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The shape of Mid-IR PAH bands in the Universe

Published online by Cambridge University Press:  30 March 2011

C. Joblin ,
A.G.G.M. Tielens ,
O. Berné ,
P. Pilleri  and
C. Joblin
O. Berné
Affiliation:
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden,The Netherlands
P. Pilleri
Affiliation:
Université de Toulouse, UPS, CESR, 9 avenue du Colonel Roche, 31028 Toulouse Cedex 4, France CNRS, UMR 5187, 31028 Toulouse, France
C. Joblin
Affiliation:
Université de Toulouse, UPS, CESR, 9 avenue du Colonel Roche, 31028 Toulouse Cedex 4, France CNRS, UMR 5187, 31028 Toulouse, France

Abstract

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A large number of galactic and extragalactic sources exhibit a mid-IR spectrum that isdominated by PAH emission. Looking at these spectra in more details reveals a strongvariability in the shape/position of the observed features, depending on the observedsource, or even the region within a source. In this article, we present the results of ananalysis that has allowed us to decompose these spectra into components having a physicalmeaning. Most, if not all PAH dominated mid-IR spectra of HII regions, PDRs,protoplanetary disks, galaxies etc. can be fitted efficiently using a combination of thesecomponents. The results of these fits provide further insight in the composition of theemitting material and the local physical conditions. In the frame of the future IR spacemissions (JWST, SPICA), this approach can be very useful to probe the physical conditionsin distant galaxies.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 46: PAHs and the Universe: A Symposium to Celebrate the 25th Anniversary of the PAH Hypothesis , 2011 , pp. 49 - 54
Copyright
© EAS, EDP Sciences 2011

References

Berné, O., Joblin, C., Mulas, G., Tielens, A.G.G.M., & Goicoechea, J.R., 2009c, SPICA joint European/Japanese Workshop, July, 2009
Berné, O., Fuente, A., Goicoechea, J.R., et al., 2009b, ApJL, 706, 160 CrossRef
Berné, O., Joblin, C., Fuente, A., & Ménard, F., 2009a, A&A, 495, 827
Berné, O., Joblin, C., Deville, Y., et al., 2007, A&A, 469, 575
Galliano, F., Madden, S.C., Tielens, A.G.G.M., Peeters, E., & Jones, A.P., 2008, ApJ, 679, 310 CrossRef
Hony, S., Van Kerckhoven, C., Peeters, E., et al., 2001, A&A, 370, 1030
Joblin, C., Szczerba, R., Berné, O., Szyszka, C., et al., 2008, A&A, 490, 189
Joblin, C., Tielens, A.G.G.M., Geballe, T.R., & Wooden, D.H. 1996, ApJ, 460, L119
Peeters, E., Hony, S., Van Kerckhoven, C., et al., 2002, A&A, 390, 189
Rapacioli, M., Joblin, C., & Boissel, P., 2005, A&A, 429, 193
Micelotta, E.R., Jones, A.P., & Tielens, A.G.G.M., 2010, A&A, 510, 37
Tielens, , 2008, ARA&A, 46, 289 CrossRef
Tielens, A., 2005 (Cambridge University Press)
Vega, O., Bressan, A., Panuzzo, P., et al., 2010, ApJ, 721, 1090 CrossRef
Werner, M.W., Uchida, K.I., Sellgren, K., et al., 2004, ApJS, 154, 309 CrossRef