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Evidence For The WHIM in The Diffuse X-ray Emission with Xmm-Newton

The Warm & Hot Universe New York, 7-9 May 2008. Evidence For The WHIM in The Diffuse X-ray Emission with Xmm-Newton. Massimiliano Galeazzi Anjali Gupta Eugenio Ursino. The missing baryon problem. WHIM. More than half the baryons at z=0 are unaccounted for;

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Evidence For The WHIM in The Diffuse X-ray Emission with Xmm-Newton

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  1. The Warm & Hot Universe New York, 7-9 May 2008 Evidence For The WHIMin The Diffuse X-ray Emissionwith Xmm-Newton Massimiliano Galeazzi Anjali Gupta Eugenio Ursino

  2. The missing baryon problem WHIM • More than half the baryons at z=0 are unaccounted for; • Hydrodynamic simulations predict that about 40% of the baryons are “hidden” in filaments with 105 < T < 107and 10 < r/ro < 1000, the Warm-Hot Intergalactic Medium (WHIM);

  3. WHIM detection MKN 421 (Nicastro et al., 2005) PKS 2155-304 (Fang et al., 2007) Redshifted emission lines Angular distribution Absorption Emission

  4. WHIM detection MKN 421 (Nicastro et al., 2005) PKS 2155-304 (Fang et al., 2007) Redshifted emission lines Angular distribution Absorption Emission

  5. WHIM angular distribution Angular Autocorrelation Function WHIM Groups Clusters

  6. XMM-Newton Data Lockman Hole Hubble Deep Field N Deep Field 1334+37 AXAF Ultra deep F Mosaic images of the targets used in this investigation. Energy range 0.4-0.6 keV The white circles represent the identified point sources. Eridanus Hole

  7. The Diffuse X-ray Background NH NH Local Bubble Unresolved point sources Galactic Halo WHIM Solar Wind Charge Exchange ~40 AU Detector Background ~100 pc ~2-5 kpc ~z<1

  8. Removal of contamination n2 w(Θ)=np2 wp(Θ)+nb2 wb(Θ)+nw2 ww(Θ) Detector Background Point Sources

  9. Control Observations NH NH MBM20 Eridanus Hole Local Bubble Unresolved point sources Galactic Halo WHIM Solar Wind Charge Exchange ~40 AU Detector Background ~100 pc ~2-5 kpc ~z<1

  10. Control Observations • MBM20 • l=211º24’15.7”, b=-36º33’46.7” • NH=15.9*1020 cm-2 • Absorption=75% at ¾ keV • 112±15 pc < d < 161±21 pc • Eridanus Hole • l=213º25’52.3”, b=-39º5’26.6” • NH=0.86*1020 cm-2 • Absorption=8% at ¾ keV IRAS 100 m map of MBM20 and surroundings with the two XMM pointing used in our investigation.

  11. Control Observations Calculated AcF for the two control targets: MBM20 (red) and the Eridanus hole (blue) ON-CLOUD: c2=16, n=19 OFF-CLOUD: c2=60, n=19

  12. Unidentified Point Sources n2 w(Θ)=np2 wp(Θ)+nb2 wb(Θ)+nw2 ww(Θ) • np from McCammon et al. • wp(q) from indentified point sources • - Giacconi et al. • - Hubble Deep Field N

  13. Results Conclusions Several sigma detection of the WHIM signature in the AcF of XMM-Newton blank fields. 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.

  14. Detecting the WHIM • Soft X-ray signature (redshifted OVII and O VIII lines) • Only “controversial” evidence is absorption from MRK421 (Nicastro et al. 2005) • Possibility of detecting it in emission through the Autocorrelation function (AcF – Ursino and Galeazzi, 2007) AcF 0.4 kev < E < 0.6 keV

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