Optical-IR Echelle Spectroscopy of NGC 6302

Details Optical-IR Echelle Spectroscopy of NGC 6302 Optical-IR Echelle Spectroscopy of NGC 6302

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002rmxac..12..132c&link_type=abstract

Ionized Gaseous Nebulae, a Conference to Celebrate the 60th Birthdays of Silvia Torres-Peimbert and Manuel Peimbert, Mexico City

Astronomy and Astrophysics

Astronomy

1

Dust, Extinction, Infrared: Ism, Ism: Lines And Bands, Planetary Nebulae: Individual (Ngc 6302)

Scientific paper

Echelle spectroscopy of [Si VI] 1.96 mu m, [Mg VIII] 3.03 mu m, and [Ar VI] 4.53 mu m, using UKIRT+CGS4, shows the line profiles in PN NGC 6302 are singly peaked and unresolved even at R ~ 20 000, with line widths less than 22 kms-1. A photoionized structure is evidenced by spatial and velocity stratification as a function of ionization potential. But a variety of models, with density and T[e] gradients, reproduce the spectrum equally well. Preliminary analysis of the 3000-10000 Å echellogram of NGC 6302, acquired at R ~ 80 000 using VLT+UVES, confirms the stratified nebular structure, but yields intriguing results concerning the line profiles: [Ne V] 3426 Å is broader than [Ne IV] 4723 Å. These observations rule out the existence of an evacuated cavity, or hot bubble, at least on 1'' and 3 km s-1 scales. We do not confirm the broad wings in [Ne V] 3426 Å reported by Meaburn & Walsh (1980).

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