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Home All issues Volume 504 / No 3 (September IV 2009) A&A, 504 3 (2009) 945-958 Online Material
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Issue
A&A
Volume 504, Number 3, September IV 2009
Page(s) 945 - 958
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/200911776
Published online 27 May 2009

Online Material

Appendix B: Gaussian profile fits to H$_{\alpha }$ and He I 5875 Å

 \begin{figure} \par\mbox{\includegraphics[angle=-90,width=8cm,clip]{11776A1a.ps}... ....ps}\includegraphics[angle=-90,width=8cm,clip]{11776A1h.ps} } \par \end{figure} Figure B.1:

H$_{\alpha }$ profile from each epoch (102, 131, 160, 208, 240, 273, 475, and 497 days after explosion going left-right from top to bottom). The profiles are decomposed into 2 or more components representing the broad, intermediate and narrow velocity components. Note that in the later spectra only the broad and intermediate components are observed. The parameters of these fits are presented in Table 3.
Open with DEXTER
 \begin{figure} \par\mbox{\includegraphics[angle=-90,width=8cm,clip]{11776A2a.ps}... ...g.ps}\includegraphics[angle=-90,width=8cm,clip]{11776A2h.ps} } \par \end{figure} Figure B.2:

H$_{\alpha }$ profile from each epoch (102, 131,160, 208, 240, 475, 497, and 507 days after explosion going left-right from top to bottom) decomposed into 3 or more components representing the two broad, the intermediate and narrow velocity components. In the later spectra, only the broad and intermediate components are observed. Parameters for these fits are presented in Table 4.
Open with DEXTER

 \begin{figure} \par\mbox{\includegraphics[angle=-90,width=8.25cm,clip]{11776A3a.... ...ps}\includegraphics[angle=-90,width=8.25cm,clip]{11776A3h.ps} } \par\end{figure} Figure B.3:

He I 5875 Å profile from each epoch (102, 131,160, 208, 240, 475, 497, and 507 days after explosion going left-right from top to bottom) decomposed into 3 or more components representing the two broad, the intermediate and narrow velocity components. In the later spectra, only the broad and intermediate components are observed. Parameters for these fits are presented in Table 4.
Open with DEXTER


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