Issue |
A&A
Volume 410, Number 3, November II 2003
|
|
---|---|---|
Page(s) | 911 - 916 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20031267 | |
Published online | 17 November 2003 |
The kinematics of the most oxygen-poor planetary nebula PN G 135.9+55.9
1
Observatorio Astronómico Nacional, Instituto de Astronomía, UNAM, PO Box 439027, San Diego, CA 92143-9027, USA e-mail: {jal, wsteffen, gag}@astrosen.unam.mx
2
LUTH, Observatoire de Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: grazyna.stasinska@obspm.fr
3
Instituto de Astronomía, UNAM, Apartado Postal 70-264, 04510 México, D.F. México e-mail: jer@astroscu.unam.mx
Corresponding author: M. Richer, richer@astrosen.unam.mx
Received:
16
December
2002
Accepted:
2
August
2003
PN G 135.9+55.9 is a compact, high excitation nebula
that has been identified recently as the most oxygen-poor
halo planetary nebula. Given its very peculiar
characteristics and potential implications in the realms
of stellar and Galactic evolution, additional data are needed to firmly
establish its true nature and evolutionary history. Here we
present the first long-slit, high spectral resolution
observations of this object in the lines of Hα and
λ4686. The position-velocity data
are shown to be compatible with the interpretation
of PN G 135.9+55.9 being a halo planetary nebula.
In both emission lines, we find
the same two velocity components that characterize the
kinematics as that of an expanding elliptical envelope.
The kinematics is consistent with a prolate
ellipsoidal model with axis ratio about 2:1, a radially decreasing
emissivity distribution, a velocity distribution that is radial,
and an expansion velocity of 30 km s-1 for the bulk of the material.
To fit the observed line profiles, this model requires an asymmetric
matter distribution,
with the blue-shifted emission considerably stronger than the
red-shifted emission. We find that the widths of the two velocity
components are substantially wider than those expected due to
thermal motions, but kinematic structure in the projected area
covered by the slit appears
to be sufficient to explain the line widths.
The present data also rule out the possible
presence of an accretion disk in the system that could have
been responsible for a fraction of the Hα flux, further
supporting the planetary nebula nature of PN G 135.9+55.9.
Key words: planetary nebulae: individual: PN G 135.9+55.9, SBS 1150+599A
© ESO, 2003
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