The mixed chemistry phenomenon in Galactic Bulge PNe

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Volume 495 / No 2 (February IV 2009)

A&A, 495 2 (2009) L5-L8

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Issue		A&A Volume 495, Number 2, February IV 2009


Page(s)		L5 - L8
Section		Letters
DOI		https://doi.org/10.1051/0004-6361:200811457
Published online		20 January 2009

Online Material

Appendix A: Tables

Table A.1: The other Galactic Bulge PNe observed with Spitzer/IRS (program $\char93$ 3633).

Table A.2: The rest of PNe (non-Galactic Bulge) observed within Spitzer/IRS program $\char93$ 3633.

Appendix B: Spectra

$\begin{figure} \par\includegraphics[width=18cm,clip]{1457Fig3.eps} \end{figure}$

Figure B.1:

Spitzer/IRS spectra of Galactic Bulge PNe, which show dual-dust chemistry (see Table 1). The spectral type is shown under name of PN. Note the simultaneous detection of PAH emission features in the 6-14 $\mu$ m range (dashed vertical lines at 6.2, ``7.7'', 8.6 and 11.3 $\mu$ m - right panels) together with crystalline silicate features (dashed vertical lines at 23.5, 27.5 and 33.8 $\mu$ m - left panels).

Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{1457Fig4.eps} \end{figure}$

Figure B.2:

Spitzer/IRS spectra of Galactic Bulge PNe, which show dual-dust chemistry cont. (see Table 1). The spectral type is shown under name of PN; none - means neither [WC] nor wels. Note the simultaneous detection of PAH emission features in the 6-14 $\mu$ m range (dashed vertical lines at 6.2, ``7.7'', 8.6 and 11.3 $\mu$ m - right panels) together with crystalline silicate features (dashed vertical lines at 23.5, 27.5 and 33.8 $\mu$ m - left panels).

Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{1457Fig5.eps} \end{figure}$

Figure B.3:

Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm]{1457Fig6.eps} \end{figure}$

Figure B.4:

Spitzer/IRS spectra of Galactic Bulge PNe, which do not show dual-dust chemistry (see Table A.1). The spectral type is shown under name of PN; none - means neither [WC] nor wels. Dashed vertical lines at 23.5, 27.5 and 33.8 $\mu$ m on the left panels mark position of crystalline silicate bands, while those at 6.2, ``7.7'', 8.6 and 11.3 $\mu$ m on the right panels show position of PAH features.

Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm]{1457Fig7.eps} \end{figure}$	Figure B.5: Spitzer/IRS spectra of PNe, which are classified here as non-Galactic Bulge sources (see Table A.2). The spectral type is shown under name of PN. Dashed vertical lines at 23.5, 27.5 and 33.8 $\mu$ m on the left panels mark position of crystalline silicate bands, while those at 6.2, ``7.7'', 8.6 and 11.3 $\mu$ m on the right panels show position of PAH features.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cmh]{1457Fig8.eps} \end{figure}$

Figure B.6:

Spitzer/IRS spectra of PNe, which are classified here as non-Galactic Bulge sources cont. (see Table A.2). The spectral type is shown under name of PN; none - means neither [WC] nor wels. Dashed vertical lines at 23.5, 27.5, and 33.8 $\mu$ m on the left panels mark position of crystalline silicate bands, while those at 6.2, ``7.7'', 8.6, and 11.3 $\mu$ m on the right panels show position of PAH features.

Open with DEXTER

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