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An XMM-Newton view of M101 Diffuse X-ray emission

An XMM-Newton view of M101 Diffuse X-ray emission. R.S. Warwick, L.P. Jenkins, A.M. Read, etal Reporter: FengLi. A Serie of papers. Jenkins et al.(2004a) , the spectral and timing properties of the brightest X-ray sources were investigated.

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An XMM-Newton view of M101 Diffuse X-ray emission

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  1. An XMM-Newton view of M101 Diffuse X-ray emission R.S. Warwick, L.P. Jenkins, A.M. Read, etal Reporter: FengLi

  2. A Serie of papers • Jenkins et al.(2004a) , the spectral and timing properties of the brightest X-ray sources were investigated. • Jenkins et al.(2005b) reported on the full catalogues of Xray source detected in M101 by XMM-Newton. • Warwick et al.(2007c) focus on the morphology and spectral properties of the diffuse X-ray component in M101.

  3. outlines • M101 • XMM study of X-ray emission properties • Spectra of diffuse x-ray emission and morphology properties • Future possible work

  4. M101 • Also named NGC 5457, a nearby face-on spiral galaxy • Center of M101 ( RA 14h 3m 12.55s, Dec +54◦ 20’56.5” ) • Distance to us, 7.2 Mpc • Apparent Dimension, 22.0 (arc min) • On the line-of-sight direction to M101

  5. XMM study of X-ray emission properties • Two Regions : 10’ from galactic centre (GC)* 5’ from GC • Three bands:* soft 0.3—1kev medium 1—2kev hard 2—6kev • bright sources L>1037erg/s are excluded, residual emissions are studied. The GALEX near-UV (NUV:2310 °A) band image of M101

  6. Residual x-ray emission components • the residual soft X-ray luminosity of the inner (10.5kpc radius) disk of M101 to be: • 20% of this flux may originate in unresolved relatively bright point X-ray sources ,Lx<1036erg/s • 5% of the flux may be attributable to intermediate luminosity sources, Lx<1034erg/s • at very faint levels, the integrated emission of dwarf stars may account for another 10% contribution

  7. Spectra of residual x-ray emission • The EPIC spectrum of the residual emission can be modelled as the sum of two thermal plasma components at temperatures of and

  8. Morphology of the residual emission • the spatial distribution of the residual soft X-ray emission in M101 shows it may comprise both a spiral arm component and a smoother disk component. • And the morphology show a good correlation with bands:FUV, NUV, UVW1, U, B and V, the best match is obtained with the U band data.

  9. These implies a close link between the X-ray emission and recent starformation.

  10. Future possible work • Given enough signal to noise and clarity of the spiral arm features might predict a spatial offset between the diffuse X-ray emission and the other spiral tracers.

  11. Thank you!

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