terry walker fcp05

Cosmology and AstrophysicsFCP05: 

Cosmology and Astrophysics FCP05 Beacom(OSU), Hodges(UW), Abu-Zayyad(Utah), Yuksel(UW), Strigari (OSU), Collins (UMass), Kadota (FNAL), Bean (Princeton), Fry (UFL), Ralston (KU), Teegarden (NASA/Goddard), Bell (CalTech), Mirabolfathi (UCB), Shutt (Case), Duffy (UFL), Beatty (OSU), Ritz (NASA/Goddard), Zentner (Chicago), Sinnis(LANL) TPW Vanderbilt 5/28/05

Cosmology/Astrophysics TopicsFrontiers in Contemporary Physics-III: 

Cosmology/Astrophysics Topics Frontiers in Contemporary Physics-III n Astrophysics (10 MeV - Joule) ICECUBE/ANITA g-ray Astrophysics (10 GeV - TeV) MILAGRO/GLAST/HESS UHECR Astrophysics (Joule) HIRES/AUGER Dark Matter CDMS/XENON/ADMX Dark Energy DES/LSST/JDEM

Three Neutrino Frontiers: 

Three Neutrino Frontiers The Neutrino Universe Awaits Us J.Beacom (OSU)

The Future of Solar n’sT.Shutt (Case): 

The Future of Solar n’s T.Shutt (Case) Last 40 years: 8B ne oscillate in matter (LMA) (msw-to-vacuum transition cross-check) 7Be ne flux basically unmeasured The Future: Borexino (KamLAND)

Supernova neutrinos: 

Supernova neutrinos

Slide6: 

Diffuse Supernova Neutrino Background L.Strigari (OSU/UCI) Recent DSNB predictions: ~ 3 events/yr above 18 MeV ~ 6 events/yr above 10 MeV Ando, Sato & Totani 2003 Fukugita & Kawasaki 2003 Strigari, Kaplinghat, Steigman & Walker 2004 Atmospheric Background Reduction Beacom & Vagins 2004

Slide7: 

Cosmic Star Formation Rate UV luminosity density > ~ 8 Solar Mass SDSS and 2dF galaxy surveys > ~ 1 Solar Mass Diffuse Supernova Neutrino Background > ~ 8 Solar Mass Excludes allowed astronomical models Concordance Region Strigari, Beacom, Walker, Zhang, JCAP04(2005)017

Slide8: 

Supernova Neutrinos from a Few Mpc

TeV Neutrinos AGNs as the ultimate beam dump : 

TeV Neutrinos AGNs as the ultimate beam dump

Milagro: A Tera-Volt Astrophysical Observatory G.Sinnis (LANL): 

Milagro: A Tera-Volt Astrophysical Observatory G.Sinnis (LANL) Physics Goals Particle acceleration Astrophysical shocks Black hole environments Neutron star environments Gamma-ray bursts Solar physics Space weather Open aperture/continuous observation Monitoring of variable sources Study large-scale structure of sources Discovery potential Milagro’s detection of 20 Jan 2005 solar flare particles > 10 GeV with <1 minute risetime Milagro’s flux of g-rays (red cross) from the Galactic plane--likely due to cosmic-ray production of po -> g + g Milagro’s observation of ~ 6o Ø source in the Cygnus region of our galaxy.

ICECUBEJ.Hodges(UW): 

ICECUBE J.Hodges(UW) AMANDA II (9 additional strings) is no ICECUBE As a proof of concept, AMANDA has not seen any statistically significant n background, pointsources, or GRB-correlated signal ICECUBE is the future.

Slide12: 

Preliminary Preliminary Muon Neutrino Flux Limits

GZK NeutrinosCollisions of the Universe’s highest and lowest energy particles: 

GZK Neutrinos Collisions of the Universe’s highest and lowest energy particles

Slide14: 

cosmic rays Messengers of the Extreme Universe: Cosmic Rays Neutrinos Halzen, Ressell & Turner n Energy (eV) e+e-

HiRes (EAS fluorescence) Abu-Zayyad (Utah): 

HiRes (EAS fluorescence) Abu-Zayyad (Utah) Monocular v. Stereo Second monocular spectrum consistent with first (i.e. still no super-GZK events) Preliminary stereo spectrum has 400 events above 1019 GeV Stay tuned ICRC 8/2005

Future Neutrino Sensitivity: 

Future Neutrino Sensitivity Semikoz, Sigl, hep-ph/0309328

Anita-lite & other limits & projections  J.Beatty(OSU): 

Anita-lite & other limits & projections J.Beatty(OSU) ANITA-lite: 18.4 days of data, net 40% livetime with 60% analysis efficiency for detection Ice coverage & average depths included No candidates survive impulse cuts in 2 independent analyses Z-burst model (nn annihilation --> UHECR) strongly excluded: we expect 20-30 events, see none Large extra dimensions: No limit yet MC modeling is more complicated than expected ANITA projected sensitivity: ne nm nt included, full-mixing assumed 1.5-2.5 orders of magnitude gain! RICE limits for 3500 hours livetime in embedded South Pole array GLUE limits ~120 hours livetime, Lunar regolith observations FORTE limits on 3 days of satellite observations of Greenland ice sheet Preliminary

ANITA’s science reach: 

ANITA’s science reach

Dark Matter: 

Dark Matter

GLAST: 

GLAST

Electron-Positron Annihilation Radiation (511 keV) Teegarden(NASA/Goddard): 

Electron-Positron Annihilation Radiation (511 keV) Teegarden(NASA/Goddard) Bulge distribution Data are reasonably well fit by symmetric gaussian with FWHM = 8° ± 1° No evidence for OSSE “fountain” Ensemble of point sources cannot be ruled out Concentration of flux at GC suggests older population.

Slide22: 

Tree level process must be accompanied by the radiative correction Detectable photons emitted via “Internal Bremsstrahlung” processs. Can positrons really be produced INVISIBLY? N.Bell (CalTech)

Slide23: 

Bremsstrahlung Spectrum & COMPTEL/EGRET constraints Maximum permitted contribution of internal bremsstrahlung photons

XENONT.Shutt (Case): 

XENON T.Shutt (Case) Size matters Liquid Xe could be competitive with Ge at low recoil (< 20 keV) 10 tons required to get to most MSSM LSPs Xe isotopes probe spin-dependent s Prototype stage is encouraging

ADMX: 

ADMX P ~ gg2rama L.Duffy (UFL)

The CDM Paradigm M.Kaplinghat (UCI): 

The CDM Paradigm M.Kaplinghat (UCI) Cosmology constraints Free-streaming cut-off Phase space limited Adequate reionization Non-linear small scale structure [Charged-NLSP+g+baryon fluid] [CMB black body] [BBN] Probes: BBN, CMB, CMB lensing, Weak lensing, Reionization, 21 cm, Ly-a forest, … Rich phenomenology (cosmology) of dark matter from decays with a lifetime of order a month.

Satellites & The Power Spectrum A.Zenter (Chicago): 

Satellites & The Power Spectrum A.Zenter (Chicago) A WMAP-like PS helps alleviate the subhalo “number crisis” because subs are fewer and less dense (ARZ & Bullock PRD 2002, ApJ 2004) Can more easily accommodate a “sharp” transition between light and dark halos implied by some feedback scenarios (Shaviv & Dekel 2003; Bullock et al. 2001; Benson et al. 2002) rms density fluctuation Mass scale  (length scale)1/3

Slide29: 

If Mx  100 GeV or less, N ~ 1 detectable subhalos per GLAST field of view, need a  500 hour exposure with VERITAS to detect the line emission. If Mx > 100GeV any detection must rely on serendipitous discovery The observability of the Milky Way substructure Detection schemes: Mx < 50 GeV GLAST 50 GeV < Mx < 100 GeV GLAST + VERITAS Mx > 100 GeV VERITAS Koushiappas, ARZ, & Walker 2004; ARZ, Koushiappas, & Kazantzidis 2005 Confirmed by Pieri et al. 2005 result

Dark Energy: 

Dark Energy

Acceleration from superhorizon pertubations?No – acts as neglible curvature and then dust J.Fry (UFL): 

Acceleration from superhorizon pertubations? No – acts as neglible curvature and then dust J.Fry (UFL) ``I think Rocky was wrong when he said `We think Einstein was right we he said he was wrong’.’’ T. Weiler FCP05

J.Ralston (KU): Naughty Virgo. Evidence for a preferred direction in space?: 

J.Ralston (KU): Naughty Virgo. Evidence for a preferred direction in space? Impossible for the null to verify the data: symmetries have been broken Statistical significance is quite high The physical mechanism for these duality-violating correlations is unknown Hutsemekers has just doubled his data; the effect is getting more serious

Slide36: 

Constraining V(f) with the CMB K. Kadota (FNAL)

The trans-Planckian signals H.Collins (UMass): 

The CMB spectrum observed today is the product of initial state effects and their evolution the initial state effects are generically more sensitive to physics at some scale M above the expansion rate during inflation H A variety of ad hoc models estimate that these ‘trans-Planckian’ effects appear as H ⁄ M corrections to the power spectrum The primordial power spectrum is currently measured to about a 1% accuracy, but this should eventually improve by a factor of 103 In hep-th/0501158, we develop an effective theory description of these initial state effects initial state structure appears in propagator new divergences appear at one loop order We show that this description is consistent by renormalizing the theory at the initial time trans-Planckian signals correspond to irrelevant boundary counterterms obtain an RG-flow for the initial conditions The trans-Planckian signals H.Collins (UMass) … and effective initial conditions 10–2 observable now, 10–6 observable eventually NASA/WMAP Science Team

Cosmology/Astrophysics TopicsFrontiers in Contemporary Physics-III: 

Cosmology/Astrophysics Topics Frontiers in Contemporary Physics-III n Astrophysics (10 MeV - Joule) ICECUBE/ANITA g-ray Astrophysics (10 GeV - TeV) MILAGRO/GLAST/HESS UHECR Astrophysics (Joule) HIRES/AUGER Dark Matter CDMS/XENON/ADMX Dark Energy DES/LSST/JDEM The age of ultrahigh energy astronomy is upon us

Fine’: 

Fine’ Beacom(OSU) Hodges(UW) Abu-Zayyad(Utah) Yuksel(UW), Strigari (OSU) Collins (UMass) Kadota (FNAL) Bean (Princeton) Fry (UFL) Ralston (KU) Teegarden (NASA/Goddard) Bell (CalTech), Mirabolfathi (UCB) Shutt (Case) Duffy (UFL) Beatty (OSU) Ritz (NASA/Goddard) Zentner (Chicago) Sinnis(LANL) TPW Vanderbilt 5/28/05