CNO Abundances in Metal-Rich Environments:Infrared Space ObservatorySpectroscopy of Ionized Gas in M51
Autor: | Richard C. Henry, Evan D. Skillman, Michael Edmunds, Donald R. Garnett, Bernard Pagel |
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Rok vydání: | 2004 |
Předmět: |
Physics
H II region Infrared Analytical chemistry Doubly ionized oxygen Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Photoionization Photodissociation region Spectral line Space and Planetary Science Emission spectrum Spectroscopy Astrophysics::Galaxy Astrophysics |
Zdroj: | The Astronomical Journal. 128:2772-2782 |
ISSN: | 1538-3881 0004-6256 |
DOI: | 10.1086/425883 |
Popis: | We present Infrared Space Observatory (ISO) Long Wavelength Spectrograph observations centered on the H II region CCM 10 in the spiral galaxy M51. We detect several emission lines in this spectrum, including [O I] 63 and 145 μm, [C II] 158 μm, [O III] 88 μm, and [N II] 122 μm, with a significant upper limit on [N III] 57 μm. We use these measurements to estimate abundances for C, N, and O in the interstellar medium in M51. We compare our [O III] 88 μm flux with the flux for [O III] λ5007 obtained from narrowband imaging. The derived 5007 A/88 μm ratio yields an electron temperature Te = 5300 ± 300 K. This temperature agrees with estimates of T[O III] based on photoionization models of CCM 10 with log O/H = -3.2, an abundance that is about a factor of 2 smaller than earlier results for this object derived from photoionization modeling of the visible spectrum. A possible cause for the discrepancy is that the older photoionization models based on CLOUDY predict significantly larger optical emission-line strengths than the current version of CLOUDY at the same metallicity; models with the more recent version are more consistent with the observed spectra of M51 H II region with reduced O/H. Assuming N/O = N+2/O+2, the upper limit for [N ]/[O ] yields log N/O < -0.5, which is consistent with the trend of N/O versus O/H seen in other spiral galaxies. C/O is estimated from the [C ]/[O ] ratio using photodissociation region models constrained by published CO line ratios, [C ]/CO, and [O ] 63 μm/145 μm. With these various constraints on ne and G0, the observed [C ]/[O ] intensity ratio is in good agreeement with that predicted by photodissociation region models with approximately solar abundances. We infer from this that C/O in M51 is consistent with the solar neighborhood value. |
Databáze: | OpenAIRE |
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