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Studying the Galactic Ridge Emission with SIMBOL-X

Studying the Galactic Ridge Emission with SIMBOL-X. Sandro Mereghetti IASF - Milano. Galactic Ridge X-ray Emission. X-ray emission extending along the Galactic plane Longitude extent ~ +/- 40 deg  Inner Galaxy R ~ 4 kpc Latitude extent ~ few deg  small scale height ~100 pc

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Studying the Galactic Ridge Emission with SIMBOL-X

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  1. Studying the Galactic Ridge Emission with SIMBOL-X Sandro Mereghetti IASF - Milano S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  2. Galactic Ridge X-ray Emission • X-ray emission extending along the Galactic plane • Longitude extent ~ +/- 40 deg  Inner Galaxy R ~ 4 kpc • Latitude extent ~ few deg  small scale height ~100 pc • High peak at GC • Luminosity ~ 2 10^38 erg/s • Intense emission lines S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  3. S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  4. Double T NEI model • Soft component kT~0.8 keV • Hard component kT~7 keV S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  5. Valinia et al. 2000 S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  6. 20-40 keV Lebrun et al. 2004 Nature 40-60 keV GRXE resolved by IBIS above 40 keV 60 – 120 keV 120-220 keV S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  7. S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  8. Ebisawa et al. 2005 S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  9. SIMBOL-X IMAGING DIFFUSE EMISSION NO IMAGING DISCRETE SOURCES ? S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  10. Simbol-X contribution: • Population studies in hard X-rays • Mapping of emission lines • Imaging-spectroscopy at >10 keV with point sources removed S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  11. Highly absorbed HMRXB discovered by INTEGRAL Tip of the iceberg ? 1 ) Population studies • Several hundreds of pointings at low Galactic latitude • FoV = p (0.1)^2 ~ 0.03 square deg  Sky coverage ~ several square deg •  Sensitivity tens of mCrabs • (100 x better than IBIS)  ~ 10 sources/square deg (2-10 keV)  ~100 serendipitous sources ..but how many in the 10-40 keV ? S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  12. 2 ) Mapping of emission lines Compare with XMM / EPIC :  Effective area larger than EPIC pn at E >~4-5 keV  similar energy resolution  similar angular resolution  much lower instrumental background Anticoincidence system Soft protons magnetic diverter  better modelling of continuum emission thanks to extended energy range S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  13. 3 ) Spectroscopy above 10 keV Done up to now only with collimated instruments Difficult to correctly estimate point sources contribution Deep pointings of selected regions in Galactic Plane can for the first time properly measure the GRXE spectrum Also the spatial distribution, e.g. latitude dependence, can be directly measured S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  14. Simulation of 500 ks pointing with Simbol-X spectrum of diffuse emission from 6 arcmin radius extraction region S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  15. S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  16. 3 ) Spectroscopy above 10 keV Done up to now only with collimated instruments Difficult to correctly estimate point sources contribution Deep pointings of selected regions in Galactic Plane can for the first time properly measure the GRXE spectrum Also the spatial distribution, e.g. latitude dependence, can be directly measured CAVEAT: Accuracy depends ultimately on good knowledge of instrumental background It is essential to control the systematics uncertainties S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  17. Formation flight can help: Mirror field of view detector S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  18. Formation flight can help: detector S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  19. Formation flight can help: detector S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  20. Formation flight can help: detector S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  21. Formation flight can help: Mirror field of view The external parts of the detection plane can monitor the instrumental background detector S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

  22. Conclusions • The spectral/imaging capabilities of SX will allow for the first time detailed studies of the GRXE above 10 keV • It will be possible to determine the contribution of hard X-ray sources and verify if a hot plasma is really needed • These studies have obvious implications on our understanding of the X-ray emission from the Galactic Center region • Several dedicated long (~500 ks) pointings required in addition to results from “serendipitous” sources • A small background level is not enough: It is essential to be able to reproduce its spatial and temporal variations S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/2007

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