activity
20002020
most citedMESS (Mass-loss of Evolved StarS), a Herschel Key Program

134 citations · 209 across the 9 of their papers we have counts for

collaborators

9 papers

astro-ph.SR2020★ 2 cited

Current and future development of the photoionization code Cloudy

P. A. M. van Hoof, G. C. Van de Steene, F. Guzmán +3

The gas that is present in the interstellar medium is usually very far removed from (local) thermodynamic equilibrium, and in some cases may also not be in a steady-state equilibri…

astro-ph.SR2014★ 14 cited

Herschel imaging of the dust in the Helix Nebula (NGC 7293)

G. C. Van de Steene, P. A. M. van Hoof, K. M. Exter +19

In our series of papers presenting the Herschel imaging of evolved planetary nebulae, we present images of the dust distribution in the Helix nebula (NGC 7293). Images at 70, 160,…

astro-ph.SR2013★ 14 cited

A Herschel study of NGC 650

P. A. M. van Hoof, G. C. Van de Steene, K. M. Exter +15

As part of the Herschel Guaranteed Time Key Project MESS (Mass loss of Evolved StarS) we have imaged a sample of planetary nebulae. In this paper we present the PACS and SPIRE imag…

astro-ph.SR2010★ 134 cited

MESS (Mass-loss of Evolved StarS), a Herschel Key Program

M. A. T. Groenewegen, C. Waelkens, M. J. Barlow +39

MESS (Mass-loss of Evolved StarS) is a Guaranteed Time Key Program that uses the PACS and SPIRE instruments on board the Herschel Space Observatory to observe a representative samp…

astro-ph2008★ 7 cited

Kinematics and H_2 morphology of the multipolar Post-AGB star IRAS 16594-4656

G. C. Van de Steene, T. Ueta, P. A. M. van Hoof +2

context: The spectrum of IRAS 16594-4656 shows shock excited H_2 emission and collisionally excited emission lines such as[O I],[C I],and [Fe II]. aim: The goal is to determine the…

astro-ph2007★ 22 cited

IRAS08281-4850 and IRAS14325-6428: two A-type post-AGB stars with s-process enrichment

M. Reyniers, G. C. Van de Steene, P. A. M. van Hoof +1

One of the puzzling findings in the study of the chemical evolution of (post-)AGB stars is why very similar stars (in terms of metallicity, spectral type, infrared properties, etc.…