Recoiled Black Holes in Galaxy Mergers: Gravitational Wave Emission Study

1. Accretion wake of recoiled black holes Roya Mohayaee CNRS, Institut d’Astrophysique de Paris Jacques Colin Observatoire de la Côte d’Azur, Nice Joe Silk University of Oxford astro-ph/07093321 J-P Lasota conference,Wroclaw 2007

2. Galaxy (black hole) mergers BHs at the centre of many galaxies Galaxy mergers BH mergers Emission of gravitational waves HST : colliding galaxies in Canis Major NGC 2207 –IC 2163 formation of a new centralBH

3. Black hole & dark matter Initially : initial ~ r- Adiabatic accretion: ffinal(Efinal,Lfinal) = finitial(Einitial,Linitial)

4. Black hole & dark matter (Young 1980, Gondolo & Silk 1999) Without BH : initial ~ r- With BH : final ~ r-(9-2)/(4-)

5. Absolute luminosity (L) of BH in -rays  +   L =luminosity factorx ∫2 dV /s luminosity factor =[N<v>/m2]c4/cm 3/s/Gev2 For M31: Fornasa et al 2007

6. Galaxy (black hole) mergers BHs at the centre of many galaxies Galaxy mergers BH mergers Emission of gravitational waves HST : colliding galaxies in Canis Major NGC 2207 –IC 2163 If isotropic formation of a new centralBH

7. Galaxy (black hole) mergers BHs at the centre of many galaxies Galaxy mergers BH mergers Emission of gravitational waves HST : colliding galaxies in Canis Major NGC 2207 –IC 2163 If isotropic If anisotropic Ejection of the BH From the galaxy formation of a new centralBH

8. Ejection of a black hole during galaxies mergers

9. Ejection of a black hole during galaxies mergers Spin=zero X=0.38

10. Ejection of a black hole during galaxies mergers spin ≠ 0 recoil velocity 4000 km/s Campanelli et al 2007

11. Orbit of an ejected BH high  V~0 low  high v Virial radius

12. Density profile of the accretion wake • Cold medium >Bondi-Hoyle accretion (1944) • Two-body problem +mass conservation  V r  (q) dq  (x) dx=(q) dq

13. Density profile of the accretion wake hot medium (e.g. Maxwellian velocity distribution) > Danby & Camm (1957)  V Jean’s theorem numerical solution for density Analytic solution for stationary BHs : (r)~ 1/√r

14. Wake density : radius of influence

15. Wake density : hot versus cold medium Hot environment 

16. Wake density : hot versus cold medium Hot environment Cold environment  

17. Constant density contours : large

18. Constant density contours : reducing 

19. Wake density contours Wake density contours,small 

20. Highest density at the apapsis passage high  V~0 low  high v Virial radius

21. Time to reach the apapsis Initial velocity of BH / escape velocity

22. Absolute luminosity of a recoiled BH in -rays L(M,z) = [N<v>/m2] ∫2 dV /s L= 1025 (1+z)4 (M/Mo) R2cutoff /s LBH /Lhost galaxy

23. Diffused -ray background

24. BH Mass function Press & Schechter (1974) Density peaks in initially random gaussian field collapse to form ‘‘galaxies’’ Number density of galaxies of mass M at redsift z N(M,z)

25. Diffused -ray background =H0 ∫∫t(M,z) L(M,z) N(M,z) dM dr(z) Time the BH spends at apapsis Press-Schechter mass function 1025 (1+z)4 (M/Mo) R2cutofff/s

26. Time spent at apapsis =H0 ∫∫ t(M,z) L(M,z) N(M,z) dM dr(z)

27. Future Prospects: Confronting the observations  > 10 -8  cm-2 s-1 sr-1

28. Future Prospects: Confronting the observations  > 10 -8  cm-2 s-1 sr-1  cm-2 s-1 sr-1 EGRET 10-7 GLAST 10-8 10-9 10-10 10-11 MAGIC 10-12 HESS, VERITAS