LF (smaller INTEGRAL sample) RXTE Slew Survey 3-20 keV LF (Sazonov & Revnivtsev 2004) HEAO keV LF (Shinozaki et al. 2006)

19 N( F > 1 mCrab)=M F -a a = 1.62 ± 0.15 M = (5.7 ± 0.7) / deg keV, |b|>5 o, z < 0.1 Extragalactic source counts Most of the unidentified sources in the Galactic Plane should be of Galactic origin ~1% CXB Expected Measured