Gemini and Subaru Observations of Planetary Nebulae and Proto- - - PowerPoint PPT Presentation

Gemini and Subaru Observations

• f Planetary Nebulae and Proto-

Planetary Nebulae

in search for answers to questions on morphological transformation and chemical synthesis

Sun Kwok May 19, 2009

Origin of planetary nebulae

• PN are the result of dynamical interaction

between the remnant of the AGB wind and a newly developed fast wind

• The interacting winds model has

successfully predicted (i) the optical halo; (ii) fast wind (by IUE); (iii) dust envelopes (IRAS); and the X-ray bubble (ROSAT, Chandra)

NGC 6578 NGC 6629 NGC 5979 NGC 5882 NGC 2022

Shells, Rims, Crowns, and Haloes Multi-shell morphology can be explained by 1-D interacting winds dynamics

Morphological transformation to Bipolar Nebulae

NGC 6302 Eastern lobe NGC 2346 Confined by dust torus?

Many well-known PN, such as the Ring, the Dumbbell, the Owl, the Eskikmo, NGC 7027, are bipolars.

IC 4406 H2

Ionized (104-106 K), molecular (101- 102 K) and dust (102 K) components

1 10 100

Wavelength (µm)

1 10 100 1000 10000

Flux (10-10 erg s-1 cm-2) BD +30° 3639

Dust continuum b-f continuum

Spitzer MIPS imaging of the dust components

Su et al. 2004

torus Warm dust in lobes AGB remnant NGC 2346

Mid-IR imaging of dust torus

Muthu et al. 2006 Hen 3-401 T-ReCS at Gemini South (10.36,

10.38, 11.66, 12.33, 18.30, 24.56 µm) Subtraction of the 10.38 µm image from the 11.66 µm image gives the distribution of the 11.3 µm AIB feature. Most of the fluxes emitted >30 µm, so at 20 µm we are still seeing warm dust

Shaping occurs early, in the PPN stage

The Walnut Nebula The Water Lily Nebula The Spindle Nebula The Silkworm Nebula The Cotton Candy Nebula

Dust in the torus and in the lobes

IRAS 16594-4656, the Water Lily Nebula

T-ReCS, Gemini South

Edge-on torus

Closed lobes, fast wind yet to break through

Confined by very low temperature dust HST WFPC2 I band: all scattered light HST NICMOS H2

Imaging of edge-on torus in PPN

IRAS 17441-2411, the Silkworm Nebula

Volk and Kwok (2007)

After deconvolution

Equatorial disk as collimating agent

Misaligned by 23 degrees! A precessing outflow? HST I-band image

NGC 6881 (HST [NII], Kwok & Su 2005)

Multipolar Nebula

Gemini T-ReCS

Synthesis of complex organic compounds in post-AGB evolution

• AGB: over 60 gas-phase molecules

including chains and rings

• Late AGB (extreme carbon stars): acetylene
• PPN: aromatics and aliphatics
• PN: strong aromatics

Kwok, Volk & Hrivank 1999, A&A, 350, L35; Kwok, Volk, & Bernath 2001, ApJ, 554, L87; Kwok 2004, Nature, 430, 985; Kwok 2009, ApSS, 319, 5

Aromatic Infrared Bands

Gemini OSCIR

2 4 6 8 10 12 14 16 18 20

Wavelength (µm)

500 1000 1500

λFλ(10-10erg cm-2 s-1 )

NGC 7027

6.2

3.3 7.7 11.3

[NeV] [SiIV] [NeIII] [MgV] 3.3: sp2 C-H stretch 6.2: sp2 C=C stretch 7.7: sp2 C-C stretch 8.6: sp2 =C-H in-plane bend

8.6

11.3: sp2 =C-H out-of-plane bend

12.0 12.7 13.5

Aromatic and aliphatic features in PPN

Observational confirmation of the chemical synthesis history

• When do the carriers of the AIB form?
• When do the transformation from aliphatics

to aromatics occur?

• Narrow-band imaging (Kwok et al. 2001)
• Imaging spectroscopy (Goto et al. 2007)

Aliphatic sidegroups

3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 3.9 4.0

Wavelength (µm)

1.0 2.0 3.0 4.0 5.0 6.0 7.0 8.0

λFλ(10-10erg cm-2 s-1)

21282+5050

3.4 3.462 3.515 3.56

3.40: asym. CH2, CH3 3.46: lone C-H group 3.51: symmetric CH2 3.29: aromatic C-H stretch Keck NIRSPEC

3.29

3.56: aldehydes C-H stretch

Diffraction-limited 3-µm spectroscopy

Subaru IR Camera & Spectrograph with AO 05341: unresolved, 04296: 400-640 AU, 22272: extends to 2000 AU

Goto et al. 2007

100-160 mas

Summary

• High-resolution mid-IR imaging can map
• ut the distribution of “dark matter” in PN

and help understand the origin of bipolar/multipolar morphology

• Imaging spectroscopy can map the

distribution of aromatic/aliphatic organics and help understand the formation of these species