1. 113 vi 07DoE Program Review Kavli Institute for Particle Astrophysics and Cosmology Recent Results from KIPAC The Physics of GLAST June 13 2007 Roger D. Blandford

2. 213 vi 07DoE Program Review KIPAC - Projects and Proposals *KIPAC supports active projects –GLAST DoE, NASA; construction before KIPAC; science linked through KIPAC –CDMS DoE through campus - science connection –QUaD, SDO… NSF, NASA through campus - science connection –Suzaku, H.E.S.S. Individual involvement *KIPAC nurtures new proposals –LSST camera Lead role through DoE –SNAP Support role through DoE –EXO DoE through SLAC, campus, outside KIPAC; growing science connection –Con-X, CTA, NuSTAR, EXIST, LISA, NeXT, PoGO, Quiet,… NASA, NSF… though campus

3. 313 vi 07DoE Program Review KIPAC - non-SLAC Funding *KIPAC members non-SLAC DOE funding and non-DOE (NASA, NSF…) annual funding –~ $40M projects (SDO, GLAST, EXO, LIGO…) –~$1.5M CDMS –~$3M NASA, NSF grants (XMM-Newton, Observing, Theory, Exp. Astro, postocs…) *There will be sharp decrease in HEPL funding due to completion of SDO, HMI *Overall NASA science funding projected to decline –KIPAC members involved in all five “Beyond Einstein” topics being considered by BEPAC –KIPAC members have been very successful in NASA observing proposals –KIPAC has attracted 2 Hubble Fellows 4 Chandra Fellows and 1 Jansky Fellow –Most postdocs externally supported

4. 413 vi 07DoE Program Review KIPAC Physics *Particle Astrophysics –Black Holes, Neutron Stars, White Dwarfs… –GRBs, magnetars, supernovae… –Accretion disks and jets… –Relativistic shocks, particle acceleration, UHECR… –Solar Physics *Cosmology –Dark energy, dark matter –Gravitational lenses –Clusters of galaxies and intergalactic medium –Microwave background observations –First stars, galaxy formation –Supernovae

5. 513 vi 07DoE Program Review Madejski - A new Megamaser 3 x 10 6 M sun Black Hole

6. 613 vi 07DoE Program Review Hubble Constant - Sherry Suyu –HST KP (Freedman et al) =0.72+/-0.02+/-0.07 –Masers (Macri et al) h=0.74+/-0.03+/-0.06 –WMAP (Spergel et al) h=0.73+/-0.03 (F  CDM) –BAO (Eisenstein et al) h=0.69+/-0.02 (F  CDM) –Gravitational lenses =0.72+0.08-0.11 (Saha) =0.69+/-0.06+/-0.08 (Oguri)  S D h ~  t -1  2 O B1608+656 h=0.75+/-0.25+/-0.25

7. 713 vi 07DoE Program Review (Baltz)

8. 813 vi 07DoE Program Review Sarah Church - QUaD *CMB Polarization *Array of polarization sensitive bolometers at South Pole

9. 913 vi 07DoE Program Review Testing String Theory by CMB, A. Linde We clarified models in field theory and supergravity/string theory which predict B- modes or predict their absence. In particular, we have identified a class of models which predict a ratio of tensor to scalar perturbations r at and below the level of detection by BICEP and QUaD; Spider, SPUD, EBEX, polarBear, QUIET, Clover and Planck. This is of particular interest for CPTpol, ACTpol and CMBpol Possible values of r and n s in the theory Simplest field theory example Based on R. Kallosh, A. L, arXiv:0704.0647, JCAP 0704:017,2007 and A. L. arXiv:0705.0164 At large r can be below 0.14 of standard chaotic inflation with quadratic potential We studied the effect of future detection/non-detection of B-mode polarization from inflation on fundamental physics.

10. 1013 vi 07DoE Program Review Allen - Cluster Cosmology *Clusters SN +CMB *=>w=-1.01 +/-0.09

11. 1113 vi 07DoE Program Review Marusa Bradac - Bullet Cluster X-rays + weak lensing => Dark matter is collisionless Petrosian!

12. 1213 vi 07DoE Program Review Morganson - Galaxy Angular Correlation Function NOT gravitational clustering Faintest sources on sky 10 x number of galaxies Assembling galactic subcomponents They should be clustered They are! We can find out where they are etc by measuring weak lensing anisotropy in their correlation function

13. 1313 vi 07DoE Program Review The Physics of GLAST *General Purpose Observatory *GLAST-Physics emphasis: –Dark Matter and New Physics –Cosmic Particle Acceleration –Relativistic Outflows VERITAS/HESS

14. 1413 vi 07DoE Program Review Dark Matter and New Physics *~ 100 GeV WIMPS are best candidate for dark matter (but don’t forget axions!) *May be supersymmetric partners *May annihilate to create GeV gamma rays, detectable by GLAST *One of the rationales for DOE investing in GLAST *How do we best use the GLAST data to detect or limit the possibilities and how do we combine GLAST measurements with LHC, underground and astronomical measurements?

15. 1513 vi 07DoE Program Review Baltz - Dark Matter

16. 1613 vi 07DoE Program Review GLAST may “see” dark matter halos Complementary to LHC/ILC and underground searches

17. 1713 vi 07DoE Program Review 7/3 3/2 4/3 Moskalenko and Wai Dark Matter Burners  ~10 9 cm ~ 0.01 R sun *Extremely high dark matter density possibly exists near the supermassive black hole at the Galactic center *WIMP-nucleon scattering leads to gravitational capture and the accumulation of WIMPs stars *WIMP pair annihilation creates a new energy source in stars, i.e. the “burning” of dark matter *Degenerate electron cores at the Galactic center can “burn” dark matter quickly enough to be observable (Moskalenko & Wai 2007, ApJ 659, L29) 7/3 3/2 4/3 Capture rate vs distance from the central BH for Oxygen (left) and Iron (right) white dwarfs of T eff =(1.0- 1.5)x10 5 K. Numbers (7/3- adiabatic, 3/2, 4/3-instant) show power-law indices for the central spike profile.

18. 1813 vi 07DoE Program Review Cosmic Particle Acceleration *Active Galactic Nuclei, pulsars, supernova remnants accelerate particles to high energies *eg UHECRs accelerate to ZeV = billion TeV energies –Conservative view is this due to rapidly spinning massive black holes in the nuclei of distant galaxies generated ZV EMFs *Recent observations show that SNR accelerate PeV cosmic rays *Favored mechanism is Fermi acceleration at shock fronts *GLAST will provide the missing link that will help us understand the mechanism

19. 1913 vi 07DoE Program Review Funk- HESS Observations of SNR 10’ GeV TeV PeV Cosmic ray spectrum extends up to ZeV energies Break in spectrum (“knee”) at ~ 1 PeV HESS observes  -rays up to 100TeV =>cosmic rays below knee accelerated in SNR! Are they hadronic or leptonic? How are the magnetic fields amplified? Aharonian et al

20. 2013 vi 07DoE Program Review Stawarz - Relativistic Shocks Jet termination shocks accelerate a power-law distribution of electrons beaking at an energy of ~1 GeV, the proton rest mass => ionic plasma Stawarz, Cheung, et al. (2007): Spitzer Cygnus A

21. 2113 vi 07DoE Program Review Relativistic Outflows *Black Holes of all sizes and neutron stars are observed to launch pairs of relativistic jets with ultrarelativistic speeds in anti-parallel directions *These emit nonthermal photons throughout the entire 70 octave electromagnetic spectrum *We do not understand the composition of these jets, how they are collimated and where the emission originates *The most common source that GLAST will see are the jets from AGN pointed towards us and multiwavelength observing should help us answer these questions

22. 2213 vi 07DoE Program Review Paneque- Rapid variability of  -ray jets *Relativistic jets created by spinning black holes in nearby galaxies are powerful TeV  -ray emitters *MKN 501 (and PKS 2155-304) –The flux changes on timescales from months to ~2min –Higher energies later! *Great prospects for GLAST

23. 2313 vi 07DoE Program Review Cheung - Persistence of Relativistic Jets Cheung, Harris, & Stawarz (2007): Multiwavelength of M87 shows outbursts and ultrarelativistic speeds 100 pc from the black hole. M87 is a variable TeV source Where will GeV gamma rays observed by GLAST originate?

24. 2413 vi 07DoE Program Review Abel et al - Relativistic Outflows Abel, Wang & Zhang, 3D AMR Hydro => Relativistic jets GR MHD on the way. Visualization! Jets are turbulent Asymmetry can develop naturally

25. Fuerst - Relativistic Radiative Transfer q r Wang et al Take a GR MHD numerical simulation and compute the radiative transfer of Photons emitted by the hot gas in the flow

26. 2613 vi 07DoE Program Review Spitkovski -Pulsar Physics *How do pulsars shine? *Magnetosphere structure? –Wagoner 1971 Spitkovsky Thompson High confidence Low confidence GLAST?

27. 2713 vi 07DoE Program Review Romani - GLAST pulsar searches *GLAST should see 200 pulsars *Timing should explain how they work and enable new physics experiments eg in relativity High Energy Astrophysics Laboratory

28. 2813 vi 07DoE Program Review Breakout Sessions *Jha - Type 1a supernova *Stawarz - Astrophysical Jets *Amin - Structure Formation in the Universe *Do Couto e Silva - Gamma ray Bursts *Wise - Computational Cosmology *Funk, Cameron, DuBois - Gamma rays *Gilmore, Schindler, Burke - LSST *Roodman, Haller - SNAP *Allen - X-ray Cosmology *Church - QUaD (CMB polarization) *Tajima - Detectors

29. Steven Fuerst: General Relativistic Radiative Transfer Investigating the physics of accretion disks around black holes. Home-grown computer code uses ray-tracing to calculate the emission from arbitrary distributions and motions of gas. It can use analytic models of the flow, or results from GRMHD simulations as the “raw data”. The amount of emission and absorption is calculated from the state of the gas, and these are integrated along the line of sight to obtain images and spectra. Image of accretion disk and jet base calculated from density, temperature and velocity maps from Peng Wang and Weiqun Zhang's GRMHD simulation results. Cross section of an analytic accretion flow, showing the intensity of light as a function of position. The radiation field is calculated using a covariant moment method, and includes the effects of Thomson scattering. Current work involves extending the code to include scattering via the method of short characteristics, and making the code parallel to run on the new KIPAC cluster. q r