figure 7 (ps) (gif): flat (left) and steep (right) tomography images (15 nov 2001)

figure 8 (ps) (gif): C band POLI (top left) and FPOL (top right), L band POLI (bottom left) and FPOL (bottom right) (16 feb 2002)

figure 9 (ps) (gif): tvhueint of depolarization, using 6 cm total intensity as brightness (15 nov 2001)

figure 10 (ps) (gif): tvhueint of rotation measure using L band POLI as brightness (15 nov 2001)

figure 11 (ps): magnetic field orientation using polarization angle difference map between L and C band and computing rotation manually, contours are 6 cm total intensity, all vectors are the same length (15 nov 2001)

figure 12 (eps) (gif): radio (upper left), X-ray (upper right), Halpha (lower left), and IR (lower right) images (16 feb 2002)

figure 13 (ps) (eps): X-ray brightness vs depolarization. The X's are averaged X-ray brightness values in bins which are 45 beam independent data points wide in depolarization. X's placed at median depol value in bins, error bars are RMS of the average X-ray brightness values (15 nov 2001)

figure 14 (ps) (eps): X-ray brightness vs rotation measure. The X's are averaged X-ray brightness values in bins which are 50 beam independent data points wide in rotation measure. X's placed at median depol value in bins, error bars are RMS of the average X-ray brightness values (16 feb 2002)

figure 15 (ps) (eps): angle averaged radial profiles in the north-northeast, northwest, and south at all wavebands (15 nov 2001)

figure 16 (ps) (eps): angle averaged radial profiles in the north-northeast, northwest, and south for X-ray, flat radio, and steep radio (15 nov 2001)

figure 17 (ps) (eps): azimuthal plot from -90 to 90 degrees, error bars plotted every 3 independent data points (2 feb 2002)

proper motion (ps): radio proper motions calculated between 1985 and 1997 (10 oct 2000)

radio C band color image (ps) (gif) (using tvhueint) at best resolution (2.28 x 1.38 arcsec beam), image max=2.6 mJy/bm, off source rms=0.02 mJy/bm, total flux density about 6.1 Jy (10 oct 2000)

radio C band color image (ps) (gif) (using xv) at best resolution (10 oct 2000)

radio C band grayscale image (ps) (gif) at best resolution (10 oct 2000)

ROSAT HRI image (ps) 7.2 arcsec resolution (18 sep 2000)

Halpha image (ps) from Blair, 7.2 arcsec resolution (18 sep 2000)

Halpha image (ps) (gif) from Blair et al. 1991, ApJ, 366, 484 at best resolution (27 nov 2001)

ISO 12 micron image (ps) from Douvion & Lagage (Douvion et al. 2001, A&A, 373, 281) at 7.2 arcsec resolution (18 sep 2000)

northern half of (gif): (from top) steep, -flat, IR, Halpha, X-ray, radio

southern half of (gif): (from top) -flat, X-ray, steep

spectral index plot1 (ps): To show that our spectral index variations are robust. L band brightness vs C band brightness for a flat region in the north (stars) and the steep western ear (boxes). The lines are least-squares fits. (18 sep 2000)

spectral index plot2 (ps): To show that our spectral index variations are robust. log-log plot of L band brightness vs C band brightness for a flat region in the north (stars) and the steep western ear (boxes). The lines are least squares fits. (18 sep 2000)

paper figure 7 (ps): To show that our spectral index variations are robust. log(L band brightness) vs log(C) - log(L) plot of L band brightness vs C band brightness for a flat region in the north (diamonds) and the steep western ear (pluses). The lines are first order least squares fits. The stars are second order least squares fits. (9 feb 2001)

paper figure 5 (ps): One independent measure of spectral index vs. the other with first and second order least squares fits. (9 feb 2001)

L band brightness vs. C band brightness (ps) (9 feb 2001)

spectral index difference between 2 independent measures (before blanking) vs radio intensity (ps) (18 sep 2000 but fixed 15 nov 2001)