Table 1
144 MHz flux densities (Stokes I and V) of our population.
| Star name | SI (mJy) | SV (mJy) | CPF (%) | Observation start |
|---|---|---|---|---|
| Sig CrB (TZ Crb) | 5.78 | −4.47 | 77.3 | 2018-05-14 20:14:38 |
| BQ CVn | 1.99 | −1.59 | 79.8 | 2014-06-26 12:48:00 |
| FG UMa | 0.47 | 0.37 | 78.7 | 2015-04-25 17:08:00 |
| BF Lyn | 0.82 | 0.63 | 77.2 | 2018-02-13 19:22:21 |
| DM UMa | 2.38 | −1.28 | 53.9 | 2017-10-13 05:47:00 |
| EV Dra | 1.67 | −1.44 | 86.2 | 2016-05-24 20:00:00 |
| DG CVn (GJ3789) | 0.73 | −0.57 | 78.2 | 2018-04-17 19:10:34 |
| EZ Peg | 0.63 | 0.54 | 85.3 | 2016-10-22 16:52:33 |
| BH CVn (HR 5110) | 2.09 | 1.11 | 53.2 | 2019-04-11 19:32:53 |
| WW Dra | 0.5 | −0.35 | 70.6 | 2018-11-30 06:51:00 |
| YY Gem | 1.37 | −0.64 | 46.6 | 2017-10-15 03:00:00 |
| II Peg | 3.49 | 2.43 | 69.6 | 2016-12-20 13:14:47 |
| BD+334462 | 1.45 | −0.77 | 53 | 2018-10-15 16:13:22 |
| FG Cam (HD 61396) | 1.18 | −0.75 | 63.5 | 2019-05-24 10:55:34 |
Notes. The flux uncertainties are typically 0.1 mJy. The Stokes V sign convention is similar to that used in Pulsar observations (van Straten et al. 2010) and opposite of the IAU convention (Hamaker & Bregman 1996). Each observation lasted eight hours. The observation start date is in YYYY-MM-DD format.
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