Other
Scientific paper
Dec 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.9711t&link_type=abstract
American Astronomical Society, 189th AAS Meeting, #97.11; Bulletin of the American Astronomical Society, Vol. 28, p.1403
Other
1
Scientific paper
We have carried out 3600 - 6800 Angstroms \ long slit echelle spectroscopy of this bipolar nebula at the 2.1-m telescope of Observatorio Astronomico Nacional in San Pedro Martir, Baja California, Mexico. The emission in the lobes is dominated by the Balmer lines; they also show emission in He I, [N II], [N I], [O III], [O II], [O I], [S III], and [S II]. In all emission lines the southern lobe emission is blueshifted while the northern one is redshifted relative to the systemic velocity, typically Delta V ~ 30 km/s between the bright knots separated ~ 40". The condensations appear as intensity maxima with peculiar velocities. The core shows a faint featureless continuum and a very complex emission spectrum. In addition to those lines characteristic of PNe, it exhibits numerous relatively bright emission lines ([Fe II], [Fe III], Si II, [Fe I] and [Ni II]). These lines are also prominent in eta Car and in RR Tel. All the lines are very wide, with a FWHM at least 50 km s(-1) , some lines are as wide as FWHM ~ 100 km s(-1) (Hα has been reported to have extensions up to 1000 km s(-1) , typical of symbiotic stars Balick 1989, AJ 97, 671). The velocity profiles of the core show different unresolved regions with large velocities that are producing the emission. The Balmer lines are double peaked with a dominating red component (Hα , Hβ , Hγ , ... ), some of the high excitation forbidden lines are also double peaked with a dominating {it blue} component ([O III], [Ne III], ...) while others are single peaked (He I 5876, [N II] 6584, [O I] 6300) at the systemic velocity. We derive the physical conditions and chemical compostion of the lobes and the core. We present possible kinematical models of the core emitting region.
Arrieta Anabel
Torres-Peimbert Silvia
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