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Analyzing astronomical observations with the NASA Ames PAHdatabase

Published online by Cambridge University Press:  30 March 2011

C. Joblin ,
A.G.G.M. Tielens  and
J. Cami
J. Cami*
Affiliation:
Department of Physics and Astronomy, University of Western Ontario, London, Ontario N6A 3K7, Canada SETI Institute - 189 Bernardo Ave., Suite 100 - Mountain View, CA 94043, USA

Abstract

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We use the NASA Ames Polycyclic Aromatic Hydrocarbon (PAH) infrared spectroscopicdatabase to model infared emission of PAHs following absorption of a UV photon. Wecalculate emission spectra resulting from the full cooling cascade for each species in thedatabase. Using a least squares approach, we can find out what PAH mixtures best reproducea few typical astronomical observations representing the different classes of UIR spectra.We find that we can reproduce the observed UIR spectra in the wavelength range 6–14μm, offering support for the hypothesis that the UIR bands are indeeddue to vibrational modes of PAHs and related molecular species. Spectral decompositions ofour best fit models confirm and reinforce several earlier results: (i)the 6.2 μm band requires a significant contribution ofnitrogen-substituted PAHs (PANHs); (ii) the reported components and theirvariations in the 7.7 μm band are indicative of changes in the sizedistribution of the contributing molecules; (iii) there is a significantcontribution of anions to the 7.7 μm band; (iv) the 11.2μm band is due to large, neutral and pure PAHs; (v)the 11.0 μm band is due to large PAH cations.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 46: PAHs and the Universe: A Symposium to Celebrate the 25thAnniversary of the PAH Hypothesis , 2011 , pp. 117 - 122
Copyright
© EAS, EDP Sciences 2011

References

Allamandola, L.J., Tielens, A.G.G.M., & Barker, J.R., 1989, ApJS, 71, 733 CrossRef
Bauschlicher, C.W., Boersma, C., Ricca, A., et al., 2010, ApJS, 189, 341 CrossRef
d’Hendecourt, L., Léger, A., Boissel, P., & Désert, F., 1989, IAUS, 135, 207
Hudgins, D.M., Bauschlicher, C.W. Jr., & Allamandola, L.J., 2005, ApJ, 632, 316 CrossRef
Pech, C., Joblin, C., & Boissel, P., 2002, A&A, 388, 639 PubMed
Peeters, E., Hony, S., van Kerckhoven, C., et al., 2002, A&A, 390, 1089
Pirali, O., Vervloet, M., Mulas, G., Malloci, G., & Joblin, C., 2009, Phys. Chem. Chem. Phys., 11, 3443 CrossRef
Tielens, A.G.G.M., 2005, The Physics and Chemistry of the Interstellar Medium(Cambridge University Press)
van Diedenhoven, B., Peeters, E., van Kerckhoven, C., et al., 2004, ApJ, 611, 928 CrossRef