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AGN from the 13H XMM/Chandra deep radio/X-ray survey

AGN from the 13H XMM/Chandra deep radio/X-ray survey. Nick Seymour (SSC) NRAO 17th May. AGN from the 13H XMM/Chandra deep radio/X-ray survey. The 13hr core team: Southampton: Ian McHardy, Katherine Gunn, Derek Moss, Tom Dwelly MSSL: Mat Page, Nicola Loaring, Keith Mason

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AGN from the 13H XMM/Chandra deep radio/X-ray survey

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  1. AGN from the 13H XMM/Chandra deep radio/X-ray survey Nick Seymour (SSC) NRAO 17th May

  2. AGN from the 13H XMM/Chandra deep radio/X-ray survey • The 13hr core team: • Southampton: Ian McHardy, Katherine Gunn, Derek Moss, Tom Dwelly • MSSL: Mat Page, Nicola Loaring, Keith Mason • Liverpool JM: Andy Newsam • USA: Tim Sasseen, Jamie Kennea, France Cordova • Subaru: Kaz Sekiguchi, T. Takata • Spitzer MIPS team: George Rieke et. al. Nick Seymour (SSC) NRAO 17th May

  3. AGN from the 13H XMM/Chandra deep radio/X-ray survey • The 13hr field • Location of UK Rosat deep survey. Lowest Galactic NH • 200ks XMM-Newton • 120ks Chandra mosaic • Deep VLA+MERLIN+GMRT • Deep optical imaging from CFHT + WHT + Subaru • Optical spectroscopy from WHT + CFHT + Keck • Ultra-deep 3.6-170 mm imaging with Spitzer • IR imaging from UKIRT (coming next month)

  4. The 20cm deep radio counts

  5. The 20cm deep radio counts • Sub-mJy up-turn known for 2 decades

  6. The 20cm deep radio counts • Sub-mJy up-turn known for 2 decades • Successfully modeled from star-burst population

  7. The 20cm deep radio counts • Sub-mJy up-turn known for 2 decades • Successfully modeled from star-burst population • Direct evidence is scarce, many faint radio sources remain un-identified (difficult for R ≥ 26)

  8. The 20cm deep radio counts • Sub-mJy up-turn known for 2 decades • Successfully modeled from star-burst population • Direct evidence is scarce, many faint radio sources remain un-identified (difficult for R ≥ 26) • models suggest that AGN may still contribute 20% even at the faintest fluxes

  9. optical morphology/colours AGN/SFG Discrimination

  10. optical morphology/colours AGN/SFG Discrimination

  11. optical morphology/colours AGN/SFG Discrimination

  12. optical morphology/colours AGN/SFG Discrimination 1.4GHz R-band 635MHz i´-band

  13. optical morphology/colours • optical spectra - need high S/N for line diagnostics AGN/SFG Discrimination

  14. optical morphology/colours • optical spectra - need high S/N for line diagnostics • X-ray spectra AGN/SFG Discrimination

  15. Spectra of NELGs • Lots of them are absorbed. • Some are not. • Some absorbed and with reprocessed soft component.

  16. Spectra of NELGs • Lots of them are absorbed. • Some are not. • Some absorbed and with reprocessed soft component.

  17. Spectra of NELGs • Lots of them are absorbed. • Some are not. • Some absorbed and with reprocessed soft component.

  18. Star-forming galaxies? AGN-powered • You can tell the AGN by a combination of properties. • Variable • Power law spectra • Point-like sources • How many sources with L2-10 < 1042 are powered by star formation rather than AGN? Star-powered • Answer is 2. • Both have L2-10 <= 1040 • The ambiguous region of 1040<LX<1042 is almost entirely AGN. Page et al. 2006

  19. optical morphology/colours • optical spectra - need high S/N for line diagnostics • radio morphology (AGN=compact/lobes, SFGs=galaxy sized) • X-ray spectra • radio spectra/morphology (AGN=flat compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep) AGN/SFG Discrimination

  20. HzRGs compared to other radio sources Log(L1.4GHz) [W/Hz] 30µJy detection limit Redshift

  21. HzRGs compared to other radio sources Log(L1.4GHz) [W/Hz] Starburst galaxies? Redshift

  22. HzRGs compared to other radio sources Log(L1.4GHz) [W/Hz] Radio-loud QSOs Redshift

  23. HzRGs compared to other radio sources HzRGs Log(L1.4GHz) [W/Hz] Redshift

  24. HzRGs compared to other radio sources Log(L1.4GHz) [W/Hz] ?? Redshift

  25. optical morphology/colours • optical spectra - need high S/N for line diagnostics • radio morphology (AGN=compact/lobes, SFGs=galaxy sized) • X-ray spectra • radio spectra/morphology (AGN=flay compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep) • Spitzer observations: IRAC for photometric redshifts and MIPS for FIR SED distribution AGN/SFG Discrimination

  26. optical morphology/colours • optical spectra - need high S/N for line diagnostics • radio morphology (AGN=compact/lobes, SFGs=galaxy sized) • X-ray spectra • radio spectra/morphology (AGN=flay compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep) • Spitzer observations: IRAC for photometric redshifts and MIPS for FIR SED distribution: cold reservoir of dust for star-formation and hot dust heated by the AGN. AGN/SFG Discrimination

  27. optical morphology/colours • optical spectra - need high S/N for line diagnostics • radio morphology (AGN=compact/lobes, SFGs=galaxy sized) • X-ray spectra • radio spectra/morphology (AGN=flay compact cores/ultra-steep lobes, SFGs=galaxy sized, moderately steep) • Spitzer observations: IRAC for photometric redshifts and MIPS for FIR SED distribution: cold reservoir of dust for star-formation and hot dust heated by the AGN. Some redshifts available with IRS spectroscopy AGN/SFG Discrimination

  28. Photometric redshifts One faint source with S=120Jy at 20cm R z´ Ks Over an order of magnitude break between R and z´

  29. Photometric redshifts One faint source with S=120Jy at 20cm R z´ Ks Over an order of magnitude break between R and z´, hence either z~1.1 L~1023.5 SFG (v dusty) z~6.4 L~1024.9  AGN (lensed?) Deep(er) J, H, K and IRAC data is in hand

  30. some AGN are radio loud QSOs at z~1-2 • some are hidden in SFGs with L1.4GHz~ 1022-23 W/Hz • low-luminosity counterparts to classical radio galaxies must exist at high-z, but remain to be discovered Conclusions

  31. some AGN are radio loud QSOs at z~1-2 • some are hidden in SFGs with L1.4GHz~ 1022-23 W/Hz • low-luminosity counterparts to classical radio galaxies must exist at high-z, but remain to be discovered • follow-up in X-ray/optical/IR is crucial (and labour intensive) Conclusions

  32. some AGN are radio loud QSOs at z~1-2 • some are hidden in SFGs with L1.4GHz~ 1022-23 W/Hz • low-luminosity counterparts to classical radio galaxies must exist at high-z, but remain to be discovered • follow-up in X-ray/optical/IR is crucial (and labour intensive) • as are wider/deeper radio observations Conclusions

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