Physical Properties of the Very Young PN Hen3-1357 (Stingray Nebula) Based on Multiwavelength Observations

We carried out a detailed analysis of the interesting and important very young planetary nebula (PN) Hen3-1357 (Stingray Nebula) based on a unique data set of optical to far-IR spectra and photometric images. We calculated the abundances of nine elements using collisionally excited lines (CELs) and...

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Bibliographic Details
Published in:The Astrophysical journal 2017-03, Vol.838 (1), p.71
Main Authors: Otsuka, Masaaki, Parthasarathy, M., Tajitsu, A., Hubrig, S.
Format: Article
Language:English
Subjects:
ABUNDANCE
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
ASYMPTOTIC SOLUTIONS
COMPARATIVE EVALUATIONS
Cosmic dust
DETECTION
Dust
dust, extinction
DUSTS
EVOLUTION
INFRARED SPECTRA
Infrared spectroscopy
Ionization
ISM: abundances
MASS
Nuclear fusion
NUCLEOSYNTHESIS
PHOTOIONIZATION
PHYSICAL PROPERTIES
PLANETARY NEBULAE
planetary nebulae: individual (Hen3-1357)
RECOMBINATION
STARS
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Summary:We carried out a detailed analysis of the interesting and important very young planetary nebula (PN) Hen3-1357 (Stingray Nebula) based on a unique data set of optical to far-IR spectra and photometric images. We calculated the abundances of nine elements using collisionally excited lines (CELs) and recombination lines (RLs). The RL C/O ratio indicates that this PN is O-rich, which is also supported by the detection of the broad 9/18 m bands from amorphous silicate grains. The observed elemental abundances can be explained by asymptotic giant branch (AGB) nucleosynthesis models for initially 1-1.5 M stars with Z = 0.008. The Ne overabundance might be due to the enhancement of 22Ne isotope in the He-rich intershell. Using the spectrum of the central star synthesized by Tlusty as the ionization/heating source of the PN, we constructed the self-consistent photoionization model with Cloudy to the observed quantities and derived the gas and dust masses, dust-to-gas mass ratio, and core mass of the central star. About 80% of the total dust mass is from warm-cold dust component beyond ionization front. Comparison with other Galactic PNe indicates that Hen3-1357 is an ordinary amorphous silicate-rich and O-rich gas PN. Among other studied PNe, IC4846 shows many similarities in properties of the PN to Hen3-1357, although their post-AGB evolution is quite different from each other. Further monitoring of observations and comparisons with other PNe such as IC4846 are necessary to understand the evolution of Hen3-1357.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa64d0