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Philadelphia, 22 April 2008

Sources of contamination in the emission from the Local Bubble. Anjali Gupta Massimiliano Galeazzi Eugenio Ursino. Philadelphia, 22 April 2008. Outline. The Diffuse X-ray background Unidentified point sources Spectral Properties The Warm Hot Intergalactic Medium (WHIM)

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Philadelphia, 22 April 2008

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  1. Sources of contamination in the emission from the Local Bubble Anjali Gupta Massimiliano Galeazzi Eugenio Ursino Philadelphia, 22 April 2008

  2. Outline • The Diffuse X-ray background • Unidentified point sources • Spectral Properties • The Warm Hot Intergalactic Medium (WHIM) • Spectral properties • Angular properties Philadelphia, 22 April 2008

  3. The Diffuse X-ray Background Philadelphia, 22 April 2008

  4. The Diffuse X-ray Background NH NH Local Bubble Unresolved point sources Galactic Halo WHIM Solar Wind Charge Exchange ~40 AU ~100 pc ~2-5 kpc M. Galeazzi and A. Gupta (tomorrow) This Talk ~z<1

  5. Identification of the point sources Lockman Hole Hubble Deep Field Deep Field 1334+37 AXAF Ultra deep F Eridanus Hole Mosaic images of the targets used in this investigation. The white circles represent the identified point sources. Philadelphia, 22 April 2008

  6. The logN-logS The averaged logN-logS for all the targets used in our investigation Philadelphia, 22 April 2008

  7. Spectral Properties of the point sources Average spectrum of all the sources detected in the 0.5-2.0 keV (black circles) and 0.4-0.6 keV (pink circles) bands. The black and red curve represent the powerlaw fit with the photon index of 1.77±0.01 and 1.93±0.01, for the two bands respectively. Philadelphia, 22 April 2008

  8. Spectral Properties of the bright and the faint sources Average spectrum of the bright (black) and faint (pink) sources detected in the 0.5-2.0 KeV. The black and red curve represent the powerlaw fit with the photon index of 1.87±0.01 and 1.40±0.05, for the bright and faint sources respectively. Excess emission Average spectrum of the bright (black) and faint (pink) sources detected in the 0.4-0.6 KeV. The black and red curve represent the powerlaw fit with the photon index of 2.05±0.01 and 1.69±0.04, for the bright and faint sources respectively. Philadelphia, 22 April 2008

  9. The Warm Hot Intergalactic Medium Borgani et al. 2004 Cen & Ostriker, 1999 Spatial distribution of the WHIM at z~0 Philadelphia, 22 April 2008

  10. Flux vs. Redshift Expected average flux in the energy range 0.370-0.925 keV due to the WHIM as a function of red-shift. The total average flux due to the WHIM is about 5.7 photons/cm2/s/sr The total DXB flux is about 29.3 photons/cm2/s/sr (derived using data from McCammon et al., 2002 - ApJ 576, 188). Philadelphia, 22 April 2008

  11. Spectral Distribution of the WHIM Philadelphia, 22 April 2008

  12. WHIM signature in the Angular distribution of X-ray images Lockman Hole Hubble Deep Field Deep Field 1334+37 AXAF Ultra deep F Eridanus Hole Mosaic images of the targets used in this investigation. The white circles represent the identified point sources. Philadelphia, 22 April 2008

  13. AngularAutocorrelation The fraction of X-rays due to the WHIM in the energy band 0.4-0.6 keV is 18±5% of the total diffuse X-ray emission. Calculated AcF for the two control targets, MBM20 (squares) and the Eridanus hole (full circles), compared with the average AcF (empty circles). Philadelphia, 22 April 2008

  14. Conclusion NH Local Bubble Solar Wind Charge Exchange (18±5)% (11.7)% Unresolved point sources Galactic Halo WHIM The End ~40 AU ~100 pc ~2-5 kpc Philadelphia, 22 April 2008 ~z<1

  15. Angular Autocorrelation • n2 w(Θ)=np2 wp(Θ)+nb2 wb(Θ)+nw2 ww(Θ) ACF of the diffuse X-ray background and its components.

  16. Acf of Hubble Deep field North

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