1. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006  Supernovae as neutrino and gravitational wave sources Cosmological Backgrounds of Neutrinos, Photons, And Gravitational Waves Günter Sigl GReCO, Institut d’Astrophysique de Paris, CNRS et Fédération de Recherche Astroparticule et Cosmologie, Université Paris 7 http://www2.iap.fr/users/sigl/homepage.html

2. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Onion structure of a supernova Convection, turbulence Janka, Mueller

3. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Supernovae as Neutrino and Gravitational Wave Sources Anisotropic mass motion and neutrino emission in massive star collapse leads to gravitational wave emission. At low frequencies neutrino emission with luminosity L ν (t) and anisotropy q(t) dominates and leads to dimensionless strain at distance D: L(t) memory h(t) q(t) A rotating core collapse model by Müller & Janka

4. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 neutrino spectra gravitational wave spectra Simulated individual signals ordinary SN ≥100M sun PopIII Individual supernovae (SN) in our Galaxy can give prominent signals in neutrinos in Super-Kamiokande, Amanda, ICECUBE, Uno… and in gravitational waves in Virgo/EGO, LIGO…, but are RARE events. 2x10 -3 M sun in gw, ~3% 10 -8 M sun in gw, ~0.5%

5. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 The background is then given by integration over all events The Gaussianity of the signal is given by the “duty factor” which is proportional to the event rate: Where τ(f) is the time scale over which frequency f is emitted “coherently” In a given event. For us: τ(f)~1/f

6. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Ordinary SN ~ 1/sec + very massive PopIII stars at z ≥ 15 with rate ~ 0.2 (f III /10 -3 )/sec, where f III = baryon fraction cycled thru PopIII stars. future input from SWIFT … However, backgrounds from cosmological SN may soon be detectable by gadolinium upgrade of Super-K in neutrinos and by gravitational wave detectors such as the Big Bang Observatory (BBO). SN rate

7. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 => diffuse neutrino spectra from ordinary SN close to current sensitivities stochastic gravitational wave background Ando and Sato, astro-ph/0410061Buonanno, Sigl, Raffelt, Janka, Mueller, Phys.Rev.D 72 (2005) 084001

8. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Diffuse infrared background can not be explained by galaxies alone -> may need a Pop III contribution Dwek et al., astro-ph/0508262 Pop III fraction of baryons f III and infrared background resulting from Lyα emission Madau, Silk., astro-ph/0502304

9. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Fate of a massive star as function of progenitor mass and metallicity low metallicity: less cooling, larger progenitor masses, less mass loss, more powerful explosions. Heger et al., astro-ph/0211062

10. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Fate of a massive star as function of progenitor mass and metallicity Heger et al., astro-ph/0211062

11. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Compare this with upper limits, sensitivities, and cosmological predictions Giovannini BBO BBO correlated SN and PopIII

12. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Consequence: Gravitational Wave Background from type II supernovae and PopIII stars could mask inflationary background

13. Günter Sigl, Astroparticules et Cosmologie, ParisILIAS/N5-N6 meeting, Paris, January 23-24, 2006 Conclusions There is a deep connection between neutrino and gravitational wave emission by collapsing massive stars. Both signals have good chances to be seen by future experiments.