# The list below includes all the published pulsars in globular clusters # with references. # Total number of pulsars: 140, in 26 globular clusters. # Added 3 new pulsars to previous version of this page: M28L, M22A and B # Cluster/ Offset Period (a) dP/dt (a,b) DM Pb x e m2 (c) # Pulsar (arcmin)(ms) (10-20) (cm-3 pc) (days) (s) (solar masses) 47 Tuc (NGC 104) J0023-7204C 1.21 5.75678 -4.9850(6) 24.599(2) i i i i J0024-7204D 0.68 5.35757 -0.3429(7) 24.729(2) i i i i J0024-7205E 0.65 3.53633 +9.8510(6) 24.230(2) 2.25684 1.98184 0.00031 0.18 J0024-7204F 0.19 2.62358 +6.4500(4) 24.379(5) i i i i J0024-7204G 0.29 4.04038 -4.215(2) 24.441(5) i i i i J0024-7204H 0.77 3.21034 -0.183(1) 24.36(3) 2.35770 2.15281 0.07056 0.19 (i) J0024-7204I 0.29 3.48499 -4.587(2) 24.42(2) 0.22979 0.03844 <0.0004 0.015 J0023-7203J 1.00 2.10063 -0.97922(9) 24.5848(9) 0.12066 0.04040 <0.00004 0.024 J0024-7204L 0.14 4.34617 -12.206(4) 24.38(5) i i i i J0023-7205M 1.05 3.67664 -3.844(3) 24.42(2) i i i i J0024-7204N 0.49 3.05395 -2.1870(9) 24.57(2) i i i i J0024-7204O 0.06 2.64334 +3.0354(9) 24.363(10) 0.13597 0.04515 <0.00016 0.025 J0024-7204P * 3.64302 * 24.3 0.1472 0.0380 0.0 0.02 J0024-7204Q 0.98 4.03318 +3.402(2) 24.29(2) 1.18908 1.46221 0.000085 0.21 J0024-7204R * 3.48046 * 24.4 0.0662 0.0334 0.0 0.030 J0024-7204S 0.19 2.83041 -12.054(2) 24.353(9) 1.20172 0.76627 0.00039 0.10 J0024-7204T 0.34 7.58848 +29.37(1) 24.39(6) 1.12618 1.33850 0.00040 0.20 J0024-7203U 0.94 4.34283 +9.523(1) 24.335(4) 0.42911 0.52695 0.00015 0.14 J0024-7204V * 4.810 * 24.1 0.227 0.85 0.0 * J0024-7204W 0.08 2.35234 * 24.3 0.1330 0.2435 0.0 0.14 J0024-7204X * 4.771 * 24.0 * * * * J0024-7204Y * 2.19666(g) * 24.2 0.52194 0.67176 0.0 0.16 J0024-7204Z * 4.554(g) * 24.47(1)(g) i i i i NGC 1851 J0514-4002 0.08 4.99058 0.117(14) 52.1489(6) 18.7852 36.2966 0.88798 1.1 (ii) M53 (NGC 5024) B1310+18 * 33.1632 * 24.0(1.5) 255.8 84.2 <0.01 0.35 M3 (NGC 5272) J1342+2822A * 2.545 * 26.5 * * * * J1342+2822B 0.14 2.389 +1.858 26.148(2) 1.41735 1.8756 0.0 0.21 J1342+2822C * 2.166 * 26.5 * * * * J1342+2822D 0.23 5.443 * 26.34(2) 128.752 38.524 0.0753 0.21 M5 (NGC 5904) B1516+02A 0.50 5.55359 +4.122(6) 30.08(5) i i i i B1516+02B 0.30 7.94694 -0.33(3) 29.47(11) 6.85845 3.04859 0.13784 0.13 (iii) J1518+0204C * 2.484 * 29.3 0.087 0.057 0.0 0.04 J1518+0204D * 2.988 * 29.3 1.22 1.6 0.0 0.2 J1518+0204E * 3.182 * 29.3 1.10 1.2 0.0 0.18 M4 (NGC 6121) B1620-26 0.767 11.0758 -5.4693(3) 62.8633(5) 191.443 64.8095 0.02532 0.33 M13 (NGC 6205) B1639+36A * 10.3775 <4.5 30.36(4) i i i i B1639+36B * 3.52807 * 29.5(1.5) 1.25911 1.389 <0.001 0.19 J1641+3627C * 3.722 * 30.1 i i i i J1641+3627D * 3.118 * 30.6 0.591 0.92 0.0 0.21 J1641+3627E * 2.487 * 30.3 0.213 0.17 0.0 0.07 M62 (NGC 6266) J1701-3006A 0.32 5.24157 -13.196(9) 115.03(4) 3.80595 3.48372 0.00000 0.23 J1701-3006B 0.028 3.59385 -34.978(7) 113.44(4) 0.14455 0.25277 <0.00007 0.14 J1701-3006C 0.175 7.61285 -3.189(11) 114.56(7) 0.21500 0.19288 <0.00006 0.08 J1701-3006D * 3.41777 * 114.31(3) 1.11790 0.9880 0.00045 0.14 J1701-3006E * 3.23374 * 113.78(1) 0.15848 0.0701 0.0 0.035 J1701-3006F * 2.294727 * 113.36(5) 0.20549 0.0573 0.0 0.024 NGC 6342 B1718-19 2.3 1004.04 +1.59(2)*10-15 71.0(2) 0.25827 0.3526 <0.005 0.13 NGC 6397 J1740-5340 0.917 3.65033 +16.8(7) 71.8(2) 1.35406 1.65284 <0.0001 0.22 (iv) Terzan 5 J1748-2446A 0.50 11.5632 -3.40(4) 242.1(2) 0.07565 0.11971 0.0 0.10 J1748-2446C 0.17 8.43610 -60.6(4) 237(1) i i i i J1748-2446D * 4.71398 * 243.83 i i i i J1748-2446E * 2.19780 * 236.84 60.06 23.6 0.02 0.25 J1748-2446F * 5.54014 * 239.18 i i i i J1748-2446G * 21.6719 * 237.57 i i i i J1748-2446H * 4.92589 * 238.13 i i i i J1748-2446I * 9.57019 * 238.73 1.328 1.818 0.428 0.24 (v) J1748-2446J * 80.3379 * 234.35 1.102 2.454 0.350 0.39 (vi) J1748-2446K * 2.96965 * 234.81 i i i i J1748-2446L * 2.24470 * 237.74 i i i i J1748-2446M * 3.56957 * 238.65 0.4431 0.596 0 0.16 J1748-2446N * 8.66690 * 238.47 0.3855 1.619 0.000045 0.56 J1748-2446O * 1.67663 * 236.38 0.2595 0.112 0 0.04 J1748-2446P * 1.72862 * 238.79 0.3626 1.272 0 0.44 J1748-2446Q * 2.812 * 234.50 30.295 28.602 0.722 0.53 J1748-2446R * 5.02854 * 237.60 i i i i J1748-2446S * 6.11664 * 236.26 i i i i J1748-2446T * 7.08491 * 237.70 i i i i J1748-2446U * 3.28914 * 235.46 3.57026 5.97248 0.60498 0.45 J1748-2446V * 2.07251 * 239.11 0.5036 0.567 0 0.14 J1748-2446W * 4.20518 * 239.14 4.877 5.869 0.015 0.34 J1748-2446X * 2.99926 * 240.03 4.99850 5.1071 0.3024 0.29 J1748-2446Y * 2.04816 * 239.11 1.17 1.16 0 0.16 J1748-2446Z * 2.46259 * 238.85 3.48807 3.5304 0.7608 0.25 (g) J1748-2446aa * 5.78804 * 237.42 i i i i (g) J1748-2446ab * 5.11971 * 238.34 i i i i (g) J1748-2446ac * 5.08691 * 238.72 i i i i (g) J1748-2446ad * 1.39595 * 235.6 1.09443 1.1028 0 0.16 J1748-2446ae * 3.65859 * 238.75 0.17073 0.0406 0 0.019 J1748-2446af * 3.30434 * 237.34 i i i i (g) J1748-2446ag * 4.44803 * 237.75 i i i i (g) J1748-2446ah * 4.96515 * 237.75 i i i i (g) NGC 6440 B1745-20 0.04 288.603 +0.39933(10)*10-15 219.4(2) i i i i J1748-2021B 0.07 16.7601 -32.913(16) 220.922(11) 20.5500 4.46699 0.57016 0.090 (vii) J1748-2021C 0.45 6.22693 -5.984(16) 226.95(6) i i i i J1748-2021D 0.55 13.4958 58.678(16) 224.98(3) 0.28607 0.3972 0.00 0.14 J1748-2021E 0.13 16.2640 31.24(4) 224.10(4) i i i i J1748-2021F 0.09 3.79363 -1.055(18) 220.43(8) 9.83397 9.49757 0.0531 0.35 NGC 6441 J1750-37A 0.21 111.608 566.1(8) 233.82(3) 17.3343 24.439 0.71243 0.7 (viii) J1750-3703B 0.33 6.07454 1.92(4) 234.391(9) 3.60511 2.8659 0.00404 0.19 J1750-3703C 0.11 26.5687 -99.6(3) 230.67(2) i i i i J1750-3703D 0.05 5.13994 49.28(2) 230.09(17) i i i i NGC 6517 J1801-0857A * 7.176 * 183.0 i i i i J1801-0857B * 28.961 * 182.5 * * * * J1801-0857C * 3.739 * 182.4 i i i i NGC 6539 B1802-07 0.25 23.1009 +47.0(4) 186.38(1) 2.61676 3.92059 0.21206 0.35 (ix) NGC 6522 J1803-30 * 7.101 * 192 i i i i J1803-3002B * 4.397 * 192.6 i i i i J1803-3002C * 5.840 * 194.5 i i i i NGC 6544 J1807-2459A * 3.05945 * 134.0(4) 0.07109 0.01220 0.0 0.010 J1807-2459B * 4.186 * 134 * * * * NGC 6624 B1820-30A 0.05 5.44000 +338.5(1) 86.8(1) i i i i B1820-30B 0.23 378.596 +0.0315(3)*10-15 87.0(1) i i i i J1823-3021C * 405.934 * 87 i i i i J1823-3021D * 3.020 * 86.9 i i i i J1823-3021E * 4.394 * 91.4 i i i i J1823-3021F * 4.850 * 86.7 * * * * M28 (NGC 6626) B1821-24A 0.203 3.05431 +155(7) 120 i i i i J1824-2452B * 6.547 * 119.5 i i i i J1824-2452C * 4.159 * 120.7 8.078 7.356 0.847 0.30 J1824-2452D * 79.832 * 119.5 30.404 24.877 0.776 0.45 J1824-2452E * 5.420 * 119.8 i i i i J1824-2452F * 2.451 * 123.8 i i i i J1824-2452G * 5.909 * 119.4 0.1046 0.0165 0.0 0.011 J1824-2452H * 4.629 * 121.5 0.435 0.7195 0.0 0.20 J1824-2452I * 3.932 * 119.0 0.45941 0.7658 0.0 0.20 J1824-2452J * 4.039 * 119.2 0.0974 0.0250 0.0 0.015 J1824-2452K * 4.461 * 119.8 3.91034 2.6050 0.00152 0.16 J1824-2452L * 4.100 * 119.0 0.22571 0.0570 0.0 0.022 M22 (NGC 6656) J1836-2354A * 3.35434 * 89.1 0.20276 0.0464 0.0 0.020 J1836-2354B * 3.23227 * 93.7 i i i i NGC 6749 J1905+0154A * 3.193 * 193.692(8) 0.81255 0.5886 0.0 0.090 J1905+0154B * 4.968 * 192 * * * * NGC 6752 J1911-5958A 6.39 3.26619 +0.307(10) 33.68(1) 0.83711 1.20605 <0.00001 0.22 (x) J1910-5959B 0.10 8.35780 -79.9(5) 33.28(4) i i i i J1911-6000C 2.70 5.27733 +0.22(7) 33.21(4) i i i i J1910-5959D 0.19 9.03529 +96.3(3) 33.32(5) i i i i J1910-5959E 0.13 4.57177 -43.7(1) 33.29(5) i i i i NGC 6760 J1911+0102A 0.42 3.61852 -0.658 202.678(3) 0.140996 0.03766 <0.00013 0.020 J1911+0101B 0.12 5.38432 -0.2 196.69(2) i i i i M71 (NGC 6838) J1953+1846A * 4.888 * 117 0.1766 0.0782 0.0 0.032 M15 (NGC 7078) B2127+11A 0.018 110.665 -2107(3) 67.31(5) i i i i B2127+11B 0.079 56.1330 +956(6) 67.69(12) i i i i B2127+11C 0.944 30.5293 +499.1(2.5) 67.13(5) 0.33528 2.5183 0.68139 1.13 (xi) B2127+11D 0.019 4.80280 -107.5(1.2) 67.28(21) i i i i B2127+11E 0.135 4.65144 +17.8(7) 66.51(12) i i i i B2127+11F 0.279 4.02704 +3.2(8) 65.52(15) i i i i B2127+11G 0.106 37.6602 +195(45) 66.43(24) i i i i B2127+11H 0.038 6.74339 +2.4(1.3) 67.15(12) i i i i M30 (NGC 7099) J2140-2310A 0.067 11.0193 -5.181(20) 25.0640(41) 0.17399 0.23494 <0.00012 0.11 J2140-2310B * 13.0 * 25.09(0.12) >0.8 >0.1 >0.52 >0.02 Notes: Pulsar names are as indicated in the latest literature. If there is no available position, the name will refer, by default, to the coordinates of the centre of the cluster. The new ATNF pulsar catalogue retains such names even if, after finding a timing solution, the pulsar's position is found to be different. Pulsars 47 Tuc A and B (ajm+89) have never been confirmed. Pulsar 47 Tuc K (mlj+90), was later found to be the third harmonic of 47 Tuc D (rlm+95). Pulsar Ter 5 B (ljm+90) was later renamed PSR J1744-2444 and suspected of not being associated with the cluster (lmbm00). This is confirmed by the DM distribution of the recent discoveries (rhs+05). * - Parameter is still not well determined - this indicates that there is still no published timing/orbital solution. i - Isolated pulsar. (g) Not published elsewhere. (i) The rate of advance of periastron of 47 Tuc H has been measured (fck+03), it is 0.066(1) degrees/year (1-sigma). This implies a total system mass of 1.61(4) solar masses. From this, we can derive m1 < 1.52 and m2 > 0.164 solar masses respectively. The median of the probability for the mass of the pulsar, assuming a flat cos i distribution, is 1.44 solar masses. (ii) The rate of advance of periastron of NGC 1851A has been measured (frg07), it is 0.01289(4) degrees/year (1-sigma). This implies a total system mass of 2.453(14) solar masses. From this, we can derive m1 < 1.5 and m2 > 0.96 solar masses respectively. Furthermore, the median of the expected pulsar masses (assuming a flat cos i distribution) is 1.35 solar masses. (iii) The rate of advance of periastron has been detected for M5 B (awkp97); its value is 0.015 +/- 0.01 degrees per year (this is a 3-sigma uncertainty). To the same 99.72% confidence level, we can say that the total system mass is between 0.45 and 5.5 solar masses. (iv) The mass ratio for PSR J1740-5340 has been measured from spectroscopic measurements of the motion of the companion star (fsg+03) to be m1/m2 = 5.85(13). Assuming a pulsar mass between 1.4 and 1.9 solar masses, this constrains the inclination to be between 47 and 56 degrees. (v) The rate of advance of periastron of Ter 5 I has been measured (rhs+05), it is 0.255(1) degrees/year (1-sigma). This implies a total system mass of 2.17(2) solar masses. From this, we can derive m1 < 1.96 and m2 > 0.24 solar masses respectively. Furthermore, the median of the expected pulsar masses (assuming a flat cos i distribution) is 1.87 solar masses. (vi) The rate of advance of periastron of Ter 5 J has been measured (rhs+05), it is 0.327(4) degrees/year (1-sigma). This implies a total system mass of 2.20(4) solar masses. From this, we can derive m1 < 1.96 and m2 < 0.38 solar masses respectively. The median of the expected pulsar masses (assuming a flat cos i distribution) is 1.73 solar masses. (vii) The rate of advance of periastron of NGC 6440B has been measured (frb+07), it is 0.00391(18) degrees/year (1-sigma). This implies a total system mass of 2.92(20) solar masses. From this, we can derive m1 < 3.24 and m2 > 0.11 solar masses respectively. Furthermore, the median and 1-sigma limits of the expected pulsar mass (assuming a flat cos i distribution) is 2.74 +/- 0.20 solar masses, there is a 1 % chance that the inclination is low enough to make the mass of the pulsar smaller than 2 solar masses. This is by far the largest pulsar mass ever measured. (viii) The rate of advance of periastron of NGC 6441A has been measured (frb+07), it is 0.0055(3) degrees/year (1-sigma). This implies a total system mass of 1.97(15) solar masses. From this, we can derive m1 < 1.65 and m2 > 0.53 solar masses respectively. The medians for the pulsar and companion masses are 1.26 and 0.67 solar masses. Another measurement of the rate of periastron has been published by pcm+06; this yields a total system mass of 2.15 +/- 0.06 solar masses, consistent with the measurement above. (ix) The rate of advance of periastron of PSR B1802-07 has been measured (tamt93), it is 0.060(9) degrees/year (1-sigma). This implies a total system mass of 1.7(4) solar masses. From this, we can derive m1 < 1.7 and m2 < 0.23 solar masses respectively. (x) Further constraints on the masses of the components of this system have been obtained by bkkv06. They obtained the mass ratio from the measured orbital velocity of the white dwarf, it is 7.36+/-0.25. Using mass-radius relations appropriate for low-mass helium-core white dwarfs, they infer m2 = 0.18+/-0.02 solar masses, and m1 = 1.40 +0.16/-0.10 solar masses. If the white-dwarf spectrum and the distance of NGC 6752 are used instead to determine the white-dwarf radius, they find r2 = 0.058+/-0.004 solar radii. For the observed temperature, the mass-radius relations predict a white-dwarf mass of m2 = 0.175+/-0.010 solar masses, constraining the pulsar mass to m1 = 1.34+/-0.08 solar masses. These results are consistend with those of cfpd06. (xi) For the M15 C double neutron star system, the rate of advance of periastron, the relativistic gamma parameter and the orbital decay due to emission of gravitational waves have been measured, this system is now over-determined and represents therefore the first test of GR for a binary system in a globular cluster (jcj+06). The pulsar mass is 1.358 +/- 0.010 solar masses and the companion mass is 1.354 +/- 0.010 solar masses.