Andrea Albert (The Ohio State University) on behalf of The Fermi LAT Collaboration. HEP Seminar University of Virginia 12/05/12
|
|
- Garry Clifford Hoover
- 5 years ago
- Views:
Transcription
1 Indirect Searches for Dark Matter with the Fermi Large Area Telescope Andrea Albert (The Ohio State University) on behalf of The Fermi LAT Collaboration HEP Seminar University of Virginia 12/05/12
2 Outline Dark Matter Overview The Fermi Large Area Telescope The Gamma-ray Sky Recent Dark Matter Results Focus on spectral line search 12/05/2012 2
3 Outline Dark Matter Overview The Fermi Large Area Telescope The Gamma-ray Sky Recent Dark Matter Results Focus on spectral line search 12/05/2012 3
4 Astrophysical Evidence for Dark Matter Majority of mass in galaxies is dark Coma Cluster + Virial Theorem F. Zwicky (1937) Dark Matter clumps in large halos around galaxies Galactic Rotation Curves V. Rubin et al (1980) Dark Matter is virtually collisionless The Bullet Cluster D. Clowe et al (2006) www4.nau.e Dark Matter is non-baryonic CMB Acoustic Oscillations WMAP (2010) 12/05/2012 4
5 Astrophysical Evidence for Dark Matter Majority of mass in galaxies is dark Coma Cluster + Virial Theorem F. Zwicky (1937) Dark Matter clumps in large halos around galaxies Galactic Rotation Curves V. Rubin et al (1980) Dark Matter is virtually collisionless The Bullet Cluster D. Clowe et al (2006) www4.nau.e Dark Matter is non-baryonic CMB Acoustic Oscillations WMAP (2010) 12/05/2012 5
6 WIMPs detectable by Fermi LAT Weakly Interacting Massive Particle (WIMP) GeV-TeV mass scale Assume: Can annihilate or decay into SM particles Assume: Accounts for measured DM density Ex) Neutralino Predicted by many SUSY models LHC experiments starting to put strong constraints on SUSY Electrically neutral LSP stable particles GeV-TeV mass 12/05/2012 6
7 WIMPs as a Thermal Relic If WIMP was a thermal relic, then it was in creation/annihilation equilibrium in early universe Once universe cools enough, amount of dark matter freezes out No longer created, and expansion causes annihilation rate to drop to ~0 Assume weak scale σ ann observed abundance (~23%) <σv> ann ~ 3e-26 cm 3 /s (σ ann ~ 3 pb) v CDM ~ 0.3c Virial theorem -> to form stable halos around galaxies, DM particle should be non-relativistic (cold dark matter) ned.ipac.caltech.edu 12/05/2012 7
8 How to Detect WIMPs χ Production (collider) SM Direct Detection? (underground detectors) χ Indirect Detection SM 12/05/2012 8
9 WIMP Signatures (1) γ, Z, H 0, WIMP annihilation or decay can produce a variety of detectable SM particles Goal is to detect these particles and disentangle intrinsic WIMP properties 12/05/2012 9
10 WIMP Signatures (2) What we observe Φ,= DM Flux (events/cm 2 /s) Region of Interest (ROI) (dwarf galaxy, the whole sky, etc) 12/05/
11 WIMP Signatures (2) Intrinsic Particle Properties Φ,= Annihilation Cross Section * velocity (v ~ 0.3c) <σv> ann ~ 3e-26 cm 3 /s (σ ann ~ 3 pb) Predicted gamma ray dn/de from various annihilation channels Note: large fraction of predicted gamma s have E γ < m DM Gustafsson et al. PRL /05/
12 WIMP Signatures (2) Φ,= Dark matter density distribution (example simulation) Astrophysics 2 2 J-factor Line of sight integral over a ROI North Galactic Pole 90 0 lat South Galactic Pole lat 12/05/
13 WIMP Signatures (2) Φ,= Astrophysics 2 2 J-factor Line of sight integral over a ROI Various models for the smooth DM density as a function of distance from galactic center (r) Derived from fits to N-body simulations 12/05/
14 Outline Dark Matter Overview The Fermi Large Area Telescope The Gamma-ray Sky Recent Dark Matter Results Focus on spectral line search 12/05/
15 Fermi Large Area Telescope (LAT) On board the Fermi Gamma-ray Space Telescope Launched June 11, 2008 Started taking data Aug year mission Mission extended at least through 2016 Can go >300 GeV 12/05/
16 NASA Calorimeter to measure gamma-ray energy 12/05/
17 Fermi LAT Public Data Release: All γ-ray data made public within 24 hours (usually less) Si-Strip Tracker: convert γ->e + e - reconstruct γ direction EM v. hadron separation γ Fermi LAT Collaboration: ~400 Scientific Members, NASA / DOE & International Contributions Hodoscopic CsI Calorimeter: measure γ energy image EM shower EM v. hadron separation Trigger and Filter: Reduce data rate from ~10kHz to Hz e + e - Anti-Coincidence Detector: Charged particle separation 12/05/
18 Fermi LAT Effective Area M. Ackermann et al (The Fermi LAT Collaboration) ApJS 203, 4 (2012) arxiv: < 100 MeV limited by 3 in-a-row trigger requirement & drop in pair production cross section (see slide 16) > 100 GeV limited by backsplash See arxiv: for more info on Fermi LAT performance/validation 12/05/
19 Fermi LAT Point Spread Function (PSF) Vela Pulsar Counts Map (10 0 x10 0 ) A. Abdo et al (The Fermi LAT Collaboration) ApJ A (2009) MeV GeV >3 GeV M. Ackermann et al (The Fermi LAT Collaboration) ApJS 203, 4 (2012) arxiv: Limited by multiple scattering at low E Limited by strip pitch at high E (pitch = 228 µm) See arxiv: for more info on Fermi LAT performance/validation 12/05/
20 Fermi LAT Energy Dispersion M. Ackermann et al (The Fermi LAT Collaboration) ApJS 203, 4 (2012) arxiv: Limited by energy loss in tracker at low E Limited by leakage and CAL saturation at high E See arxiv: for more info on Fermi LAT performance/validation 12/05/
21 Outline Dark Matter Overview The Fermi Large Area Telescope The Gamma-ray Sky Recent Dark Matter Results Focus on spectral line search 12/05/
22 Daily Gamma-ray Sky 12/05/
23 Gamma-ray Sun Sun is typically not the brightest gamma-ray source Solar flares however APOD March 15, /05/
24 Fermi LAT Gamma-ray Sky 1 year all sky map (E > 1 GeV) 12/05/
25 Fermi LAT GammaGamma-ray Sky 4 year all sky map (E > 1 GeV) 12/05/
26 Fermi LAT GammaGamma-ray Sky Nature has given us a rich and complicated gamma-ray sky! Diffuse - complex gas structure - Various CR interactions Sources - Pulsars, AGN, SNR, etc Galactic Plane Isotropic - sources + diffuse - Extragalactic Dark Matter? - Will be a small piece 12/05/
27 Outline Dark Matter Overview The Fermi Large Area Telescope The Gamma-ray Sky Recent Dark Matter Results Focus on spectral line search 12/05/
28 Dark Matter Searches with the Fermi LAT 12/05/
29 Unexpected Excess in the Cosmic Ray e± Spectrum ATIC observed an unexpected bump in the CR e± spectrum Fermi observes a broader excess around the same energy This feature can be accounted for by adjusting the CR injection spectrum or nearby pulsars Can also be explained with leptophillic DM annihilation models Requires large <σv> ann to explain excess 12/05/
30 Unexpected Rise in local CR Positron Fraction Fermi measures a rise in the local highenergy CR positron fraction, consistent with the PAMELA results No magnet on-board, so use Earth s magnetic field Rise in local positron fraction disagrees with conventional model for cosmic rays Local positrons are secondaries created by CR nuclei interactions (this should cause fraction to decrease) This can be explained with leptophilic annihilating/decaying DM Requires large <σv> ann to explain excess Antiproton fraction does not rise; need to suppress hadronic modes see T. A. Porter et al. (2011) arxiv: v1; D. Grasso et al. (2009) arxiv: v3 for more 12/05/
31 DM Constraints from the Milky Way Halo Look in 2 year diffuse from GeV Mask out known gamma-ray sources Region of Interest: two off-plane rectangles (5 0 < b <15 0 & l <80 0 ) Minimizes DM profile uncertainties (central cuspiness varies) Limits astrophysical uncertainties (mask bright plane, avoid high latitude Fermi lobes and Loop I) This analysis focuses on setting limits on possible DM signals See non-dm like residuals (e.g. not centrally peaked) 12/05/
32 MW Halo Results- bƃ Annihilation Decay M. Ackermann et al (Fermi LAT Collaboration) Accepted for publication in ApJ (arxiv: ) bƃ annihilation spectrum is similar in shape to DM annihilations/decays producing heavy quarks and gauge bosons in this energy range Exclude canonical thermal relic WIMPs for masses below ~30 GeV in bƃ 12/05/
33 MW Halo Results-τ + τ - Annihilation Decay M. Ackermann et al (Fermi LAT Collaboration) Accepted for publication in ApJ (arxiv: ) Set limits assuming only Final State Radiation and FSR + Inverse Compton Only FSR = only photons produced by taus (no electrons) FSR + IC includes IC gamma rays from electrons produced via DM annihilation/decay Contours show 2σ and 3σ CL fits to PAMELA (purple) and Fermi (blue) positron fraction DM interpretation of positron fraction strongly disfavored (for annihilating DM) 12/05/
34 Constraints from dwarf galaxies Dwarf galaxies have a large mass-to-light ratio Good signal-to-noise for a DM search 12/05/
35 Combined dsphs Results Joint likelihood analysis of 10 dwarf galaxies 4 years of data in energy range 100 MeV 500 GeV Account for uncertainties in J-factor DM distribution determined using observed stellar velocities 4 annihilation channels considered No DM seen Exclude canonical thermal relic crosssection for masses less than ~10 GeV (in bƃ and tau s) Thermal relic cross-section 12/05/
36 Combined dsphs Results Joint likelihood analysis of 10 dwarf galaxies 4 years of data in energy range 100 MeV 500 GeV Account for uncertainties in J-factor DM distribution determined using observed stellar velocities 4 annihilation channels considered No DM seen Exclude canonical thermal relic crosssection for masses less than ~10 GeV (in bƃ and tau s) Thermal relic cross-section 12/05/
37 Projected Limit Improvement with dsphs 12/05/
38 Virgo Galaxy Cluster (1) Virgo ROI counts map DM annihilation profile Han et al Han et al 2012 (arxiv ) claimed ~4 sigma evidence from dark matter annihilation in the Virgo galaxy cluster Very extended DM annihilation profile (from substructure), majority of excess comes from inner 3 deg of the profile 12/05/
39 Virgo Galaxy Cluster (2) TS map with 0.5 deg bins TS map with 0.2 deg bins New Point Sources Interstellar Emission Model cluster center Fermi-LAT Col. Publication in preparation Macias-Ramirez et al. (2012) Fermi-LAT Col. Publication in preparation Excess is not in the cluster center (as expected from DM) Macias-Ramirez find 7 new candidate point sources that could explain excess Han et al 2012 (arxiv ) find 4 new candidate point sources Significance depends strongly on the interstellar emission model Requires a detailed study of systematic uncertainties especially of the interstellar emission model even for extragalactic regions Virgo is at fairly low galactic latitude and in a challenging region for diffuse emission modeling. 12/05/
40 Search for Gamma-ray Spectral Lines Gustafsson et al. PRL Annihilation/decay directly into γγ or Xγ (X = Z 0, H 0, ) Smoking Gun channel Advantage: sharp, distinct feature Disadvantage: low predicted counts 12/05/
41 The Fermi LAT Line Search 2 year analysis accepted for publication in PRD Current analysis uses similar method 4 year analysis nearing completion Use Reprocessed Pass 7 Clean data Low cosmic-ray contamination Reprocessing shifts energy scale by 1-4% to account for expected accumulation of radiation damage to calorimeter Plan to submit paper to PRD end of December 2012 Search for lines from 5 to 300 GeV Maximum Likelihood Fit Use sliding ±6σ E windows Fit for energies in σ E steps Perform finer 0.5σ E scan near significant energies Model bkg as single powerlaw Γ bkg and f sig free in fit M. Ackermann el al. (FERMI-LAT) PRD 86, (2012) arxiv: /05/
42 Improved Model for LAT Response to a Line Use full detector simulation to get Fermi LAT energy dispersion Previously modeled line with a triple gaussian fit ( 1D PDF ) This analysis adds a 2 nd dimension to line model: P E P E is the probability that measured energy is true energy Labeled CTBBestEnergyProb in our extended data 2D PDF (a function of both energy and P E ) Break Line into 10 P E slices and do triple gaussian fit in each slice separately Fit explicitly at 9 energies and interpolate parameters in each slice to produce lines at other energies Including P E ~15% improvement to signal sensitivity (when there is signal) and counts upper limit (when there is no signal) 100 GeV Line Model M. Ackermann et al. (FERMI-LAT) PRD 86, (2012) arxiv: D PDF 2D PDF 12/05/
43 Region of Interest (ROI) Optimization Many have shown ROI optimization importance in line searches e.g. C. Weniger JCAP 1208 (2012) 007 Find R GC that optimizes sig/sqrt(bkg) ROI choices made a priori using MC sig from J factor in that ROI bkg from MC simulation of galactic diffuse model _details/pass7_galactic.html Search in 5 ROIs R0 (12 x10 GC box) R16 (Einasto Optimized) R41 (NFW Optimized) Relative S/N R90 (Isothermal Optimized) R180 (2 year Analysis ROI) R GC (degrees) R GC NFW Optimized ROI E > 2.6 GeV 12/05/
44 Spectral Line 95% CL Flux Upper Limit R16 No globally significant lines found Most significant fit was in R0 at 5 GeV, ~2σ (3.7σ local) Expected limits calculated from powerlaw-only pseudo-experiments No systematic errors applied Einasto optimized ROI 12/05/
45 95% CL <σv> γγ Einasto Upper Limit R16 Einasto optimized ROI Expected limits calculated from powerlaw-only pseudo-experiments No systematic errors applied 12/05/
46 Line-like Feature near 135 GeV Our blind search does not find globally significant feature near 135 GeV Reprocessing shifts feature from 130 GeV to 135 GeV Most significant fit was in R0, 2.23σ local (<0.5σ global) Much interest after detection of line-like feature localized in the Galactic center at 130 GeV See C. Weniger JCAP 1208 (2012) 007 arxiv: σ (local) 1D fit at 130 GeV with 4 year unreprocessed data Look in 4 x4 GC ROI Use 1D PDF (no use of P E ) Note: Fit in 4 x4 GC ROI Not one of our a priori ROIs 12/05/
47 Line-like Feature near 135 GeV Our blind search does not find globally significant feature near 135 GeV Reprocessing shifts feature from 130 GeV to 135 GeV Most significant fit was in R0, 2.23σ local (<0.5σ global) Much interest after detection of line-like feature localized in the Galactic center at 130 GeV See C. Weniger JCAP 1208 (2012) 007 arxiv: σ (local) 1D fit at 130 GeV with 4 year unreprocessed data Look in 4 x4 GC ROI Use 1D PDF (no use of P E ) 3.73σ (local) 1D fit at 135 GeV with 4 year reprocessed data Look in 4 x4 GC ROI Use 1D PDF (no use of P E ) Note: Fit in 4 x4 GC ROI Not one of our a priori ROIs 12/05/
48 Line-like Feature near 135 GeV Our blind search does not find globally significant feature near 135 GeV Reprocessing shifts feature from 130 GeV to 135 GeV Most significant fit was in R0, 2.23σ local (<0.5σ global) Much interest after detection of line-like feature localized in the Galactic center at 130 GeV See C. Weniger JCAP 1208 (2012) 007 arxiv: σ (local) 1D fit at 130 GeV with 4 year unreprocessed data Look in 4 x4 GC ROI Use 1D PDF (no use of P E ) 3.73σ (local) 1D fit at 135 GeV with 4 year reprocessed data Look in 4 x4 GC ROI Use 1D PDF (no use of P E ) 3.35σ (local) 2D fit at 135 GeV with 4 year reprocessed data Look in 4 x4 GC ROI Use 2D PDF P E in data feature is slightly narrower than expected <2σ global Note: Fit in 4 x4 GC ROI Not one of our a priori ROIs 12/05/
49 Spatial Morphology of Features in Galactic Plane Fit in 4 x4 ROIs along the Galactic plane in 1 steps Fit with 1D PDF To find where the counts are coming from Allowed for negative fluctuations Find excess near ~135 GeV near GC But find similar features at other energies along the GP Some indication the 135 feature not smooth, but 2-3 smaller hot spots Excess near 135 GeV is one of the largest and near GC, but is not otherwise unique Fits at 93 GeV Fits at 136 GeV Fit Significance (σ) 12/05/
50 135 GeV in the Earth Limb spectrum (1) Earth Limb is a bright, well understood source γ rays from CR interactions in the atmosphere Expected to be a smooth power-law Can be used to study instrumental effects Can see in loosest cuts can study cut efficiencies Need to cut on times when the LAT was pointing at the limb Have made changes to increase our Limb dataset Pole-pointed observations each week Extended targets of opportunity Trace limb while target is occulted θ zenith θ inc γ ray Preliminary Zenith Angle 12/05/
51 135 GeV in the Earth Limb spectrum (2) P7Transient to P7Clean Efficiency Fit to Limb data Preliminary Points: Flight Data Curve: MC 111 < θ zenith < 113 Rocking Angle > 52 Dips in efficiency below and above 135 GeV Appear to be related to CAL-TKR agreement Could be artificially sculpting the energy spectrum Line-like feature in the limb at 135 GeV Appears when LAT is pointing at the Limb Surprising since limb should be smooth S/N limb ~18%, while S/N GC ~30% - 66% (depending on ROI choice) Limb feature not large enough to explain all the GC signal 12/05/
52 Pass 8 Better event selection (higher signal efficiency at the same bkg level) Expect a ~25% increase in high-energy effective area in the standard photon classes Better control over systematic uncertainties Extend both low and high energy reach Include calorimeter-only events (substantial effective area increase above 40 GeV) Better high-energy point spread function 12/05/
53 Summary The Fermi LAT team has looked for indirect DM signals using a wide variety of different methods So far no signals have been detected and strong constraints have been set Observed deviations from conventional models in e + e - spectrum Confirm PAMELA e + fraction increase We do not see any globally significant spectral lines Uncovered some aspects of the 135 GeV line that require more study Significance decreases with analysis improvements Also present in the Earth limb Too soon to draw firm conclusions, more data needed More data + Pass 8 will give a more definitive answer in 1 year Current searches are already exploring interesting parts of WIMP phase space and will just keep getting more sensitive; stay tuned for more exciting Dark Matter results from the Fermi LAT! 12/05/
54 Fermi LAT Collaboration References For a list of Fermi LAT collaboration publications see The Fermi Large Area Telescope On Orbit: Event Classification, Instrument Response Functions, and Calibration arxiv: Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV arxiv: Measurement of separate cosmic-ray electron and positron spectra with the Fermi Large Area Telescope arxiv: Constraints on the Galactic Halo Dark Matter from Fermi-LAT Diffuse Measurements arxiv: Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope arxiv: Fermi LAT Search for Dark Matter in Gamma-ray Lines and the Inclusive Photon Spectrum arxiv: Anisotropies in the diffuse gamma-ray background measured by the Fermi LAT *** arxiv: Profumo and Linden, Gamma-ray Lines in the Fermi Data: is it a Bubble? *** arxiv: M.N. Mazziotta et al A model-independent analysis of the Fermi Large Area Telescope gamma-ray data from the Milky Way dwarf galaxies and halo to constrain dark matter scenarios *** arxiv: M. Ajello et al (The Fermi LAT Collaboration) Constraints on dark matter models from a Fermi LAT search for highenergy cosmic-ray electrons from the Sun *** arxiv: ***not discussed in this talk 12/05/
55 BACKUP SLIDES
56 Halo Method I No-background Limits Conservative Method II w/detailed bkg modeling on next slide No non-dm background modeling Robust to many uncertainties Expected DM counts (n DM ) compared to observed counts (n data ) and 3σ and 5σ upper limits are set using n 3(5) n > DM DM n data in at least one energy bin 12/05/
57 Halo Method II Limits + Bkg Modeling Profile likelihood fit combining several GALPROP diffusion models with DM Derives DM limits marginalized over astrophysical uncertainties Allow several bkg parameters to vary CRE injection index, diffuse halo height, gas (HI) to dust ratio, CR source distribution, local H 2 to CO factor, and isotropic normalization Distribution of CR sources is uncertain, so left free in radial Galactic bins. To be conservative to DM constraints, CR source distribution set to zero in the inner 3 kpc Maps of each GALPROP + DM model are made and fit to the Fermi LAT data, incorporating both morphology and spectra 12/05/
58 MW Halo Results-µ + µ - Set limits assuming only Final State Radiation and FSR + Inverse Compton Only FSR = only photons produced by muons (no electrons) FSR + IC includes IC gamma rays from electrons produced via DM annihilation/decay Contours show 2σ and 3σ CL fits to PAMELA (purple) and Fermi (blue) positron fraction DM interpretation of positron fraction strongly disfavored (for annihilating DM) 12/05/
59 Fractionally small, but significant deviations We see fractionally small, but significant fluctuations in the galactic data and limb spectrum at low energies Fractional deviation or smaller than uncertainties in A eff See similar features in earth limb at low energies See section 7.5 of Pass 7 performance paper The Fermi-LAT Col. ApJS 203, 4 (2012) Need to consider both fit significance and fractional deviation resid resid The Fermi LAT Col. ApJS 203, 4 (2012) arxiv: frac norm ( ni = f i ( ni = f i f f i i ) ) n i f i 12/05/
Update on the Two Smoking Gun" Fermi LAT Searches for Dark Matter- Milky Way Dwarfs and Lines
Update on the Two Smoking Gun" Fermi LAT Searches for Dark Matter- Milky Way Dwarfs and Lines Elliott Bloom KIPAC-SLAC, Stanford University On Behalf of the Fermi-LAT Collaboration What We are Learning
Using the Fermi-LAT to Search for Indirect Signals from Dark Matter Annihilation
Using the Fermi-LAT to Search for Indirect Signals from Dark Matter Annihilation Tim Linden UC - Santa Cruz Representing the Fermi-LAT Collaboration with acknowledgements to: Brandon Anderson, Elliott
Indirect searches for dark matter with the Fermi LAT instrument
Indirect searches for dark matter with the Fermi LAT instrument M. Nicola Mazziotta INFN-Bari mazziotta@ba.infn.it 2nd international workshop on HERD Beijing Dec 2-3, 2013 Indirect Dark Matter Search +
A New View of the High-Energy γ-ray Sky with the Fermi Telescope
A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11
Tentative observation of a gamma-ray line at the Fermi Large Area Telescope
Tentative observation of a gamma-ray line at the Fermi Large Area Telescope arxiv:1203.1312 with T. Bringmann, X. Huang, A. Ibarra, S. Vogl (accepted for JCAP), arxiv:1204.2797 (accepted for JCAP) Christoph
Constraining Galactic dark matter in the Fermi-LAT sky with photon counts statistics
Constraining Galactic dark matter in the Fermi-LAT sky with photon counts statistics Moriond Cosmology 2018 Silvia Manconi (University of Turin & INFN) March 20, 2018 In collaboration with: Hannes Zechlin,
M. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009
M. Lattanzi ICRA and Dip. di Fisica - Università di Roma La Sapienza In collaboration with L. Pieri (IAP, Paris) and J. Silk (Oxford) Based on ML, Silk, PRD 79, 083523 (2009) and Pieri, ML, Silk, MNRAS
Recent Searches for Dark Matter with the Fermi-LAT
Recent Searches for Dark Matter with the Fermi-LAT on behalf of the Fermi-LAT Collaboration CETUP* DM Workshop Deadwood, SD 7 July 2016 A One-Slide History of Dark Matter Particle Physics Astrophysics
Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration
Measurement of the cosmic ray positron spectrum with the Fermi LAT using the Earth s magnetic field Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration International Cosmic Ray
Testing a DM explanation of the positron excess with the Inverse Compton scattering
Testing a DM explanation of the positron excess with the Inverse Compton scattering Gabrijela Zaharijaš Oskar Klein Center, Stockholm University Work with A. Sellerholm, L. Bergstrom, J. Edsjo on behalf
Latest Results on Dark Matter and New Physics Searches with Fermi. Simona Murgia, SLAC-KIPAC on behalf of the Fermi-LAT Collaboration
Latest Results on Dark Matter and New Physics Searches with Fermi Simona Murgia, SLAC-KIPAC on behalf of the Fermi-LAT Collaboration TeV Particle Astrophysics 2009 SLAC, July 13-16 2009 DM and New Physics
Indirect dark matter detection and the Galactic Center GeV Excess
Image Credit: Springel et al. 2008 Indirect dark matter detection and the Galactic Center GeV Excess Jennifer Siegal-Gaskins Caltech Image Credit: Springel et al. 2008 Jennifer Siegal-Gaskins Caltech Image
Hunting for Dark Matter in Anisotropies of Gamma-ray Sky: Theory and First Observational Results from Fermi-LAT
Hunting for Dark Matter in Anisotropies of Gamma-ray Sky: Theory and First Observational Results from Fermi-LAT Eiichiro Komatsu (Texas Cosmology Center, Univ. of Texas at Austin) MPA Seminar, September
The High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
Sep. 13, JPS meeting
Recent Results on Cosmic-Rays by Fermi-LAT Sep. 13, 2010 @ JPS meeting Tsunefumi Mizuno (Hiroshima Univ.) On behalf of the Fermi-LAT collaboration 1 Outline Introduction Direct measurement of CRs CRs in
Dark Matter searches with astrophysics
Marco Taoso IPhT CEA-Saclay Dark Matter searches with astrophysics IAP 24 February 2013 The cosmological pie Non baryonic Dark Matter dominates the matter content of the Universe Motivation to search for
Indirect Dark Matter Detection
Indirect Dark Matter Detection Martin Stüer 11.06.2010 Contents 1. Theoretical Considerations 2. PAMELA 3. Fermi Large Area Telescope 4. IceCube 5. Summary Indirect Dark Matter Detection 1 1. Theoretical
The Characterization of the Gamma-Ray Excess from the Central Milky Way
The Characterization of the Gamma-Ray Excess from the Central Milky Way Tim Linden along with: Tansu Daylan, Doug Finkbeiner, Dan Hooper, Stephen Portillo, Tracy Slatyer, Ilias Cholis 1402.6703 1407.5583
Constraining Dark Matter annihilation with the Fermi-LAT isotropic gamma-ray background
Constraining Dark Matter annihilation with the Fermi-LAT isotropic gamma-ray background Fiorenza Donato @ Physics Dept., Un. Torino The gamma-ray sky - Minneapolis, October 10, 2013 Plan of my talk What
Fundamental Physics with GeV Gamma Rays
Stefano Profumo UC Santa Cruz Santa Cruz Institute for Particle Physics T.A.S.C. [Theoretical Astrophysics, Santa Cruz] Fundamental Physics with GeV Gamma Rays Based on: Kamionkowski & SP, 0810.3233 (subm.
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission 1 Outline Mainly from 2009 ApJ 697 1071 The Pair Conversion Telescope The Large Area Telescope Charged Background and Events
Tesla Jeltema. Assistant Professor, Department of Physics. Observational Cosmology and Astroparticle Physics
Tesla Jeltema Assistant Professor, Department of Physics Observational Cosmology and Astroparticle Physics Research Program Research theme: using the evolution of large-scale structure to reveal the fundamental
PHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
Searching for spectral features in the g-ray sky. Alejandro Ibarra Technische Universität München
Searching for spectral features in the g-ray sky Alejandro Ibarra Technische Universität München Oslo 5 November 2014 Outline Motivation Indirect dark matter searches with gamma-rays. Overcoming backgrounds
Searching for Dark Matter in the Galactic Center with Fermi LAT: Challenges
Searching for Dark Matter in the Galactic Center with Fermi LAT: Challenges Simona Murgia University of California, Irvine Debates on the Nature of Dark Matter Sackler 2014 19-22 May 2014 arxiv:0908.0195
The Characterization of the Gamma-Ray Excess from the Central Milky Way
The Characterization of the Gamma-Ray Excess from the Central Milky Way Tim Linden along with: Tansu Daylan, Doug Finkbeiner, Dan Hooper, Stephen Portillo, Tracy Slatyer, Ilias Cholis 1402.6703 1407.5583
Dark Matter. Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET)
Dark Matter Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET) 1 Dark Matter 1933 r. - Fritz Zwicky, COMA cluster. Rotation
Searching for dark matter annihilation lines with HESS II. Knut Dundas Morå for the HESS collaboration
Searching for dark matter annihilation lines with HESS II Knut Dundas Morå for the HESS collaboration Outline Indirect Dark Matter detection Dark Matter signatures Dark Matter distributions Fermi Line
Interstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
Gamma-ray emission at the base of the Fermi bubbles. Dmitry Malyshev, Laura Herold Erlangen Center for Astroparticle Physics
Gamma-ray emission at the base of the Fermi bubbles Dmitry Malyshev, Laura Herold Erlangen Center for Astroparticle Physics On behalf of the Fermi-LAT collaboration TeVPA 2018, Berlin Fermi bubbles surprise
Indirect Dark Matter Searches in the Milky Way Center with the LAT on board Fermi
Indirect Dark Matter Searches in the Milky Way Center with the LAT on board Fermi B. Cañadas, A. Morselli and V. Vitale on behalf of the Fermi LAT Collaboration Outline Gamma rays from Dark Matter Dark
Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity
Cosmic Positron Signature from Dark Matter in the Littlest Higgs Model with T-parity Masaki Asano The Graduate University for Advanced Studies Collaborated with Shigeki Matsumoto Nobuchika Okada Yasuhiro
Spectra of Cosmic Rays
Spectra of Cosmic Rays Flux of relativistic charged particles [nearly exactly isotropic] Particle density Power-Law Energy spectra Exponent (p, Nuclei) : Why power laws? (constraint on the dynamics of
Probing Dark Matter with Cosmic Messengers
Probing Dark Matter with Cosmic Messengers Andrea Albert Los Alamos National Lab 3rd KMI International Symposium January 6, 2017 Outline Indirect Detection Overview evidence for dark matter dark matter
Indirect Dark Matter Searches: a Review Eric Charles SLAC National Lab.
Indirect Dark Matter Searches: a Review Eric Charles SLAC National Lab. 13 eme Recontres de Vietnam: Exploring the Dark Universe 24 July 2017, Quy Nhon, Vietnam Outline 2 I. Review / Context: indirect
EGRET Excess of diffuse Galactic Gamma Rays as a Trace of the Dark Matter Halo
EGRET Excess of diffuse Galactic Gamma Rays as a Trace of the Dark Matter Halo Indirect Search for Dark Matter W. de Boer 1, I. Gebauer 1, A.V. Gladyshev 2, D. Kazakov 2, C. Sander 1, V. Zhukov 1 1 Institut
The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays
The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays Simona Murgia, SLAC-KIPAC for the Fermi LAT Collaboration Dark Matter Signatures in the Gamma-ray Sky Austin, Texas 7-8 May 2012 arxiv:0908.0195
Dark matter in split extended supersymmetry
Dark matter in split extended supersymmetry Vienna 2 nd December 2006 Alessio Provenza (SISSA/ISAS) based on AP, M. Quiros (IFAE) and P. Ullio (SISSA/ISAS) hep ph/0609059 Dark matter: experimental clues
Fermi: Highlights of GeV Gamma-ray Astronomy
Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration Neutrino Oscillation Workshop Otranto, Lecce, Italy
Dark Matter in the Galactic Center
Dark Matter in the Galactic Center Tim Linden University of Chicago along with: Eric Carlson, Ilias Cholis, Dan Hooper, Manoj Kaplinghat, Stefano Profumo, Jennifer Siegal-Gaskins, Tracy Slatyer, Hai-Bo
The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays
The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays Simona Murgia, SLAC-KIPAC for the Fermi LAT Collaboration UCLA Dark Matter 2012 Marina del Rey 22-24 February 2012 arxiv:0908.0195 Gamma
Indirect Detection of Dark Matter with Gamma Rays
Indirect Detection of Dark Matter with Gamma Rays Simona Murgia SLAC-KIPAC University of California, Irvine on behalf of the Fermi LAT Collaboration Dark Attack 212 Ascona, Switzerland 15-2 July 212 WIMP
Recent Results on Dark Matter Searches with Fermi. Simona Murgia, SLAC-KIPAC on behalf of the Fermi-LAT Collaboration
Recent Results on Dark Matter Searches with Fermi Simona Murgia, SLAC-KIPAC on behalf of the Fermi-LAT Collaboration KITP-UCSB 8 December 2009 The Observatory Observe the gamma-ray sky in the 20 MeV to
Fermi measurements of diffuse gamma-ray emission: results at the first-year milestone
SciNeGHE 2009 Assisi, October 7th Fermi measurements of diffuse gamma-ray emission: results at the first-year milestone Luigi Tibaldo luigi.tibaldo@pd.infn.it INFN Sezione di Padova Dip. di Fisica G. Galilei,
Gamma rays from Galactic pulsars: high- and lowlatitude
Francesca Calore Gamma rays from Galactic pulsars: high- and lowlatitude emission Conca Specchiulla, 8th September 2014 based on: F. Calore, M. Di Mauro & F. Donato, arxiv:1406.2706 F. Calore, I. Cholis
Constraining dark matter signal from a combined analysis of Milky Way satellites using the Fermi-LAT arxiv: v1 [astro-ph.
Constraining dark matter signal from a combined analysis of Milky Way satellites using the Fermi-LAT arxiv:1102.5701v1 [astro-ph.he] 28 Feb 2011 Stockholm University E-mail: maja.garde@fysik.su.se On behalf
What is known about Dark Matter?
What is known about Dark Matter? 95% of the energy of the Universe is non-baryonic 23% in the form of Cold Dark Matter From CMB + SN1a + surveys Dark Matter enhanced in Galaxies and Clusters of Galaxies
Instituto de Fisica Teórica, IFT-CSIC Madrid. Marco Taoso. DM and the Galactic Center GeV excess
Instituto de Fisica Teórica, IFT-CSIC Madrid Marco Taoso DM and the Galactic Center GeV excess Frontier Objects in Astrophysics and Particle Physics Vulcano Workshop 26-05- 2016 How and where to look for
Dark Matter in the Universe
Dark Matter in the Universe NTNU Trondheim [] Experimental anomalies: WMAP haze: synchrotron radiation from the GC Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron
GALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS. Jongkuk Kim (SKKU) Based on Physics Letters B.
GALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS Jongkuk Kim (SKKU) Based on Physics Letters B. 752 (2016) 59-65 In collaboration with Jong Chul Park, Seong Chan Park The
DeepCore and Galactic Center Dark Matter
2nd Low-Energy Neutrino Workshop (PSU July 1-2, 2010) DeepCore and Galactic Center Dark Matter Carsten Rott carott @ mps. ohio-state.nospamedu Center for Cosmology and AstroParticle Physics The Ohio State
DM subhalos: The obser vational challenge
DM subhalos: The obser vational challenge Hannes-S. Zechlin and Dieter Horns Inst. f. Experimentalphysik, Universität Hamburg, Germany July 26th, 2012 DM subhalos in the Milky Way concordance cosmology
Constraints on dark matter annihilation cross section with the Fornax cluster
DM Workshop@UT Austin May 7, 2012 Constraints on dark matter annihilation cross section with the Fornax cluster Shin ichiro Ando University of Amsterdam Ando & Nagai, arxiv:1201.0753 [astro-ph.he] Galaxy
Highlights from the Fermi Symposium
Highlights from the Fermi Symposium Aldo Morselli INFN Roma Tor Vergata 1 The LAT at 2 Years and 17 days from the 3 rd!!! 11 June 2008 2 Fermi is Making a Major Impact Science, December 2009 Breakthrough
Gamma Ray Physics in the Fermi era. F.Longo University of Trieste and INFN
Gamma Ray Physics in the Fermi era F.Longo University of Trieste and INFN Vulcano, May 22, 2018 F.Longo et al. -- 1 Gamma-ray astrophysics above 100 MeV AGILE Fermi 2 Picture of the day, Feb. 28, 2011,
DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
Structure of Dark Matter Halos
Structure of Dark Matter Halos Dark matter halos profiles: DM only: NFW vs. Einasto Halo concentration: evolution with time Dark matter halos profiles: Effects of baryons Adiabatic contraction Cusps and
Neutrinos and DM (Galactic)
Neutrinos and DM (Galactic) ArXiv:0905.4764 ArXiv:0907.238 ArXiv: 0911.5188 ArXiv:0912.0512 Matt Buckley, Katherine Freese, Dan Hooper, Sourav K. Mandal, Hitoshi Murayama, and Pearl Sandick Basic Result
SEARCH FOR AXION- LIKE PARTICLE SIGNATURES IN GAMMA-RAY DATA
SEARCH FOR AXION- LIKE PARTICLE SIGNATURES IN GAMMA-RAY DATA MANUEL MEYER, JAN CONRAD, MIGUEL SANCHEZ-CONDE DECEMBER 11, 2015 GAMMA RAYS AND DARK MATTER 2015 OBERGURGL, AUSTRIA MANUEL.MEYER@FYSIK.SU.SE
Natural explanation for 130 GeV photon line within vector boson dark matter model
Natural explanation for 130 GeV photon line within vector boson dark matter model Yasaman Farzan IPM, TEHRAN Plan of talk Direct and indirect dark matter searches 130 or 135 GeV line in FermiLAT data Challenges
Constraints on Light WIMPs from Isotropic Diffuse γ-ray Emission
Constraints on Light WIMPs from Isotropic Diffuse γ-ray Emission Michel H.G. Tytgat Université Libre de Bruxelles Belgium Rencontres de Moriond: EW Interactions and Unified Theories March 2011 There are
High-Energy GammaRays toward the. Galactic Centre. Troy A. Porter Stanford University
High-Energy GammaRays toward the Galactic Centre Troy A. Porter Stanford University Fermi LAT 5-Year Sky Map > 1 GeV Galactic Plane Galactic Centre Point Sources Diffuse γ-ray emission produced by cosmic
Non-detection of the 3.55 kev line from M31/ Galactic center/limiting Window with Chandra
Non-detection of the 3.55 kev line from M31/ Galactic center/limiting Window with Chandra Meng Su (MIT)! Pappalardo/Einstein fellow!! In Collaboration with Zhiyuan Li (NJU)!! 15 Years of Science with Chandra!
Lecture 14. Dark Matter. Part IV Indirect Detection Methods
Dark Matter Part IV Indirect Detection Methods WIMP Miracle Again Weak scale cross section Produces the correct relic abundance Three interactions possible with DM and normal matter DM Production DM Annihilation
Cosmic Ray Excess From Multi-Component Dark Matter
Cosmic Ray Excess From Multi-Component Dark Matter Da Huang Physics Department, NTHU @ LeCosPA PRD89, 055021(2014) [arxiv: 1312.0366] PRD91, 095006 (2015) [arxiv: 1411.4450] Mod. Phys. Lett. A 30 (2015)
Emmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile,
Emmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile, Italy Emmanuel Moulin CTA meeting, Zürich 2009 1 Core-energy
A New Look at the Galactic Diffuse GeV Excess
A New Look at the Galactic Diffuse GeV Excess Brian Baughman Santa Cruz Institute for Particle Physics 1 Overview Diffuse gamma-ray emission The Galactic diffuse gamma-ray GeV excess Discussion of the
Dark Matter Electron Anisotropy: A universal upper limit
Seminari teorici del venerdì Enrico Borriello Università degli Studi di Napoli Federico II & INFN Sezione di Napoli Dark Matter Electron Anisotropy: A universal upper limit Based on Borriello, Maccione,
Preliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET)
Preliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET) Y.Asaoka for the CALET Collaboration RISE, Waseda University 2016/12/15 CTA-Japan Workshop The extreme
Prospects for indirect dark matter detection with Fermi and IACTs
Prospects for indirect dark matter detection with Fermi and IACTs Francesc Ferrer Washington University in St. Louis TeV Particle Astrophysics, SLAC, July 2009 Signals of Dark Matter (DM) at γ ray telescopes
Cosmic Ray panorama. Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1
1912 1932 Cosmic Ray panorama http::// Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1 Pamela : < 0.1 evt year/gev Flux E α α 2.7 / 3.3 Statistical precision
Signatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:
Signatures of clumpy dark matter in the global 2 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:0808.088 Daniel Grin Ay. Journal Club /23/2009 /8 Signatures of clumpy dark matter in
Mattia Di Mauro. Fermi-LAT point source population studies and origin of the Fermi-LAT gamma-ray background. Trieste, May, 3, 2016
Fermi-LAT point source population studies and origin of the Fermi-LAT gamma-ray background Mattia Di Mauro On behalf of the Fermi- LAT Collaboration 1 Trieste, May, 3, 2016 THE ISOTROPIC GAMMA RAY BACKGROUND
Gamma-ray Astrophysics
Gamma-ray Astrophysics AGN Pulsar SNR GRB Radio Galaxy The very high energy -ray sky NEPPSR 25 Aug. 2004 Many thanks to Rene Ong at UCLA Guy Blaylock U. of Massachusetts Why gamma rays? Extragalactic Background
Annihilation Phenomenology. Christoph Weniger. GRAPPA, University of Amsterdam
Annihilation Phenomenology Christoph Weniger GRAPPA, University of Amsterdam Thursday 26th March 2015, Effective Field Theories and Dark Matter, Mainz 1 Overview Galactic center excess & PCA Best fit DM
CTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters
CTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters Moritz Hütten (MPP Munich) for the CTA consortium "The extreme Universe viewed in very-highenergy
Dark Matter Annihilations in the Galactic Center
Dan Hooper (Fermilab/University of Chicago) Debates on the Nature of Dark Matter, Harvard/CfA May 21, 2014 Dark Matter Annihilations in the Galactic Center This talk is based on: T. Daylan, D. Finkbeiner,
Signal Model vs. Observed γ-ray Sky
Signal Model vs. Observed γ-ray Sky Springel+, Nature (2008) Two main dark matter signal components: 1. galactocentric diffuse 2. small structures Observed sky modeled with bremsstrahlung π 0 decay up-scattered
The Sun and the Solar System in Gamma Rays
The Sun and the Solar System in Gamma Rays R. Desiante1 on behalf of the Fermi-LAT collaboration SciNeGHE 2016 1 INFN Torino Outline Introduction The Fermi Gamma-Ray Space Telescope The active Sun as seen
Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects
Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects Aldo Morselli INFN Roma Tor Vergata CTA in the quest for Dark Matter and exotic phenomena
DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT
DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT A.Malinin a, For AMS Collaboration IPST, University of Maryland, MD-20742, College Park, USA Abstract. The Alpha Magnetic Spectrometer (AMS), to be installed
Implication of AMS-02 positron fraction measurement. Qiang Yuan
Implication of AMS-02 positron fraction measurement Qiang Yuan (yuanq@ihep.ac.cn) Institute of High Energy Physics, Chinese Academy of Sciences Collaborated with Xiaojun Bi, Guo-Ming Chen, Yi-Qing Guo,
Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants
Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants Marianne Lemoine-Goumard (CENBG, Université Bordeaux, CNRS-IN2P3, France) On behalf of the Fermi-LAT and HESS Collaborations
Search for exotic process with space experiments
Search for exotic process with space experiments Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Rencontres de Moriond, Very High Energy Phenomena in the Universe Les Arc, 20-27
Searching for dark matter. with gamma-ray anisotropies
Image Credit: NASA/DOE/International LAT Team Searching for dark matter with gamma-ray anisotropies Jennifer Siegal-Gaskins CCAPP, Ohio State University with Brandon Hensley (Caltech!Princeton) Eiichiro
Signals from Dark Matter Indirect Detection
Signals from Dark Matter Indirect Detection Indirect Search for Dark Matter Christian Sander Institut für Experimentelle Kernphysik, Universität Karlsruhe, Germany 2nd Symposium On Neutrinos and Dark Matter
New results from the AMS experiment on the International Space Station. Henning Gast RWTH Aachen
New results from the AMS experiment on the International Space Station Henning Gast RWTH Aachen 1 Questions to AMS-02: Are there galaxies made of anti-matter in the Universe? What is the nature of Dark
CMB constraints on dark matter annihilation
CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:
Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Observatory Paper Review
Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Observatory Paper Review Stephen Portillo Review of R. Abbasi et al. (IceCube Collaboration), Phys. Rev. D 84, 022004 (2011). Introduction
SPATIAL UNIFORMITY OF THE GALACTIC GAMMA-RAY EXCESS. Manoj Kaplinghat, UC Irvine
SPATIAL UNIFORMITY OF THE GALACTIC GAMMA-RAY EXCESS Manoj Kaplinghat, UC Irvine Bas Observed Extended Counts Source Model THE GALACTIC CENTER EXCESS 0.69 0.95 GeV 0.95 1.29 GeV 1.29 1.76 GeV 1.76 2.40
The Egret Excess, an Example of Combining Tools
The Egret Excess, an Example of Combining Tools Institut für Experimentelle Kernphysik, Universität Karlsruhe TOOLS 2006-26th - 28th June 2006 - Annecy Outline Spectral Fit to EGRET data Problems: Rotation
Indirect Dark Matter constraints with radio observations
Indirect Dark Matter constraints with radio observations In collaboration with E.Borriello and G.Miele, University of Naples Federico II Alessandro Cuoco, Institute for Physics and Astronomy University
Quest for New Physics
Stefano Profumo UC Santa Cruz Santa Cruz Institute for Particle Physics T.A.S.C. [Theoretical Astrophysics in Santa Cruz] Cosmic Rays and the Quest for New Physics Scineghe 2010, Trieste, Italy Thursday,
The Galactic Center Excess. Kevork N. Abazajian
The Galactic Center Excess Kevork N. Abazajian WIMP Annihilation gamma rays in the Galactic Center? Model Data Abazajian & Kaplinghat 2012 Canonical Weakly-Interacting Massive-Particle (WIMP) Cold Dark
SUPPLEMENTARY INFORMATION
1. Selecting electrons in ATIC ATIC is a calorimetric instrument and, as such, relies upon the difference in the development of the cascades (showers) initiated by protons and electrons. Moreover, the
Cosmic ray electrons from here and there (the Galactic scale)
Cosmic ray electrons from here and there (the Galactic scale) Julien Lavalle Department of Theoretical Physics Torino University and INFN Outline: (i) local electrons (ii) comments on synchrotron [based
Cosmic Ray Electrons and GC Observations with H.E.S.S.
Cosmic Ray Electrons and GC Observations with H.E.S.S. Christopher van Eldik (for the H.E.S.S. Collaboration) MPI für Kernphysik, Heidelberg, Germany TeVPA '09, SLAC, July 2009 The Centre of the Milky
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background
Indirect detection of decaying dark matter
Indirect detection of decaying dark matter Alejandro Ibarra Technical University of Munich Many thanks to Chiara Arina, Wilfried Buchmüller, Gianfranco Bertone, Laura Covi, Mathias Garny, Michael Grefe,
Recent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants