(PK 334-07.1)
This object (He 3-1312) was classified as possible proto-PN in Supplement
1 (Kohoutek 1978) to CGPN (Perek & Kohoutek
1967) and included among PN in Supplement 4 to CGPN (Kohoutek
1993). It appears in SECGPN (Acker et al. 1992) as SaSt
2-12, PN G 334.8-07.4. There it is of stellar diameter, but recently
Schwarz et al. (1992) found two condensations visible through
filter (and not visible through [OIII] 5007 Å\
filter) having a separation of about 12 arcsec and lying symmetrical to the
centre (to the star). We confirm this observation (Fig. 1 (click here)) and
present the picture of this nebula showing the central object and two
condensations. May be the condensations (Table 3 (click here)) are part of a
faint outer envelope. The higher brightness in the vicinity of the star may
also be an instrumental reflection. The nature of this "faint nebulosity"
near the star cannot be recognized according to our frames.
Figure 1: 
in the light of 
with two
condensations 
(PA 
) apart; exp. 30 s
Besides, belongs to objects where the image is
larger than those of stars, which fact we interpret with the presence of a
nebulosity. This inner nebula of about 
arcsec is very
small, but reliable as we hope; its diameter is nearly the same in (4 frames) and in [OIII] 5007 Å (2 frames).
Rejected from SECGPN as symbiotic star. Our frames show H 2-2
stellar in , but elongated in y direction in [OIII] 5007 Å\
(1.4 arcsec, PA about 
), which may be caused by condensations or
loops (Fig. 2 (click here)).
Figure: H 2-2 in the light of [OIII] 5007 Å elongated in PA ;
exp. 60 s
(PK 332-9.1)
Included among PN in Supplement 5 to CGPN (Kohoutek 1996). It
appears in SECGPN as He 3-1333, PN G 332.9-09.9, stellar appearance. Small optical nebulosity of 
arcsec, PA 
,
was found (Kohoutek 1995) as well as its being nearly identical
with the speckle infrared observations of dust emission features at 
(Roche et al. 1986). This optical nebulosity was now
confirmed using all existing frames.
In SECGPN under 007.2+01.8; optical diameter 5 arcsec from Cahn &
Kaler (1971). The variability of this object (= AS Sgr) is probably
of instrumental origin (Arhipova 1973), the central star is
unknown. Hb 6 has been chosen as a standard nebula in order to compare our
measured dimension with that given in the literature. The derived nebular
diameter (see Table 3 (click here)) is somewhat smaller than that used by Cahn
& Kaler. Besides, the diameter measured in the light of [OIII]
5007 Å\
and in B-system is smaller than that in , which can be
explained by the stratification effect. A large nearly circular halo
(Table 3 (click here)) of about 50 arcsec has been found in .
In SECGPN under 058.3-10.9; optical diameter 1.6 arcsec from Cahn & Kaler (1971). The measured nebular diameter (Table 3 (click here)) of this standard object is again somewhat smaller than that given in the literature.
On the frames the objects MWC 560, MWC 574, 
and HR
Del are somewhat larger than the surrounding stars, but their nebulae, if
any, are extremely small (and the errors large), so that they should be
concidered as uncertain. The most promising of them is with the smallest mean errors. As to HR Del the nebulosity in [OIII]
5007 Å was already reported (see e.g. Kohoutek 1981). For
the year 1995 the nebulosity was expected to be larger than that we
observed, so that we think that our small values are either due to the low
brightness of the nebula relative to the very bright star in the centre,
or that we see only the brightest part of the nebula.