Table 3.
Integrated flux densities of NGC 4631.
| Telescope | Frequency | Integrated flux |
|---|---|---|
| [GHz] | density [mJy] | |
| Arecibo 300 m | 0.430 | 3072 ± 95 (a) |
| Arecibo 300 m | 0.835 | 2005 ± 80 (a) |
| Effelsberg 100 m | 1.42 | 1393 ± 140(b) |
| VLA D-configuration | 1.57 (L-band) | 1091 ± 40 |
| Effelsberg 100 m | 2.68 | 790 ± 40 (c) |
| Green Bank 140 ft | 4.75 | 546 ± 30 (d) |
| Effelsberg 100 m | 4.85 | 515 ± 40(e) |
| VLA D-configuration | 5.99 (C-band) | 284 ± 11 |
| Effelsberg 100 m | 8.35 | 310 ± 16 (f) |
| Effelsberg 100 m | 10.55 | 265 ± 12 (g) |
| OVRO 40 m | 10.70 | 255 ± 15 (d) |
| Effelsberg 100 m | 24.50 | 172 ± 15 (h) |
Notes. Values from this paper are marked in bold.
This value overestimates the flux density of the galaxy by roughly 50 mJy, since it includes the flux density of several point sources in the vicinity which we were able to distinguish in the interferometric data.
From Israel & van der Hulst (1983). This value was not taken into account to derive the spectrum of the integrated emission (Sect. 3.3), because it can be replaced by a value obtained with the Effelsberg telescope at higher angular resolution.
The flux densities in the 4.85 GHz Effelsberg map published by Mora & Krause (2013) were underestimated, because the smaller size of their scanned area made it difficult to estimate an accurate baselevel.
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