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AND F AR ...L INKS WITH THE WMAP H AZE Greg Dobler Harvard/CfA May - PowerPoint PPT Presentation

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C OSMIC R AYS N EAR AND F AR ...L INKS WITH THE WMAP H AZE Greg Dobler Harvard/CfA May 6 th , 2009 - IAP C OSMIC R AYS N EAR AND F AR ...L INKS WITH THE WMAP H AZE Doug Finkbeiner (CfA) Neal Weiner (NYU) Greg Dobler Dan Hooper (FNAL) Ilias

  1. C OSMIC R AYS N EAR AND F AR ...L INKS WITH THE WMAP H AZE Greg Dobler Harvard/CfA May 6 th , 2009 - IAP

  2. C OSMIC R AYS N EAR AND F AR ...L INKS WITH THE WMAP H AZE Doug Finkbeiner (CfA) Neal Weiner (NYU) Greg Dobler Dan Hooper (FNAL) Ilias Cholis (NYU) Gabrijela Zaharijas (ANL) Lisa Goodenough (NYU) Harvard/CfA May 6 th , 2009 - IAP

  3. WMAP

  4. WMAP Haslam et al. (1982) Finkbeiner et al. (1999) thermal dust synchrotron H α (Finkbeiner, 2003) free-free

  5. template fitting s 23 x + f 23 x + d 23 x = - c 23 x 23 GHz

  6. template fitting s 23 x + f 23 x + d 23 x = - c 23 x 23 GHz s( ν i ), f( ν i ), d( ν i ) represent estimates of the synchrotron, free-free, and dust spectra

  7. determining foreground spectra P r a = w Multi-Linear Regression r Template Fit a = ( P / σ ) + ( w / σ ) = P r - Bands are completely decoupled 2 2 a − w r P a − w 2 ≡ χ - Spectral shapes are unconstrained 2 σ σ σ - Constant across the sky Dobler & Finkbeiner, 2008 TEMPLATES CMB ESTIMATORS - Synchrotron: Haslam et al ( 1982 ) - 6 different types - Dust: FDS99 ( Finkbeiner et al 1999 ) - introduces a cross-correlation bias - Free-free: H α Map (WHAM, SHASSA, - mean zero VTSS; assembled and corrected - largest source of uncertainty for dust by Finkbeiner 2003 )

  8. peeling away foregrounds K-band: 23 GHz WMAP

  9. peeling away foregrounds K-band: 23 GHz WMAP - CMB

  10. peeling away foregrounds K-band: 23 GHz WMAP - CMB - free-free

  11. peeling away foregrounds K-band: 23 GHz WMAP - CMB - free-free - (thermal and spinning) dust

  12. peeling away foregrounds K-band: 23 GHz WMAP - CMB - free-free - (thermal and spinning) dust - (soft) synchrotron

  13. the haze • Multi-linear regression fit K: 23 GHz • Excess towards the GC Ka: 33 GHz Q: 41 GHz Dobler & Finkbeiner (2008)

  14. the haze • Multi-linear regression fit K: 23 GHz • Excess towards the GC Ka: 33 GHz Separate, hard synchrotron component Upcoming surveys at 5 GHz Q: 41 GHz (CBASS), 15 GHz, and especially Planck will provide A LOT more information! Dobler & Finkbeiner (2008)

  15. the haze spectrum K-band: 23 GHz WMAP - CMB - free-free - (thermal and spinning) dust

  16. 23 GHz Synchrotron

  17. 33 GHz Synchrotron

  18. 41 GHz Synchrotron

  19. 61 GHz Synchrotron

  20. the haze spectrum • Looks like synchrotron with, α E 2 dN/dE ∝ E -0.1 ≤ α ≤ 0.2 • If it is synchrotron, it requires – hard e + e - spectrum – extended emission • Very difficult to produce astrophysically Dobler & Finkbeiner (2008)

  21. the haze spectrum • Looks like synchrotron with, α E 2 dN/dE ∝ E -0.1 ≤ α ≤ 0.2 Can be confirmed by ICS signal in Fermi ! Dobler & Finkbeiner (2008)

  22. dark matter and the haze Galactic/baryon params: B ~ 10 µ G K(E) ~ 10 28 cm 2 /s Dark matter params: ρ = ρ (r) M ~ 100 GeV < σ v> ~ few x10 -26 cm 3 /s

  23. dark matter and the haze Galactic/baryon params: B ~ 10 µ G K(E) ~ 10 28 cm 2 /s Dark matter params: ρ = ρ (r) M ~ 100 GeV < σ v> ~ few x10 -26 cm 3 /s the haze is consistent with a WIMP annihilation scenario

  24. dark matter and the haze Galactic/baryon params: B ~ 10 µ G K(E) ~ 10 28 cm 2 /s Dark matter params: ρ = ρ (r) M ~ 100 GeV < σ v> ~ few x10 -26 cm 3 /s the haze is consistent with a WIMP annihilation scenario there are large astrophysical uncertainties!

  25. 8.5 kpc PAMELA ATIC Haze

  26. 8.5 kpc PAMELA ATIC Haze Cholis, Dobler, et al. (2008)

  27. 8.5 kpc PAMELA ATIC Haze Cholis, Dobler, et al. (2008)

  28. 8.5 kpc PAMELA ATIC Haze Cholis, Dobler, et al. (2008)

  29. the haze... facts and myths

  30. the haze... facts and myths misconceptions

  31. the haze: facts . foreground spectra have significant uncertainties - CMB cross-correlations (systematic) - template approximations

  32. the haze: facts

  33. CMB “cross-correlation” bias

  34. CMB “cross-correlation” bias s 23 x + f 23 x + d 23 x = - c 23 x 23 GHz

  35. CMB “cross-correlation” bias → + b s x

  36. CMB “cross-correlation” bias s 23 x + f 23 x + d 23 x ( ) = - c 23 x + b s x 23 GHz

  37. CMB “cross-correlation” bias s 23 x + f 23 x + d 23 x ( ) = - c 23 x + b s x 23 GHz s ν → s ν - c ν x b s f ν → f ν - c ν x b f d 23 → d ν - c ν x b d

  38. the haze: facts This ambiguity will be eliminated with Planck

  39. the haze: facts . foreground spectra have significant uncertainties - CMB cross-correlations (systematic) - template approximations . spectrum is harder than synchrotron elsewhere in the galaxy - I SN ∝ ν - α ⇒ dN/dE ∝ E -(2 α +1) - I haze ∝ ν -( α -0.5) ⇒ dN/dE ∝ E -(2 α +1)

  40. the haze: facts Dobler & Finkbeiner (2008)

  41. the haze: facts . spectra of foreground emissions have uncertainties - CMB cross-correlations (systematic) - template approximations . spectrum is harder than synchrotron elsewhere in the galaxy - I SN ∝ ν - α ⇒ dN/dE ∝ E -(2 α +1) - I haze ∝ ν -( α -0.5) ⇒ dN/dE ∝ E -(2 α +1) . morphology is roughly spherical, but there are inhomogeneities

  42. the haze: facts K-band: 23 GHz WMAP - CMB - free-free - (thermal and spinning) dust - (soft) synchrotron

  43. the haze: myths the haze... . does not exist... nobody else sees it

  44. the haze: myths Bennett et al, 2003 Hinshaw et al, 2007 Bottino et al, 2008 Dickinson et al, 2009

  45. the haze: myths Bennett et al, 2003 Hinshaw et al, 2007 Bottino et al, 2008 Dickinson et al, 2009 (implied 23 GHz)

  46. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized

  47. the haze: myths WMAP 23 GHz polarized emission Kogut et al, 2007 Note: spinning dust is important when comparing to 23 GHz total intensity!

  48. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized . is easily explained by SNe

  49. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized . is easily explained by SNe - diffused haze spectrum is (roughly) as hard as fermi spectrum extending over ~ ( 4 kpc) 3 volume

  50. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized . is easily explained by SNe . is easily explained by pulsars

  51. the haze: myths Injection spectrum : dN/dE = N 0 × f(E) with N 0 = ??? and f(E) = ??? ⇒ can (likely) fit the haze spectrum Spatial distribution : ln ρ (r,z) = -r/r 0 - |z|/z 0 with r 0 = 4.5 kpc and z 0 = 0.08 kpc ⇒ cannot fit the morphology

  52. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized . is easily explained by SNe . is easily explained by pulsars . is easily explained by small spectral index variation of Haslam

  53. the haze: myths WMAP data w/o haze template Dobler & Finkbeiner (2008) w/ haze template the haze is morphologically distinct from Haslam

  54. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized . is easily explained by SNe . is easily explained by pulsars . is easily explained by small spectral index variation of Haslam . is direct evidence of particle DM annihilation

  55. the haze: myths Galactic/baryon params: B ~ 10 µ G K(E) ~ 10 28 cm 2 /s Dark matter params: ρ = ρ (r) M ~ 100 GeV < σ v> ~ few x10 -26 cm 3 /s the haze is consistent with a WIMP annihilation scenario

  56. the haze: myths Galactic/baryon params: B ~ 10 µ G K(E) ~ 10 28 cm 2 /s Dark matter params: ρ = ρ (r) M ~ 100 GeV < σ v> ~ few x10 -26 cm 3 /s the haze is consistent with a WIMP annihilation scenario but again... there are large astrophysical uncertainties!

  57. the haze: myths the haze... . does not exist... nobody else sees it . should be strongly polarized . is easily explained by SNe . is easily explained by pulsars . is easily explained by small spectral index variation of Haslam . is direct evidence of particle DM annihilation . DM model over-produces synchrotron at high latitudes

  58. the haze: myths Galactic/baryon params: B ~ 10 µ G K(E) ~ 10 28 cm 2 /s Dark matter params: ρ = ρ (r) M ~ 100 GeV < σ v> ~ few x10 -26 cm 3 /s the haze is consistent with a WIMP annihilation scenario but again... there are large astrophysical uncertainties!

  59. comments and the future of the haze . boundary conditions - dN/dE → 0 at boundary not very realistic - spherical halo with K(E) → K(E,r,z) . full astro-uncertainties analysis for cross section and masses - Galactic magnetic field: ≥ 2 (amplitude, shape, turbulence, etc.) - ISRF: ~1.2-1.5 (see Porter et al, 2008 ) - DM halo shape: ??? (local density ~2 , radial profile, sub-[sub-]structures ~5-10 ) - uncertainties in haze analysis, etc... . Fermi ICS emission towards the GC (regardless of origin) . Planck spectral index measurements

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