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XSHOOTER spectroscopy of the enigmatic PN Lin49 in the SMC

Published online by Cambridge University Press:  08 August 2017

Masaaki Otsuka Open the ORCID record for Masaaki Otsuka [Opens in a new window] ,
Francisca Kemper ,
Marcelo L. Leal-Ferreira ,
Isabel Aleman ,
Jeronimo Bernard-Salas ,
Jan Cami ,
Bram B. Ochsendorf ,
Els Peeters  and
Peter Scicluna
Masaaki Otsuka
Affiliation:
ASIAA, 11F of Astronomy-Mathematics Building, AS/NTU. No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C. email: [email protected] (MO)
Francisca Kemper
Affiliation:
ASIAA, 11F of Astronomy-Mathematics Building, AS/NTU. No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C. email: [email protected] (MO)
Marcelo L. Leal-Ferreira
Affiliation:
Leiden Observatory, University of Leiden, PO Box 9513, 2300 RA, Leiden, The Netherlands
Isabel Aleman
Affiliation:
Leiden Observatory, University of Leiden, PO Box 9513, 2300 RA, Leiden, The Netherlands
Jeronimo Bernard-Salas
Affiliation:
Department of Physical Sciences, The Open Univ., Milton Keynes, MK7 6AA, UK
Jan Cami
Affiliation:
Department of Physics & Astronomy, The Univ. of Western Ontario, London, ON N6A 3K7, Canada SETI Institute, 189 Bernardo Ave, Suite 100, Mountain View, CA 94043, USA
Bram B. Ochsendorf
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
Els Peeters
Affiliation:
Department of Physics & Astronomy, The Univ. of Western Ontario, London, ON N6A 3K7, Canada SETI Institute, 189 Bernardo Ave, Suite 100, Mountain View, CA 94043, USA
Peter Scicluna
Affiliation:
ASIAA, 11F of Astronomy-Mathematics Building, AS/NTU. No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C. email: [email protected] (MO)
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Abstract

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We performed a detailed spectroscopic analysis of the fullerene C60-containing planetary nebula (PN) Lin49 in the Small Magellanic Cloud (SMC). Lin49 is a C-rich and metal-deficient PN (Z~0.0006) and its nebular abundances are in agreement with the AGB model for the initially 1.25 M⊙ stars with the metallicity Z = 0.001. By stellar absorption fitting with TLUSTY, we derived stellar abundances, effective temperature, and surface gravity. We constructed the photoionization model with CLOUDY in order to investigate physical conditions of Lin49. The model with the 0.005-0.1 μm radius graphite and a constant hydrogen density shell could not fit the ~1-5 μm spectral energy distribution (SED) owing to the strong near-IR excess. We propose that the near-IR excess indicates (1) the presence of extremely small carbon molecules or (2) the presence of high-density structure surrounding the central star.

Keywords

infrared: ISMISM: abundancesdustmoleculesplanetary nebulae: individual (Lin49)stars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 254 - 258
Copyright
Copyright © International Astronomical Union 2017 

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