Sin t

1
INTERNAL KINEMATICS OF MICROSTRUCTURES AND
IMPLICATIONS
Luis F. Miranda
IAA-CSIC
G. Anglada, R. Cesaroni, I. de Gregorio, J.F.
Gómez, Y. Gómez, M.A. Guerrero, J.M. Torrelles,
R. Vázquez

• Precessing outflows
• Collimated ejections from binary central stars
• Water maser emission in planetary nebulae

2
NGC 6884

• Multi-component planetary nebula
• Ellipsoidal shell
• Point-symmetric spiral structures
• Two bipolar knots

The properties of the point-symmetric spirals
agree that the spiral are precessing bipolar
outflows Vexp 55 kms-1 Precession period 475
yr (D 1.9 kpc, Palen et al. 2002)
RNII , GH? , BOIII
HST
Miranda, Guerrero, Torrelles 1999
3
Hu2-1 and IC4846
IC4846 H? HST
Hu2-1 NII HST
Binary central stars
N
The systemic velocity of the bipolar ejections
does not coincide with the systemic velocity of
the nebula Difference 8 - 10 kms-1 Interpretatio
n in terms of a binary star The velocity
difference is related to the orbital velocity
E
2"
N
E
Vsys(jets) -Vsys(shell)
Vorb ? cos i ? cos ?
2"
Orbital parameters Orbital separation lt 30
AU Orbital period lt 100 yr Related to
symbiotic stars?
4
Water maser emission from red giants to planetary
nebulae
?Typical emission from the (spherical) envelope
of red giants and AGB stars (e.g. Elitzur
1992 Habing 1996 Engels 2002)
? W43A AGB star with a precessing bipolar jet
(Imai et al. 2002)
? Detected in proto-planetary nebulae

• IRAS 192962227 (Marvel Boboltz 1998,1999)
• IRAS 16342-3814 (Likkel Morris 1988, Morris et
  al. 2003)
• More cases

? Detected in extremely young planetary nebulae

• K3-35 (Miranda et al. 2001)
• IRAS 17347-3139 (de Gregorio et al. 2003)

5
K3-35
Bipolar planetary nebula (optical size 10")
with an equatorial torus
OI
NII
OI
Strong NII and OIII emission lines HeII 4686
? Teff gt 60000 K
NII
SIII
HeI
H?
SII
Miranda et al. 2003
H?
HeII
OIII
6
K3-35

• Water maser emission in a torus (r ? 85 AU d
  5 kpc) and at the tips of precessing collimated
  outflows (? 5000 AU from the center)
• The jets are probably involved in the excitation
  of the distant water masers
• The 1665 MHz line presents high levels of
  circular polarization (50) ? magnetized torus

(Miranda et al. 2001)
7
K3-35
New VLA observations reveal changes in the water
maser spots ? Changes in region C ? No water
maser at the tips of the jets (3? 7 mJy) The
time difference between the two epochs (2.5 yr)
is too long to make a clear identification of the
same water maser spots ? Proper motions (?) ?
Destruction of the 1999 maser shell and creation
of a new (2002) maser shell (?)
Miranda et al. 2001 ( September 1999) ? de
Gregorio et al. 2003 (May 2002) ?1.3cm continuum
emission peak
(de Gregorio et al. 2003)
8
IRAS 17347-3139
N

• HST (K-band) (Bobrowsky et al. 1999)
• Bipolar nebula 2" x 0.7" , PA -40º
• Water maser emission detected with the Robledo
  70 m antenna (Madrid) (de Gregorio et al. 2003,
  Survey for water maser emission in PNe)

E
1"
The radio continuun emission (1.3 cm-6 cm)
indicates a partially optically thick ionized
nebula (de Gregorio et al. 2003) Teff gt 26000 K
Ne ? 106 cm-3 (D ? 0.8 kpc) Br? and NeII
nebular emission lines (Garcia-Lario, 2003,
private communication)
9
IRAS 17347-3139
VLA observations 2002
1.3
0.6

• 13 water maser spots tracing an ellipse ?
  0.25"?0.12" (PA ? 62)
• If circular ring ? axis tilted ? 60 w.r.t. the
  observer
• The kinematics suggests rotating and expanding
  motions in the ring
• The 1.3cm continuum emission peak (?) does not
  coincide with the center of the ellipse
• Inhomogenities in the (unresolved) ionized
  nebula large beam?
• Binary star?

-0.7
2
0.0
2.6
3.3
-2.7
3.9
-3.3
-1.3
-2.0
-4.0
1"
(De Gregorio et al. 2003)