Table 3.
Expected DM upper limit on the mean flux density Smin, and maximum possible pseudo-luminosity Lmax for each of the sources.
| Source | DM NE2001 | DM YMW16 | DMs searched | Smin | Lmax |
|---|---|---|---|---|---|
| (pc cm−3) | (pc cm−3) | (pc cm−3) | (mJy) | (mJy kpc2) | |
| G49.2−0.7 |  |
 |
10−400 | 3.1 ± 1.5 | 90 ± 44 |
| G63.7+1.1 |  |
 |
30−400 | 1.2 ± 0.6 | 40 ± 20 |
| G65.3+5.7 | 10.04 ± 2.16 |  |
2−200 | 2.9 ± 1.4 | 2.3 ± 1.1 |
| G74.9+1.2 |  |
 |
2−200 | 1.6 ± 0.8 | 60 ± 29 |
| G93.3+6.9 |  |
 |
10−350 | 0.9 ± 0.5 | 11 ± 6 |
| G141.2+5.0 |  |
 |
30−400 | 0.8 ± 0.4 | 13 ± 6 |
| G150.3+4.5 | ≤180 | ≤260 | 10−400 | 2.2 ± 1.1 | − |
| G189.1+3 |  |
 |
20−400 | 0.8 ± 0.4 | 1.8 ± 0.9 |
Notes. DM models are NE2001 (Cordes & Lazio 2002) and YMW16 (Yao et al. 2017). The errors on the DM are based on distance error (see Table 1). In the case of SNR G150.3+4.5 where no distance is known, the maximum galactic DM for its line of sight is given. The error on LOFAR flux density estimates, and thus on our Smin, is 50%.
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