Colour-coded Effelsberg 14.7-GHz map of CTB87 at 51 ′′ angular resolution. The unrelated strong source, J2015+371 (l,b = 74 • .87, 1 • .22), was removed from the map. The HPBW is indicated in the lower right corner.

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... and analysed by Kothes et al. (2020). They have angular resolutions of 2 ′ .5 and 1 ′ .2, respectively. We used these maps for TT-plots in combination with the new 14.7-GHz and 17.3-GHz maps. We present results for the combination 10.55 GHz with 14.7 GHz at 1 ′ .2 resolution in Fig. 9 and between 4.75 GHz and 10.55 GHz at 2 ′ .5 resolution in Fig. ...

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... field component along the line-of-sight in the range between 350 µG and 580 µG for the compact component of CTB87 from an analysis of polarisation data. The shift of the cooling breakfrequency to more than 18 GHz, however, reduces the magnetic field strength of the PWN by just 13%, which still implies an unreasonably high magnetic energy (see Fig. 11 of Kothes et al. (2020)), so that any break by synchrotron cooling is expected to occur at a much higher ...

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... note some similarity of the averaged radial halo-intensity of CTB87 with that of the PWN G21.5-0.9 ( Fürst et al. 1988) (Fig. 11), although the halo of G21.5-09 is about 2.3 pc in size and thus much smaller than the CTB87 halo with about 30 pc. G21.5-0.9 has a compact central component, although of different morphology compared to CTB87, and a diffuse centrally Article number, page 5 of 6 A&A proofs: manuscript no. CTB87-Reich ...

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... Fig. 11. Halo profiles of CTB87 and G21.5-0.9 compared with a halo model with constant electron density and radially decreasing magnetic field with B radial /B random = ...

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... of the electron density and the magnetic field strength of the halo of G21.5-0.9 by simple models (their Fig. 6) and concluded that G21.5-0.9 defies the explanation as an expanding synchrotron nebula. A halo model with a constant electron density and a linear decrease of the magnetic field strength from the centre outwards is shown in Fig. 11 for comparison. This is the model with an emissivity profile closest to the observations of G21.5-0.9, although it clearly does not fit the observations well. This is also the case for the halo profile of CTB87, although the electron and magnetic field distributions seems to be even more complex when compared to G21.5-0.9. The halos of ...