Spitzer mid-infrared spectroscopic observations of planetary nebulae
We present Spitzer Space Telescope archival mid-infrared (mid-IR) spectroscopy of a sample of 11 planetary nebulae (PNe). The observations, acquired with the Spitzer Infrared Spectrograph (IRS), cover the spectral range 5.2-14.5 μm that includes the H 0-0 S(2) to S(7) rotational emission lines. This...
| Autores: | , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2016 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/376213 |
| Acceso en línea: | http://hdl.handle.net/10261/376213 |
| Access Level: | acceso abierto |
| Palabra clave: | ISM: lines and bands Planetary nebulae: general Planetary nebulae: individual: (M 2-51, NGC 2346, NGC 2440, NGC 2818, NGC 3132, NGC 6072, NGC 6445, NGC 6537, NGC 6720, NGC 6781, NGC 7293 Infrared: general |
| Sumario: | We present Spitzer Space Telescope archival mid-infrared (mid-IR) spectroscopy of a sample of 11 planetary nebulae (PNe). The observations, acquired with the Spitzer Infrared Spectrograph (IRS), cover the spectral range 5.2-14.5 μm that includes the H 0-0 S(2) to S(7) rotational emission lines. This wavelength coverage has allowed us to derive the Boltzmann distribution and calculate the H rotational excitation temperature (T). The derived excitation temperatures have consistent values ≃900 ± 70 K for different sources despite their different structural components. We also report the detection of mid-IR ionic lines of [Ar], [S], and [Ne] in most objects, and polycyclic aromatic hydrocarbon features in a few cases. The decline of the [Ar]/[Ne] line ratio with the stellar effective temperature can be explained either by a true neon enrichment or by high density circumstellar regions of PNe that presumably descend from higher mass progenitor stars. © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. |
|---|