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Fluorescent Emission from Lyman Limit systems

Fluorescent Emission from Lyman Limit systems. Cristine Peroux Michael Rauch Huub Roettgering Tom Theuns. George Becker Andy Bunker Stefano Cristiani James Graham Martin Haehnelt Matt Jarvis Cedric Lacey Simon Morris. To Earth. Lyman limit. Figure by John Webb.

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Fluorescent Emission from Lyman Limit systems

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  1. Fluorescent Emission from Lyman Limit systems Cristine Peroux Michael Rauch Huub Roettgering Tom Theuns George Becker Andy Bunker Stefano Cristiani James Graham Martin Haehnelt Matt Jarvis Cedric Lacey Simon Morris

  2. To Earth Lyman limit Figure by John Webb

  3. Fluorescent re-emission of the ionizing UV background ionizing photon in • 50% of the time • photon • out LL-system 912>1 1216>10000 912 resonant scattering Photons are absorbed and re-emitted at the surface of the Lyman Limit systems. Hogan & Weiman 1987

  4. Resonant Ly scattering Ly photons are scattered into the wings of the line where they can escape. Zheng & Miralda-Escude 2002

  5. Lyman Limit systems act as a mirror uniform slab Gould & Weinberg 1996 Uniform surface brightness measure flux of UV background

  6. How strong is the expected signal ?

  7. The metagalactic ionization rate proximity effect Bolton et al. 2005

  8. What are Lyman Limit systems? The radial extension of damped Ly systems?

  9. Expected size distribution Extrapolates size dis- tribution of model for damped Ly systems of Haehnelt, Steinmetz & Rauch (1998, 2000) to smaller column den- sity.

  10. Expected luminosity distribution

  11. How can we look for it? • Long-slit spectroscopy • Narrow-band Imaging • Integral field spectroscopy • Multi-slit spectroscopy

  12. What are we looking for? Zheng & Miralda-Escude 2002

  13. What can we see with FORS? J-22= 8.0 Expect to see about 20-30 systems J-22= 6.0 J-22= 3.0

  14. Observations • large ESO program, back-up for bad seeing • field of 19th mag QSO DMS2139-0405 • FORS2 +1400V grism, 4460-5740 • R=2100, slit length = 418 arcsec • 60h so far (expect 2.5  detections)

  15. A raw frame

  16. 60h on FORS2 coadded

  17. Have we seen anything? Not yet, but should already obtain interesting upper limit ( Bunker et al.).

  18. Summary • Regions optically thick at 912 should glow fluorescently with a universal (sort of) surface brightness amplitude of metagalactic • ionization rate • Typical expected size and flux are 5 arcsec and • log f Ly = -17.67 + log • Should see 20 –30 absorbers in 120h with FORS2 at 4 . • 60h of data obtained. Expected S/N is achieved.

  19. How many are expected? optimistic model

  20. observed Compact emitters How many are expected? optimistic model

  21. Santos et al. 2004 La Delliou et al. 2005

  22. Giant Ly blobs Bower et al. 2004 Matsuda et al. 2004

  23. Bunker et al. 1999

  24. The Physics of the Intergalactic Medium (RTN 2000-2004)

  25. Comparison to other observations Our results with uncertainties (Bolton et al. 2005)

  26. Comparison to other observations Rates from QSOs (Boyle et al. 2000) + IGM re-emission (Madau, Haardt & Rees 1999, updated)

  27. Comparison to other observations Rates from galaxies (Bruzual & Charlot model), QSOs+IGM re-emission (Madau, Haardt & Rees 1999, updated)

  28. Comparison to other observations Proximity effect (Scott et al. 2000) and emission from Lyman-break galaxies (Steidel et al. 2001) JSB, Haehnelt, Viel & Springel, 2005

  29. The influence of galactic winds on the IGM 1 mean flux 0 Adelberger et al Desjaques et al. 2004 distance to next LBG

  30. Steidel @ KITP Desjaques et al. 2004 Spherical bubbles 1h-1 Mpc Volume filling factor < 1% ?

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