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XSHOOTER spectroscopy of the enigmatic planetary nebula Lin49 in the Small Magellanic Cloud

Otsuka, Masaaki ; Kemper, F ; Leal-Ferreira, M. L ; Aleman, I ; Bernard-Salas, J ; Cami, J ; Ochsendorf, B. B ; Peeters, E ; Scicluna, P

Monthly notices of the Royal Astronomical Society, 2016-10, Vol.462 (1), p.12-34 [Periódico revisado por pares]

London: Oxford University Press

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  • Título:
    XSHOOTER spectroscopy of the enigmatic planetary nebula Lin49 in the Small Magellanic Cloud
  • Autor: Otsuka, Masaaki ; Kemper, F ; Leal-Ferreira, M. L ; Aleman, I ; Bernard-Salas, J ; Cami, J ; Ochsendorf, B. B ; Peeters, E ; Scicluna, P
  • Assuntos: Astrophysics ; Asymptotic properties ; Cosmology ; Density ; Fullerenes ; Graphite ; Magellanic clouds ; Mathematical models ; Nebulae ; Planetary nebulae ; Spectrum analysis ; Star & galaxy formation ; Stars ; Wavelengths
  • É parte de: Monthly notices of the Royal Astronomical Society, 2016-10, Vol.462 (1), p.12-34
  • Notas: ObjectType-Article-1
    SourceType-Scholarly Journals-1
    ObjectType-Feature-2
    content type line 23
  • Descrição: We performed a detailed spectroscopic analysis of the fullerene C60-containing planetary nebula (PN) Lin49 in the Small Magellanic Cloud (SMC) using XSHOOTER at the European Southern Observatory Very Large Telescope and the Spitzer/Infrared Spectrograph instruments. We derived nebular abundances for nine elements. We used tlusty to derive photospheric parameters for the central star. Lin49 is C-rich and metal-deficient PN (Z ∼ 0.0006). The nebular abundances are in good agreement with asymptotic giant branch nucleosynthesis models for stars with initial mass 1.25 M⊙ and metallicity Z = 0.001. Using the tlusty synthetic spectrum of the central star to define the heating and ionizing source, we constructed the photoionization model with cloudy that matches the observed spectral energy distribution (SED) and the line fluxes in the UV to far-IR wavelength ranges simultaneously. We could not fit the ∼1–5 μm SED using a model with 0.005–0.1-μm-sized graphite grains and a constant hydrogen density shell owing to the prominent near-IR excess, while at other wavelengths the model fits the observed values reasonably well. We argue that the near-IR excess might indicate either (1) the presence of very small particles in the form of small carbon clusters, small graphite sheets, or fullerene precursors, or (2) the presence of a high-density structure surrounding the central star. We found that SMC C60 PNe show a near-IR excess component to lesser or greater degree. This suggests that these C60 PNe might maintain a structure nearby their central star.
  • Editor: London: Oxford University Press
  • Idioma: Inglês
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  • Realização: ABCD-USP USP   Logos de Redes Sociais: Freepik

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