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A deep VLT study of extended Lyman-  emission from QSOs

Background: a spin-off project (in progress) What we see Physical origin?. A deep VLT study of extended Lyman-  emission from QSOs. Johan P. U. Fynbo. www.dark-astro.dk Dark Cosmology Centre l Niels Bohr institute l Copenhagen University. Background:. Palle Møller

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A deep VLT study of extended Lyman-  emission from QSOs

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  1. Background: a spin-off project (in progress) • What we see • Physical origin? A deep VLT study of extended Lyman- emission from QSOs Johan P. U. Fynbo www.dark-astro.dk Dark Cosmology Centre l Niels Bohr institute l Copenhagen University

  2. Background: Palle Møller Bjarne Thomsen Michael Weidinger It all started 10 years ago with our wish to study the associated absorber towards Q205-30.... Collaborators:

  3. NTT 1998 results on Q1205-30

  4. VLT 2000 results on Q1205-30 The extended emission was not from the absorber, but from the QSO.

  5. How common is this? Next step is to build a sample!

  6. Spectra

  7. Spectra

  8. 1d spectra, SB profiles and velocity profiles

  9. General properties • Sizes 1-10 kpc scale length. • 400-600 km s-1 velocity widths. • No associated CIV and HeII emission.

  10. Comparison with literature: • Literature sample: 17 RLQs, 5 RQQs • Extended Lyman- emission from RQQs is on average fainter, smaller and has narrower velocity width (up to publication bias) than such emission from RLQs. For RLQs CIV and HeII is often detected, but in no case from a RQQ in our sample. • Different physical origin? Jet interaction vs. Cold accretion? More work needed. • Link to Lyman- blobs?

  11. Summary In the sample of 14 QSOs (3 radio-loud) we detect extended emission from 8 (2 radio-loud). Comparing with the literature on extended emission from radio loud QSOs the extended emission from radio quiet QSOs seems to have a different physical origin. (This is still work in progress - hopefully to be completed this summer) Thanks for your attention

  12. The narrow band filter

  13. NTT 1998 results

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