1. DISCUSSION: Symbiotic nebulae and the link with PNe
V1016 Cyg
Romano Corradi
Hugo Schwarz
Hans van Winckel
Romano Corradi
Hugo Schwarz
Hans van Winckel
He 2-147
He 2-104
R Aqr
Mike Bode
Joel Kastner
Adam Frankowski
Claudio Pereira
CH Cyg
BI Cru
HM Sge

2. Symbiotic nebulae are post-PN nebulae
The story from my point of view. I do not know if you recognize the three persons here.
Hans van Winckel and I were Hugo’s students, at the time. He tried to teach us that nebulae around symbiotic stars are nebulae produced by binary systems after they have already produced a PN. At that time, we did not have a strong opinion on this, but we promised ourselves to think about it, and in fact…
1991, ESO Chile…

3. But they are wearing a swimsuit as a hat!!!
They are pre-PN
But they are wearing a swimsuit as a hat!!!
Hans and I meet again in 1994, and concluded that symbiotic nebulae were objects in a phase just prior to the formation of a PN. [but how to trust two guys dressing in such a way?].
However, another years later also Hugo moved to the Canary Islands, and he came back trying convincing us that symbiotic nebulae are post-PN nebulae, this time I would say using sort of ‘religious’ arguments...
1994, Tenerife…

4. 1999, Tenerife… They ARE post-PN nebulae no no, they are…
who is he/she?

5. …just nebulae around symbiotic stars, similar to PNe and often misclassified with them because:
Symbiotic nebulae have high-density ionized cores as young PNe, and similar exciting conditions, thus similar spectra (but also similar to completely different objects, like eta Car!!!)
Symbiotic nebulae are similar to PNe because they are also formed by interacting stellar winds (but the origin of the fast wind is different, as it follows nova-like outbursts)

6. The formation of symbiotic nebulae
red giant
wind 1%
99%
accretion
fast winds from the WD during nova-like eruptions
ionising photons
winds interaction +
photoionisation =
Symbiotic nebulae simulate PN evolution

7. name
core Ne
Ha wings
tot [km s-1]
central absorption
FeII emission
shape
central star
M 2-9
107
11000 
Mz 3
>105
2500 -
He 2-25
107.5
3500 ?
Th 2-B
3000
M 1-91
106.5
extended
O5 + red excess
He 2-428
>1010
135
Hb 12
19W32
K0-M2
Abell 79 F0
Candidate misclassified PNe (Corradi, Mikolajewska & Mahoney eds, 2003, ASP Conf. Ser.)

8. Near-IR diagnostic diagram
Bipolar PNe
PNe
Schmeja & Kimeswenger 2001 A&A 377, L18

9. but….
Hora et al ApJS 124, 195
M 2-9
Strong dust continuum component, no direct evidence of a cool companion