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Tracing the coronal emission in AGN with VLT/NACO

Tracing the coronal emission in AGN with VLT/NACO. NACO is here !. Olivier Marco. What is an AGN ?. AGN: a closer view. Scale: << 1 pc. From seeing limited to AO images. An example: NGC1068. 2mass 10”x10”. COME-ON+ 1”x1”. NACO 1”x1” deconvolved. DSS infrared 60”x60”. Yes !

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Tracing the coronal emission in AGN with VLT/NACO

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  1. Tracing the coronal emissionin AGN with VLT/NACO NACO is here ! Olivier Marco

  2. What is an AGN ?

  3. AGN: a closer view Scale: << 1 pc

  4. From seeing limited to AO images An example: NGC1068 2mass 10”x10” COME-ON+ 1”x1” NACO 1”x1” deconvolved DSS infrared 60”x60”

  5. Yes ! But… very red objects & extended Visible-WFS (all IR flux to CONICA) or IR-WFS with 90% flux to WFS… not much left for CONICA (10%)  hard for NB filters & spectroscopy Usually (always ?) self-reference  hard to get a (real) PSF Extended objects  hard to get a sky (even with jittering) So we can we NACO for AGN…

  6. HST & NACO J, Ks combined images Circinus

  7. What/where is the coronal region in an AGN ? • What: region of high density gas where lines of high ionization (IP > 50 eV) species are excited • Where: very close to the ionization source (UV X-ray), BLRNLR & farther away (photoionized by the nuclear continuum or excited by fast (v>300 km/s) shocks) • Coronal lines can be used to directly pinpoint the location of the AGN, and measure a (parsec-scale) size

  8. Ionization Potential vs line width of the forbidden lines • An example: 1H 1934-063 (Sy1) (Rodriguez-Ardilla et al., ApJ 2003)

  9. Why use [Si VII] 2.48 µm ? • Already detected in NGC1068 • Our sample: Circinus, ESO428+G014, NGC3081 • [Si VI] 1.963 µm is contaminated by H21-0 S(3) 1.957 µm • [Si VII] is very strong

  10. NACO images of Circinus Coronal emission shows: • Extended (resolved) emission (10 pc diameter) • Hot dust mixed with CLR & NLR FWHM: 0.12" 2.42 µm continnum [Si VII] 2.48 µm line

  11. Where the CLR spots the true nucleus & the apex of the H cone • Astrometry of [Si VII] vs HST H True color image with HST 8140 Å NACO J & K bands [Si VII] 2.48µm line emission on top of HST H image

  12. NACO images of ESO428 • Coronal region shows: • A bright unresolved peak (size 10 pc) FWHM: 4.3 pixels = 0.12" same on stars into the field & PSF [Si VII] 2.48µm line emission 2.42µm continuum emission

  13. H vs [Si VII] ESO428 NGC3081

  14. More to come… • Survey has 4 objects • but already… 2 objects have shown the possibilities of: • Localization of the central source of the AGN • Measure size of [Si VII]-CLR (limit of NLR) • Trace cone illumination • Relation with luminosity of the central engine? • Fast shocks (v300 km/s) along the radio jet?

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