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  \begin{figure}
\par\includegraphics[width=8.8cm,clip]{H3453F6.ps}
\end{figure} Figure A.1: Upper left: typical ISSA map with a large scale gradient. Upper right: amplitude of the Fourier Transform of the image on the left. The cross seen here is produced by the left-right and top-bottom flux difference in the image. Lower right: amplitude of the Fourier Transform of the image apodized with a cosine function to minimize the left-right and top-bottom discontinuities. Lower left: power spectrum of the original image (solid line) and of the apodized image (red line). The power spectrum computed with the Median method is also shown (dotted line). It follows almost perfectly the power spectrum of the apodized image.


  \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F7.ps}\\ [4...
...s}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F9.ps}
\end{figure} Figure A.2: Power spectrum of three 60 $\mu $m ISSA maps. The black curve is the power spectrum of the raw ISSA map from which the power spectrum of the noise has been subtracted. The blue curve is the power spectrum (also noise subtracted) of the map from which point sources stronger than 1 Jy in the IRAS point sources catalog were removed. A power law fit of the blue curve (for k < 0.02 arcmin-1) is also shown. The red curve is the difference between the blue curve and the power law fit.


 \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F10.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F12.ps}
\end{figure} Figure A.3: See Fig. A.2.


 \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F13.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F15.ps}
\end{figure} Figure A.4: See Fig. A.2.


 \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F16.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F18.ps}
\end{figure} Figure A.5: See Fig. A.2.


  \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F19.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F21.ps}
\end{figure} Figure A.6: Power spectrum of three 100 $\mu $m ISSA maps. The black curve is the power spectrum of the raw ISSA map from which the power spectrum of the noise has been subtracted. The blue curve is the power spectrum (also noise subtracted) of the map from which point sources stronger than 1 Jy in the IRAS point sources catalog were removed. A power law fit of the blue curve (for k < 0.02 arcmin-1) is also shown. The red curve is the difference between the blue curve and the power law fit.


 \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F22.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F24.ps}
\end{figure} Figure A.7: See Fig. A.6.


 \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F25.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F27.ps}
\end{figure} Figure A.8: See Fig. A.6.


  \begin{figure}
\par\includegraphics[angle=90,width=13.3cm,clip]{H3453F28.ps}\\ [...
...}\\ [4mm]
\includegraphics[angle=90,width=13.3cm,clip]{H3453F30.ps}
\end{figure} Figure A.9: See Fig. A.6.


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