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Integral Field Spectroscopy of Faint Haloes around Planetary Nebulae

Integral Field Spectroscopy of Faint Haloes around Planetary Nebulae. Probing the mass-loss history at the tip of the AGB. D. Schönberner M. Steffen M. Roth A. Monreal A. Kelz. NGC 6720. (Spitzer Space Telescope ). Outline. Introduction: PN haloes as fossil records of AGB mass loss

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Integral Field Spectroscopy of Faint Haloes around Planetary Nebulae

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  1. Integral Field Spectroscopy ofFaint Haloes around Planetary Nebulae Probing the mass-loss history at the tip of the AGB D. Schönberner M. Steffen M. Roth A. Monreal A. Kelz NGC 6720 (Spitzer Space Telescope)

  2. Outline • Introduction:PN haloes as fossil records of AGB mass loss • Method:Plasma diagnostics with Integral Field Spectroscopy • PN halo observations with PMASObserving statisticsPreliminary results:NGC 3587(PMAS)NGC 6720(PMAS)NGC 3242(VIMOS) • Conclusions & outlook

  3. Mass loss at the tip of the AGB • Strong, dust-driven stellar winds • Enriched by freshly synthesized elements dredged-up from interior • Important contribution to the recycling of matter in galaxies • Short lifetime of high mass loss phases prevents direct detection • Theory of mass loss on the AGB and beyond is highly uncertain • Observational constraints are badly needed 2000 y Structure of AGB star

  4. Are Planetary Nebulae fossil records of the AGB mass loss history ?

  5. Rim Shell A typical double shell PN NGC6826, observed with HST

  6. Rim AGB Halo Shell IFU NGC6826, observed with PMAS A&G camera

  7. Method • Measurement of plasma diagnostic emission lines • Density diagnostics: [OII 3729] / [OII 3727] or [SII 6718] / [SII 6733]a maps ofabsolute electron densities • Temperature diagnostics:([OIII 4960] + [OIII 5007] ) / [OIII 4363][N II]amaps of electron temperatures

  8. { Integral field spectroscopy of PN haloes Radiation-hydrodynamics simulations } • Goals: • Radial density structure aFinal mass loss episode • Temperature, density aType and age of halo • Chemical abundances aNucleosynthesis & dredge-up • Physics of mysterious ring structures within haloes • Detection of new haloes not found by direct imaging

  9. Advantages of Integral Field Spectroscopy • Allows spectroscopic investigation of extremely low surface brightness targets • High sensitivity due to superbinning capability • Spatial information: Slit versus IFU • PMAS: nod & shuffle mode for accurate sky background subtraction • PMAS: large  coverage, good UV sensitivity

  10. Service A buffer run27 run28 (backup) Statistics of PN halo observations with PMAS run23 10-18 Feb 2004 19-23 Feb 2004 18-22 Aug 2004 23-28 Aug 2004 useful night run36 14/15 Mar 2005 poor observing conditions Total: 8 / 23 clouds/humidity, no observations telescope problems

  11. Preliminary results • PMAS: NGC 3578(Owl nebula) • PMAS: NGC 6720(Ring nebula) • VIMOS: NGC 3242(Jupiter´s Ghost) • (NGC 6826)

  12. Conclusions • Integral Field Spectroscopy of faint haloes around Planetary Nebulae is feasible • Line fluxes as low as 5 • 10 –18 erg/cm2/s/arcsec2 can be detected using the nod & shuffle technique even under less than ideal conditions (grey time) • Some interesting new results have already been obtained: temperature gradients within AGB haloes (NGC 3242, NGC 3578) • More PMAS observing time is needed to achieve goals(VIMOS less useful)

  13. Interior structure of an AGB star

  14. NGC 6543 (Cat‘s eye) as seen by HST

  15. Density diagnostics: [OII]

  16. Density diagnostics: [SII]

  17. Temperature diagnostics: [OIII]

  18. Temperature diagnostics: [NII]

  19. Beam Switching — „Nod-Shuffle“ Spectroscopy

  20. Cuillandre et al. 1994, A&A 281, 603 „ Va – et – Vient “

  21. Cuillandre et al. 1994, A&A 281, 603 „ Va – et – Vient “

  22. Cuillandre et al. 1994, A&A 281, 603 „ Va – et – Vient “

  23. Cuillandre et al. 1994, A&A 281, 603 „ Va – et – Vient “

  24. NGC 3587 ([O III], Palomar 5m) Teff = 105 kKL* = 70 L

  25. NGC 3587, PMAS guider image

  26. NGC 3587: Shell NGC 3587: Halo

  27. NGC 3587: radial surface brightness profile (H and [O III]) PMAS data edge of halo Hydro model

  28. Temperature gradient across PN halo: model results

  29. Temperature gradient across PN halo: NGC 3587 Spurious abundance gradient ?

  30. Corresponding PN equilibrium model Flat T-profile

  31. NGC 6720 (H, KPNO 4m) AGB halo? Recombination halo? Teff = 130 kKL* = 500 L

  32. Conventional sky subtraction

  33. Nod & shuffle sky subtraction

  34. Conventional sky subtraction Hg sky line [OIII 4363]

  35. Nod & shuffle sky subtraction Hg sky line [OIII 4363]

  36. Shell inner halo outer halo Radial intensity profile in H Radial density profile from Abel inversion

  37. Shell inner halo [OII 3729]/[OII 3727] ~ 1 outer halo inner halo: ne ~ r-1.5 ? Radial emissivity profile in H

  38. NGC 3242 VIMOS FOV: 54 x 54

  39. NGC 3242: Ring system Corradi et al. 2004

  40. NGC 3242: Ring system Radial temperature increasetowards outer halo! 20300 K 15700 K VIMOS data (Monreal-Ibero et al. 2005)

  41. First Commissioning Results August 2003

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