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A Herschel study of NGC 650
van Hoof, P.A.M.; Van de Steene, G.C.; Exter, K.M.; Barlow, M.J.; Ueta, T.; Groenewegen, M.A.T.; Gear, W.K.; Gomez, H.L.; Hargrave, P.C.; Ivison, R.J.; Leeks, S.J.; Lim, T.L.; Olofsson, G.; Polehampton, E.T.; Swinyard, B.M.; Van Winckel, H.; Waelkens, C.; Wesson, R. (2013). A Herschel study of NGC 650. Astron. Astrophys. 560: A7. https://dx.doi.org/10.1051/0004-6361/201221023
In: Astronomy & Astrophysics (Les Ulis). EDP Sciences: Les Ulis. ISSN 0004-6361; e-ISSN 1432-0746, meer
Peer reviewed article  
Beschikbaar in  Auteurs 
Author keywords
    planetary nebulae: individual: NGC 650 / circumstellar matter / dust, extinction / infrared: ISM / ISM: molecules
Auteurs  Top 
  • van Hoof, P.A.M.
  • Van de Steene, G.C.
  • Exter, K.M., meer
  • Barlow, M.J.
  • Ueta, T.
  • Groenewegen, M.A.T.
  • Gear, W.K.
  • Gomez, H.L.
  • Hargrave, P.C.
  • Ivison, R.J.
  • Leeks, S.J.
  • Lim, T.L.
  • Olofsson, G.
  • Polehampton, E.T.
  • Swinyard, B.M.
  • Van Winckel, H.
  • Waelkens, C.
  • Wesson, R.
Abstract
    As part of the Herschel guaranteed time key project Mass loss of Evolved StarS (MESS) we have imaged a sample of planetary nebulae. In this paper we present the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) images of the classical bipolar planetary nebula NGC 650. We used these images to derive a temperature map of the dust. We also constructed a photoionization and dust radiative transfer model using the spectral synthesis code Cloudy. To constrain this model, we used the PACS and SPIRE fluxes and combined them with hitherto unpublished International Ultraviolet Explorer (IUE) and Spitzer InfraRed Spectrograph (IRS) spectra as well as various other data from the literature. A temperature map combined with a photoionization model were used to study various aspects of the central star, the nebula, and in particular the dust grains in the nebula. The central star parameters are determined to be Teff = 208 kK and L = 261 L⊙ assuming a distance of 1200 pc. The stellar temperature is much higher than previously published values. We confirm that the nebula is carbon-rich with a C/O ratio of 2.1. The nebular abundances are typical for a type IIa planetary nebula. With the photoionization model we determined that the grains in the ionized nebula are large (assuming single-sized grains, they would have a radius of 0.15 μm). Most likely these large grains were inherited from the asymptotic giant branch phase. The PACS 70/160 μm temperature map shows evidence of two radiation components heating the grains. The first component is direct emission from the central star, while the second component is diffuse emission from the ionized gas (mainly Lyα). We show that previous suggestions of a photo-dissociation region surrounding the ionized region are incorrect. The neutral material resides in dense clumps inside the ionized region. These may also harbor stochastically heated very small grains in addition to the large grains.
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