Near-infrared VLT adaptive Near-infrared VLT adaptive optics imaging of optics imaging of

planetary nebulae planetary nebulae

Eric LagadecEric Lagadec(University of Manchester, UK)(University of Manchester, UK)

Main co-workers: Albert Zijlstra (University of Main co-workers: Albert Zijlstra (University of Manchester), Olivier Chesneau (OCA, Grasse), Manchester), Olivier Chesneau (OCA, Grasse),

Mikako Matsuura (NAOJ, Japan), Djamel Mékarnia Mikako Matsuura (NAOJ, Japan), Djamel Mékarnia (OCA, Nice), Jos(OCA, Nice), Joséé A. de Freitas Pacheco (OCA, A. de Freitas Pacheco (OCA,

Nice)Nice) APN4, La Palma, 19/06/2007

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Adaptive optics imaging at the Adaptive optics imaging at the VLTVLT

NACO (Naos-Conica) on UT4 NACO (Naos-Conica) on UT4 8.2m telescope8.2m telescope

Diffraction-limited imaging in the Diffraction-limited imaging in the optical and near-IRoptical and near-IR

Resolution ~ 60 mas (K-L bands)Resolution ~ 60 mas (K-L bands) Field of view from 14”*14” to Field of view from 14”*14” to

56”*56”56”*56”

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Hen 2-113 morphology+ Hen 2-113 morphology+ corecore

Infrared excess in Infrared excess in the resolved (155 the resolved (155 mas) coremas) core

Warm dust (900-Warm dust (900-1000K)1000K)

Similar dust in IRAS Similar dust in IRAS 16342-3814 16342-3814 (Sahai et al. (Sahai et al.

2005)2005) and IRAS and IRAS 18276-1431 18276-1431 (Sanchez (Sanchez Contreras et al. 2007)Contreras et al. 2007)

NACO L’ (3.8 μm) (Lagadec et al. 2006)HST H image (Sahai et al. 2000)

1 ’’

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The post-AGB star Roberts 22The post-AGB star Roberts 22

Near-infrared NACO composite image of Roberts 22 (Lagadec et al. 2007 in preparation, Eso messenger 124-21, 7”*7”)

HST optical image (Sahai et al. 1999)

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Motion of the envelope?Motion of the envelope?

Jets up to 450 Jets up to 450 km.s-1 km.s-1 (Sahai et al. (Sahai et al. 1999)1999)

D=2kpcD=2kpc HST HST

observations 3 observations 3 years beforeyears before

0.1” in 3 yrs0.1” in 3 yrs

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NACO+MIDI observations of NACO+MIDI observations of OH 231.8 OH 231.8

NACO observations of the post-AGB star OH 231.8 (Matsuura, Chesneau et al. (2006) 27”*27”)

See (and listen to!) Olivier Chesneau and Pieter Deroo’s talks!!!

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OH 231.8+3.4: dusty shell or OH 231.8+3.4: dusty shell or disc?disc?

Measurements only with baselines ~ perpendicular to the bipolar lobes

Dusty structure size measured in just one direction

New observations (PI: E. Lagadec) with 4 new baselines just obtained

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First resultsFirst results

Not a disc but rather a flattened shell (Lagadec et al. in preparation)

Visibilities similar to the Symbiotic Star HM Sge (Sacuto et al. 2007)

Gaussian Fit

Equatorial plan

Along the poles

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Interaction with a hot companion?Interaction with a hot companion?

Soker & Livio (2001)

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V HyaV Hya Evolved AGB Evolved AGB

star with high star with high velocity jets velocity jets (~200km.s-1)(~200km.s-1)

Jet orientated Jet orientated East-West East-West (Sahai et (Sahai et

al. 2003 and Hirano et al. 2004)al. 2003 and Hirano et al. 2004)

An AGB star An AGB star caught in the caught in the shaping act?? shaping act??

3.74 μm NACO image of V Hya (Mékarnia et al. in preparation)

More to come when D. More to come when D. MMéékarnia will be back from his karnia will be back from his 13 months stay in Antarctica!13 months stay in Antarctica!

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SummarySummary

Hen 2-113: warm dust (900K) in the coreHen 2-113: warm dust (900K) in the core Roberts 22: complex S-shaped Roberts 22: complex S-shaped

morphology + expansion?morphology + expansion? OH 231.8: Detection of a 25 mas (~40 OH 231.8: Detection of a 25 mas (~40

a.u.) dust corea.u.) dust core V Hya: Spherical at large scales, V Hya: Spherical at large scales,

departure from spherical symmetry at departure from spherical symmetry at scale below 1” (~300 a.u.)scale below 1” (~300 a.u.)

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Muchas Gracias!

Thank you!

Merci!

спасибо !

Trugarez!

Obrigado!

ευχαριστώ !

Kheili mamnun !

Mulţumesc !

a شكرًا

Děkuji !

Dank u!

תודה

Grazie!

Danke!

Tänan!

Mèsi!

ありがとう

Dziękuję!

Tatenda!

Kiitos!

Tankje wol!

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CO observations of V HyaCO observations of V Hya

Hirano et al. (2004)

Schematic geometry of V Hya

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Formation of OH 231.8 +3.4Formation of OH 231.8 +3.4

Soker & Livio (2001)