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Figure 1:
Map of near-infrared brightness (
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Figure 2:
Photometry of the jet in 3C 273 at 0
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Figure 3: Plot of surface brightness per beam along the jet's ridge line, i.e., showing the brightest point per column from Fig. 2. |
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Figure 4:
Normalised cuts through the jet profile at various distances from the quasar at 300 nm (solid line), 620 nm (short dash), 1.6 ![]() ![]() ![]() ![]() |
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Figure 5:
Comparison of hotspot position at optical and radio wavelengths. Greyscale shows the 620 nm image at original resolution, contours show the 1.3 cm radio map at 0
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Figure 6:
Comparison of jet full-width at half the maximum intensity at different wavelengths. The width is determined column by column on the images in
Fig. 2 as the full width at half the maximum
intensity along the column. The bottom panel shows the optical
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Figure 7:
Spectral index maps at 0
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Figure 8:
Run of the spectral indices along the jet at 0
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Figure 9:
Comparison of high-frequency spectral indices with previous observations at 1
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Figure 10: Illustration of the two different spectral fits performed. Model A assumes infrared emission in excess of the cutoff given by the optical-ultraviolet spectral index, while model B assumes an ultraviolet excess above the infrared-optical cutoff. |
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Figure 11: Location of apertures for which spectra are shown in Fig. 12. Locations at local peaks ("knots'') are marked by a line below the image, while locations in inter-knot regions are marked by a line above. |
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Figure 12:
Observed data points with fitted spectra for the points shown in
Fig. 11. To account for the observed
flattening of the spectrum towards the ultraviolet, model A assumes a
contamination in the infrared, so that the cutoff is determined by the
optical-ultraviolet spectral index there, while the cutoff in model B
is determined by the infrared-optical spectral index. Those spectra
which require an artificial high-frequency data point to obtain a fit
result are labelled "cut''; for these, models A and B are
identical, and the artificially obtained value for
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Figure 12: continued. |
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Figure 12: continued. |
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Figure 13: Maps of the cutoff frequency. Grey levels run from 1013 Hz (white) to 1017 Hz (black) with a pseudo-logarithmic stretch as indicated by the greyscale bar. The values fitted in A and B2 are lower limits. As expected, model A bears a closer resemblance to the optical-ultraviolet spectral index map, while model B is dominated by the infrared-optical spectral index map (cf. Fig. 7). Regions H2 and H1 are fitted with a different model HS. |
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Figure 14:
Run of the fitted cutoff frequency
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Figure 15:
Run of the minimum-energy field
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Figure 16:
Map of the bolometric surface brightness assuming isotropic
emissivity. Values range from 1.5 ![]() ![]() ![]() ![]() ![]() |
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Figure 17:
Run of the maximum particle Lorentz factor
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Figure 18:
Map of the maximum particle Lorentz factor
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