El presente trabajo se ha enfocado a determinar y entender las condiciones físicas en una variedad de objetos nebulares, prestando particular atención al problema de la determinación de las abundancias químicas. Para este fin, hemos utilizado métodos analíticos en algunos casos, y modelos numéricos de fotoionización en otros. El objetivo general

Based on ISO short-wavelength spectrograph (SWS)+long-wavelength spectrograph (LWS) observations, IRAS 16594-4656 is identified as a new member of the rare class of C-rich proto-planetary nebulae with the 21 μm dust feature in emission. In addition, the major polycyclic aromatic hydrocarbon (PAH) emission bands at 3.3, 6.2, 7.7, 8.6, and 11.3 μm

We present Hα, [N II] lambda6583, [O III] lambda5007 ground-based images, Hubble Space Telescope (HST) (V band) archival images, VLA-A 3.6 cm continuum data, and high-resolution long-slit spectra of the planetary nebula NGC 6884. The VLA and HST images show an extremely knotty and filamentary nebula with an elliptical central structure also

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The basic capabilities of the Wide Field Imager (WFI) were described in a previous Messenger article (No. 93, p. 13; see also Table 1) which also includes a brief account of the contributions by the three participating institutes, namely ESO (Garching and La Silla), the Max-Planck- Institut für Astronomie in Heidelberg, and the Osservatorio

We present ISOCAM and ISOPHOT observations of the galaxy pair NGC 6090. The SED derived from all ISO measurements is typical for strong starbursts which were triggered by the tidal interaction. With ISOCAM observations we could resolve the two nuclei of NGC 6090 separated by 6'' in the MIR. The NE nucleus is the more active one, both in the optical