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Dark Matter Annihilation in the Galactic Center

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Dark Matter Annihilation in the Galactic Center DARK MATTER ANNIHILATION IN THE GALACTIC CENTER Dan Hooper – Fermilab and the University of Chicago UCLA Dark Matter Conference February 18, 2016 10 Dan Hooper – DM Annihilation in the GC Sorry if I sound like a broken record… 10 Reason 1: Overwhelming Statistical Significance and Detailed Information 4 ! This excess consists of ~10 Thephotons Dark per square Matter meter, Interpretation per year (>1 GeV, within 10° of the Galactic Center) ! The spectral shape of the excess can be well fit by a dark matter Raw Mapparticle with a massResidual in the Map range (x3) of 7 to 12 GeV (similar to that required Dark Matter In The Galactic by CoGeNT, DAMA, and CRESST), annihilating primarily to τ+τ- Center Region (possibly among other leptons) ! The spectrum contains a bump-like feature at ~1-5 GeV ! The angular distribution of the ! Can be fit quite well by a simple 25-30 GeV dark matter particle, in a cusped signal is well fit by a halo profile withdistribution (γ~1.1), annihilating to bb with σv ~ 9 x 10-26 cm3/s -γ ρ(r) ~ r , with γ ~ 1.25 to 1.4 (in good agreement with expectations from simulations) ! The normalization of the signal requires the dark matter to have an annihilation cross section within a factor of a few of the value predicted for a simple thermal FIG. 9: The raw gamma-ray maps (left) andrelic the ( residualσv ~ 3x10 maps-26 after cm subtracting3/s) the best-fit Galactic di↵use model, 20 cm template, point sources, and isotropic template (right), in units of photons/cm2/s/sr. The right frames clearly contain a significant central and spatially extended excess, peaking at 1-3 GeV. Results are shown in galactic coordinates, and all maps ⇠ haveUCLA been smoothed DM by a 0.252014◦ Gaussian. of the Galactic Plane, while values greater Hooper than one and are Linden,not onlyPRD, elongated arXiv:1110.0006 along or perpendicular to the Galac- preferentially extended perpendicular to the plane. In tic Plane, but along any arbitrary orientation. Again, each case, the profile slope averaged over all orientations we find that that the quality of the fit worsens if the the is taken to be γ =1.3 (left) and 1.2 (right).UCLA From this DMtemplate 2012 is significantly elongated either along or per- figure, it is clear that the gamma-ray excess prefers to pendicular to the direction of the Galactic Plane. A mild be fit by an approximately spherically symmetric distri- statistical preference isDan found, Hooper however, - The for Hunt a morphology For Dark Matter L. Goodenough, D. Hooper, arXiv:0910.2998 bution, and disfavors any axis ratio which departs from with an axis ratio of 1.3-1.4 elongated along an axis ro- ⇠ FIG.unity 9: by The more raw than gamma-ray approximately maps (left) 20%. and the residual mapstated after subtracting35◦ counterclockwise the best-fit Galactic from the di↵ Galacticuse model, Plane 20 cm in template, point sources, and isotropic template (right), in unitsgalactic of photons/cm⇠ coordinates2/s/sr. (a similarThe right preference frames clearly was also contain found a In Fig. 11, we generalize this approach within our significant central and spatially extended excess, peaking at 1-3in GeV. our Results Inner Galaxy are shown analysis). in galactic While coordinates, this may and be aall statis- maps ⇠ UCLA DM 2010 haveGalactic been Center smoothed analysis by a 0.25 to◦ testGaussian. morphologies that are of the Galactic Plane, while values greater than one are not only elongated along or perpendicular to the Galac- preferentially extended perpendicular to the plane. In tic Plane, but along any arbitrary orientation. Again, each case, the profile slope averaged over all orientations we find that that the quality of the fit worsens if the the is taken to be γ =1.3 (left) and 1.2 (right). From this template is significantly elongated either along or per- figure, it is clear that the gamma-ray excess prefers to pendicular to the direction of the Galactic Plane. A mild be fit by an approximately spherically symmetric distri- statistical preference is found, however, for a morphology bution, and disfavors any axis ratio which departs from with an axis ratio of 1.3-1.4 elongated along an axis ro- ⇠ unity by more than approximately 20%. tated 35◦ counterclockwise from the Galactic Plane in galactic⇠ coordinates (a similar preference was also found In Fig. 11, we generalize this approach within our in our Inner Galaxy analysis). While this may be a statis- Galactic Center analysis to test morphologies that are Dan Hooper – DM Annihilation in the GC The Evolving Nature of the Galactic Center Debate Dan Hooper – DM Annihilation in the GC The Evolving Nature of the Galactic Center Debate UCLA 2010 There is no Galactic Center excess (“what are you smoking?”) Dan Hooper – DM Annihilation in the GC The Evolving Nature of the Galactic Center Debate UCLA 2010 There is no Galactic Center excess (“what are you smoking?”) UCLA 2012 Sure there seems to be a Galactic Center excess, but 1) Are we sure that it is spatially extended? 2) Are we mismodeling standard diffuse emission mechanisms? 3) Is there really a Galactic Center excess? Dan Hooper – DM Annihilation in the GC The Evolving Nature of the Galactic Center Debate UCLA 2010 There is no Galactic Center excess (“what are you smoking?”) UCLA 2012 Sure there seems to be a Galactic Center excess, but 1) Are we sure that it is spatially extended? 2) Are we mismodeling standard diffuse emission mechanisms? 3) Is there really a Galactic Center excess? UCLA 2014 What is generating this excess? 1) A large population of centrally located millisecond pulsars? 2) A series of recent cosmic ray outbursts? 3) Annihilating dark matter? Dan Hooper – DM Annihilation in the GC The Evolving Nature of the Galactic Center Debate UCLA 2010 There is no Galactic Center excess (“what are you smoking?”)* UCLA 2012 Sure there seems to be a Galactic Center excess, but 1) Are we sure that it is spatially extended? 2) Are we mismodeling standard diffuse emission mechanisms? 3) Is there really a Galactic Center excess? UCLA 2014 What is generating this excess? 1) A large population of centrally located millisecond pulsars? 2) A series of recent cosmic ray outbursts? 3) Annihilating dark matter? *Dave Klein was very supportive during this critical time Dan Hooper – DM Annihilation in the GC The Basic Features of the GeV Excess 7 ! Bright and highly statistically significant ! Distributed with spherical symmetry about the Galactic Center with a flux that falls as ~r -2.4, between ~0.06° and ~10° (if interpreted as annihilating dark matter, -1.2 ρDM ~ r between ~10-1500 pc) ! The spectrum of this excess peaks at 10 10 ~1-3 GeV, and is in good agreement with FIG. 6: Left frame: The spectrum of the dark matter component, extracted from a fit in our standard ROI (1◦ < b < 20◦, | | that predictedl < 20from◦) for a templatea ~35-50 corresponding GeV to a generalizedWIMP NFW halo profile with an inner slope of γ =1.18 (normalized to the | | flux at an angle of 5◦ from the Galactic Center). Shown for comparison (solid line) is the spectrum predicted from a 43.0 GeV 26 3 3 2 annihilating darkto matterbb (for particle example) annihilating to b¯b with a cross section of σv =2.25 10− cm /s [(0.4GeV/cm )/⇢local] . Right frame: ⇥ ⇥ as left frame, but for a full-sky ROI ( b > 1◦), with γ =1.28; shown for comparison (solid line) is the spectrum predicted from | | 26 3 3 2 a 36.6 GeV dark matter particle annihilating to b¯b with a cross section of σv =0.75 10− cm /s [(0.4GeV/cm )/⇢local] . ! To normalize the observed signal with ⇥ ⇥ annihilating ofdark the Galactic matter, plane; masking a cross the region section with b < 2◦ sistent with that extracted at higher latitudes (see Ap- | | -26changes3 the preferred value to γ =1.25 in our default pendix A).7 Shown for comparison (as a solid line) is the of σv ~ 10 ROI, cm and/sγ =1 is. 29required over the whole sky. In contrast to spectrum predicted from (left panel) a 43.0 GeV dark Ref. [8], we find no significant di↵erence in the slope pre- matter particle annihilating to b¯b with a cross section 26 3 3 2 ferred by the fit over the standard ROI, and by a fit only of σv =2.25 10− cm /s [(0.4 GeV/cm )/⇢local] , over the southern half (b<0) of the ROI (we also find and (right panel)⇥ a 36.6 GeV dark⇥ matter particle anni- DH, Goodenough (2009, 2010), DH, Linden (2011),26 no significant di↵erence between the fit over the full sky hilating to b¯b with a cross section of σv =0.75 10− and the southern half of the full sky). ThisAbazajian can be seen, Kaplinghatcm3/s [(0.4 GeV(2012),/cm3)/⇢ Gordon,]2. The spectra Macias extracted⇥ (2013), ⇥ local directly from Fig. 5, where the full-skyDaylan and southern- et al (2014),for this component Calore are, Cholis in moderately, Weniger good agreement (2014) sky fits for the same level of masking are found to favor with the predictions of the dark matter models, yielding quite similar values of γ (the southern sky distribution fits of χ2 = 44 and 64 over the 22 error bars between 0.3 is broader than that for the full sky simply due to the and 50 GeV. We emphasize that these uncertainties (and di↵erence in the number of photons).
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