Table 1.
Northern radio-quiet gamma-ray pulsars.
| Pulsar | l | b | P | 10−34Ė | fref | Sref | Ref. |
 |
Nobs | Tsky |
 |
 |
s |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (°) | (°) | (ms) | (erg s−1) | (MHz) | (mJy) | (mJy) | (K) | (h) | (mJy) | ||||
| J0002+6216* | 117.33 | −0.07 | 115.4 | 15.3 | 1400 | 0.022 (detection) | 1,2,9 | ∼0.78 | 9 | 859 | 6.5 | <2.1 | > − 2.1 |
| J0007+7303 | 119.66 | 10.46 | 315.9 | 44.8 | 820 | <0.012 | 3 | <0.18 | 9 | 619 | 5.4 | <1.7 | |
| J0106+4855* | 125.47 | −13.87 | 83.2 | 2.9 | 820 | 0.030 (detection) | 4 | ∼0.45 | 12 | 482 | 10.4 | <1.3 | > − 2.2 |
| J0357+3205 | 162.76 | −16.01 | 444.1 | 0.6 | 327 | <0.043 | 3 | <0.15 | 12 | 374 | 8.9 | <0.8 | |
| J0359+5414 | 148.23 | 0.88 | 79.4 | 131.8 | 1400 | <0.015 | 1,2 | <0.53 | 12 | 716 | 10.5 | <1.7 | |
| J0554+3107 | 179.06 | 2.70 | 465.0 | 5.6 | 1400 | <0.066 | 5 | <2.4 | 11 | 483 | 7.6 | <1.2 | |
| J0622+3749 | 175.88 | 10.96 | 333.2 | 2.7 | 820 | <0.032 | 4 | <0.48 | 7 | 457 | 5.6 | <1.4 | |
| J0631+0646* | 204.68 | −1.24 | 111.0 | 10.4 | 1400 | 0.018 (detection) | 1,2,9 | ∼0.64 | 7 | 641 | 2.0 | <3.2 | > − 2.3 |
| J0633+0632 | 205.09 | −0.93 | 297.4 | 11.9 | 1510 | <0.003 | 3 | <0.12 | 9 | 641 | 2.0 | <2.3 | |
| J1836+5925 | 88.88 | 25.00 | 173.3 | 1.1 | 820 | <0.010 | 3 | <0.15 | 3 | 493 | 2.1 | <2.5 | |
| J1838−0537 | 26.51 | 0.21 | 145.7 | 593.3 | 2000 | <0.009 | 6 | <0.57 | 4 | 4500 | 0.6 | <26 | |
| J1846+0919 | 40.69 | 5.34 | 225.6 | 3.4 | 1510 | <0.004 | 8 | <0.16 | 2 | 1370 | 0.9 | <7.6 | |
| J1906+0722 | 41.22 | 0.03 | 111.5 | 102.2 | 1400 | <0.021 | 7 | <0.75 | 9 | 2830 | 3.0 | <8.0 | |
| J1907+0602* | 40.18 | −0.89 | 106.6 | 282.4 | 1510 | 0.005 (detection) | 10,3 | ∼0.20 | 11 | 2510 | 3.2 | <7.1 | > − 3.1 |
| J1932+1916 | 54.66 | 0.08 | 208.2 | 40.7 | 1400 | <0.075 | 5 | <2.7 | 8 | 1410 | 4.1 | <2.9 | |
| J1954+2836 | 65.24 | 0.38 | 92.7 | 104.8 | 1510 | <0.004 | 8 | <0.16 | 11 | 1150 | 8.2 | <2.1 | |
| J1957+5033 | 84.60 | 11.00 | 374.8 | 0.5 | 820 | <0.025 | 8 | <0.38 | 10 | 613 | 8.6 | <1.3 | |
| J1958+2846 | 65.88 | −0.35 | 290.4 | 34.2 | 1510 | <0.005 | 3 | <0.20 | 12 | 1150 | 8.3 | <2.0 | |
| J2017+3625 | 74.51 | 0.39 | 166.7 | 1.2 | 1510 | <0.005 | 1,2 | <0.20 | 13 | 554 | 8.1 | <1.3 | |
| J2021+4026 | 78.23 | 2.09 | 265.3 | 11.4 | 2000 | <0.011 | 3 | <0.69 | 13 | 2830 | 10.3 | <3.2 | |
| J2028+3332 | 73.36 | −3.01 | 176.7 | 3.5 | 1510 | <0.004 | 4 | <0.16 | 7 | 921 | 5.2 | <1.9 | |
| J2030+4415 | 82.34 | 2.89 | 227.1 | 2.2 | 820 | <0.019 | 4 | <0.29 | 12 | 1420 | 10.1 | <2.2 | |
| J2032+4127* | 80.22 | 1.03 | 143.2 | 36.3 | 2000 | 0.05 (detection) | 11,3 | ∼3.2 | 11 | 1600 | 9.6 | <2.6 | > − 1.5 |
| J2055+2539 | 70.69 | −12.52 | 319.6 | 0.5 | 327 | <0.085 | 8 | <0.30 | 9 | 509 | 5.3 | <1.3 | |
| J2111+4606 | 88.31 | −1.45 | 157.8 | 143.6 | 820 | <0.033 | 4 | <0.50 | 9 | 886 | 7.2 | <1.9 | |
| J2139+4716 | 92.63 | −4.02 | 282.8 | 0.3 | 820 | <0.034 | 4 | <0.52 | 11 | 730 | 9.9 | <1.1 | |
| J2238+5903 | 106.56 | 0.48 | 162.7 | 88.8 | 820 | <0.027 | 3 | <0.41 | 11 | 1080 | 9.7 | <1.9 |
Notes. Column 1: name of the pulsar (pulsars with know radio emission are denoted with *). Columns 2 and 3: Galactic coordinates for each pulsar. Column 4: pulsar period (P). Column 5: spindown luminosity Ė. Columns 6 and 7: observing frequency and measured mean flux density (or upper limit) for the most constraining observation (assuming a spectral index of −1.6). Column 8: Reference (for Cols. 6 and 7). Column 9: flux density (or upper limit) from Cols. 6 and 7 extrapolated to an observing frequency of 150 MHz (using a spectral index of −1.6). Column 10: the number of good observations (usually one hour) used in the final analysis (i.e., with a sufficiently low RFI level). Column 11: sky temperature. Column 12: the equivalent duration of the dataset under the assumption of nominal gain, as given by Eq. (5). Column 13: flux density upper limit at 150 MHz (in the band 110−190 MHz) as determined in this work. Column 14: limit on the spectral index s derived from the most constraining previous detection (Cols. 6 and 7) and our flux density limit (Col. 13).
References. (1) Clark et al. (2017), (2) Wu et al. (2018), (3) Ray et al. (2011), (4) Pletsch et al. (2012b), (5) Pletsch et al. (2013), (6) Pletsch et al. (2012a), (7) Clark et al. (2015), (8) Saz Parkinson et al. (2010), (9) J. Wu (priv. comm.), (10) Abdo et al. (2010), (11) Camilo et al. (2009).
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