Pulsars in globular clusters

The table below (see ASCII version) includes all the published pulsars in globular clusters with references.

Total number of pulsars: 129, in 24 globular clusters. Check Scott Ransom's plot of discoveries per year.
Of these, 80 have no published timing solutions and two need confirmation.

Added 28 new pulsars to previous version of this page:
   Terzan 5 Z-ah, NGC6440B-E, NGC6441B-D, NGC6522B and C, NGC6624 D-F and M28 B-H.

Plots of mass function versus orbital period

Related sites:


Cluster/Pulsar Offset
(arcmin)		 Period (a)
(ms)		 dP/dt (a,b)
(10-20)		 DM
(cm-3 pc)		 Orbital Period
(days)		 x (s) Eccentricity m2 (c)
(solar masses)		 References
47 Tuc (NGC 104)
 rc = 0.44 rh = 2.79 rt = 47.25





J0023-7204C 1.21 5.75678 -4.9850(6) 24.599(2) i i i i mlj+90,rlm+95
J0024-7204D 0.68 5.35757 -0.3429(7) 24.729(2) i i i i mlr+91,rlm+95
J0024-7205E 0.65 3.53633 +9.8510(6) 24.230(2) 2.25684 1.9818423(8) 0.0003152(9) 0.18 mlr+91,rlm+95,fcl+01
J0024-7204F 0.19 2.62358 +6.4500(4) 24.379(5) i i i i mlr+91,fcl+01
J0024-7204G 0.29 4.04038 -4.215(2) 24.441(5) i i i i mlr+91,fcl+01
J0024-7204H 0.77 3.21034 -0.183(1) 24.36(3) 2.35770 2.152813(3) 0.070560(3) 0.19 (i) mlr+91,fcl+01,fck+03
J0024-7204I 0.29 3.48499 -4.587(2) 24.42(2) 0.22979 0.038447(2) < 0.0004 0.015 mlr+91,rlm+95,fcl+01
J0023-7203J (e) 1.00 2.10063 -0.97922(9) 24.5848(9) 0.12066 0.0404022(2) < 0.00004 0.024 mlr+91,rlm+95,clf+00,fck+03
J0024-7204L 0.14 4.34617 -12.206(4) 24.38(5) i i i i mlr+91,fcl+01
J0023-7205M 1.05 3.67664 -3.844(3) 24.42(2) i i i i mlr+91,fcl+01
J0024-7204N 0.49 3.05395 -2.1870(9) 24.57(2) i i i i rlm+95,fcl+01
J0024-7204O (e) 0.06 2.64334 +3.0354(9) 24.363(10) 0.13597 0.045151(2) < 0.00016 0.025 clf+00,fcl+01,fck+03
J0024-7204P * 3.64302 * 24.3 0.1472 0.0380 0.0 0.02 clf+00
J0024-7204Q 0.98 4.03318 +3.402(2) 24.29(2) 1.18908 1.462209(4) 0.000085(5) 0.21 clf+00,fcl+01
J0024-7204R (e) * 3.48046 * 24.4 0.0662 0.0334 0.0 0.030 clf+00
J0024-7204S 0.19 2.83041 -12.054(2) 24.353(9) 1.20172 0.766270(3) 0.000394(7) 0.10 clf+00,fkl01,fck+03
J0024-7204T 0.34 7.58848 +29.37(1) 24.39(6) 1.12618 1.33850(2) 0.00040(2) 0.20 clf+00,fkl01,fcl+01
J0024-7203U 0.94 4.34283 +9.523(1) 24.335(4) 0.42911 0.526950(1) 0.000149(4) 0.14 clf+00,fcl+01,egh+01
J0024-7204V (e?) * 4.810 * 24.1 0.227(16)(g) 0.85(13)(g) 0.0 ? clf+00
J0024-7204W (e) 0.08 2.35234 * 24.3 0.1330 0.2435 0.0 0.14 clf+00,egc+02,bgb05
J0024-7204X * 4.771 * 24.0(2) * * * * lcf+03
J0024-7204Y * 2.19666(g) * 24.2(1)(g) 0.52194(g) 0.671759(g) 0.0 0.16 lcf+03
NGC 1851
 rc = 0.06 rh = 0.52 rt = 11.70





J0514-4002A 0.08 4.99058 0.117(14) 52.1489(6) 18.78518 36.296588(9) 0.8879773(3) 1.1 (ii) fgri04, frg07
M53 (NGC 5024)
 rc = 0.36 rh = 1.11 rt = 21.75





B1310+18 * 33.1632 * 24.0(1.5) 255.8(6) 84.2(7) < 0.01 0.35 kapw91
M3 (NGC 5272)
 rc = 0.55 rh = 1.12 rt = 38.19





J1342+2822A * 2.545 * 26.5 * * * * hrs+07
J1342+2822B 0.14 2.389 +1.858 26.148(2) 1.41735 1.875655(2) 0.0 0.21 hrs+07
J1342+2822C (f) * 2.166 * 26.5 * * * * hrs+07
J1342+2822D 0.23(12) 5.443 * 26.34(2) 128.752(5) 38.524(4) 0.0753(5) 0.21 hrs+07
M5 (NGC 5904)
 rc = 0.42 rh = 2.11 rt = 12.07





B1516+02A 0.50 5.55359 +4.122(6) 30.08(5) i i i i awkp97
B1516+02B 0.30 7.94694 -0.33(3) 29.47(11) 6.85845 3.04859(7) 0.13784(3) 0.13 (iii) awkp97
J1518+0204C (e) * 2.484 * 29.3 0.087 0.0573 0.0 0.038 hrs+07
J1518+0204D * 2.988 * 29.3 1.22 1.60 0.0 0.20 hrs+07
J1518+0204E * 3.182 * 29.3 1.10 1.15 0.0 0.15 hrs+07
 M4 (NGC 6121)
 rc = 0.83 rh = 3.65 rt = 32.49





B1620-26 0.767 11.0758 -5.4693(3) 62.8633(5) 191.44281 64.809460(4) 0.02531545(12) 0.33 lbb+88,ml88,tat+93,tacl99,srh+03
M13 (NGC 6205)
 rc = 0.78 rh = 1.49 rt = 25.19





B1639+36A * 10.3775 < 4.5 30.36(4) i i i i kapw91
B1639+36B * 3.52807 * 29.5(1.5) 1.25911 1.389(2) < 0.001 0.19 and92
J1641+3627C * 3.722 * 30.1 i i i i hrs+07
J1641+3627D * 3.118 * 30.6 0.591 0.924 0.0 0.18 hrs+07
J1641+3627E * 2.487 * 30.3 0.117(8) 0.037(4) 0.0 0.02 hrs+07
M62 (NGC 6266)
  rc = 0.18 rh = 1.23 rt = 8.97





J1701-3006A 0.32 5.24157 -13.196(9) 115.03(4) 3.80595 3.483724(8) < 0.000004 0.23 dlm+01,pdm+03
J1701-3006B (e) 0.028 3.59385 -34.978(7) 113.44(4) 0.14455 0.252775(13) < 0.00007 0.14 pdm+03
J1701-3006C 0.175 3.80642 -3.189(11) 114.56(7) 0.21500 0.192880(12) < 0.00006 0.08 pdm+03
J1701-3006D * 3.418 * 114.4(3) 1.12 0.98 0.0(?) 0.14 cha03
J1701-3006E (e) * 3.234 * 114.4(3) 0.16 0.07 0.0 0.035 cha03
J1701-3006F * 2.295 * 114.4(3) 0.20 0.05 0.0 0.02 cha03
NGC 6342
 rc = 0.05 rh = 0.88 rt = 14.86





B1718-19 (e) 2.3 1004.04 +1.59(2)*10-15 71.0(2) 0.25827 0.3526(8) < 0.005 0.13 lbhb93,kkk+00
NGC 6397
 rc = 0.05 rh = 2.33 rt = 15.81





J1740-5340 (e) 0.917 3.65033 +16.8(7) 71.8(2) 1.35406 1.65284(7) < 0.0001 0.22 (iv) dlm+01,dpm+01,fpds01
Terzan 5
 rc = 0.18 rh = 0.83 rt = 9.84





J1748-2446A (e) 0.50 11.5632 -3.40(4) 242.1(2) 0.075646 0.11971(3) 0.0 0.10 ljm+90,lmbm00,nat00
J1748-2446C 0.17 8.43610 -60.6(4) 237(1) i i i i lmbm00
J1748-2446D * 4.71398 * 243.83 i i i i ran01,rhs+05
J1748-2446E * 2.19780 * 236.84 60.06 23.6 0.02 0.25 rhs+05
J1748-2446F * 5.54014 * 239.18 i i i i rhs+05
J1748-2446G * 21.6719 * 237.57 i i i i rhs+05
J1748-2446H * 4.92589 * 238.13 i i i i rhs+05
J1748-2446I * 9.57019 * 238.73 1.328 1.818 0.428 0.24 (v) rhs+05
J1748-2446J * 80.3379 * 234.35 1.102 2.454 0.350 0.39 (vi) rhs+05
J1748-2446K * 2.96965 * 234.81 i i i i rhs+05
J1748-2446L * 2.24470 * 237.74 i i i i rhs+05
J1748-2446M * 3.56957 * 238.65 0.4431 0.596 0 0.16 rhs+05
J1748-2446N * 8.66690 * 238.47 0.3855 1.619 0.000045 0.56 rhs+05
J1748-2446O (e) * 1.67663 * 236.38 0.2595 0.112 0 0.04 rhs+05
J1748-2446P (e) * 1.72862 * 238.79 0.3626 1.272 0 0.44 rhs+05
J1748-2446Q * 2.812 * 234.50 30.295 (h) 28.602 (h) 0.722 (h) 0.53 (h) rhs+05
J1748-2446R * 5.02854 * 237.60 i i i i rhs+05
J1748-2446S * 6.11664 * 236.26 i i i i rhs+05
J1748-2446T * 7.08491 * 237.70 i i i i rhs+05
J1748-2446U * 3.289 * 235.50 3.57 (h) 6.14 (h) 0.61 (h) 0.46 (h) rhs+05
J1748-2446V * 2.07251 * 239.11 0.5036 0.567 0 0.14 rhs+05
J1748-2446W * 4.20518 * 239.14 4.877 5.869 0.015 0.34 rhs+05
J1748-2446X * 2.99926 * 240.03 4.99850 (h) 5.1071 (h) 0.3024 (h) 0.29 (h) rhs+05
J1748-2446Y * 2.04816 * 239.11 1.16443 (h) 1.1785 (h) 0.00002 (h) 0.16 (h) rhs+05
J1748-2446Z * 2.46259 * 238.85 3.48807 3.5304 0.7608 0.25 rhs+06 (h)
J1748-2446aa * 5.78804 * 237.42 i i i i rhs+06 (h)
J1748-2446ab * 5.11971 * 238.34 i i i i rhs+06 (h)
J1748-2446ac * 5.08691 * 238.72 i i i i rhs+06 (h)
J1748-2446ad (e) * 1.39595 * 235.6 1.09443 1.1028 0 0.16 hrs+06
J1748-2446ae * 3.65859 * 238.75 0.17073 0.0406 0 0.019 rhs+06 (h)
J1748-2446af * 3.30434 * 237.34 i i i i rhs+06 (h)
J1748-2446ag * 4.44803 * 237.75 i i i i rhs+06 (h)
J1748-2446ah * 4.96515 * 237.75 i i i i rhs+06 (h)
NGC 6440
 rc = 0.13 rh = 0.58 rt = 6.31





B1745-20 0.1 288.603 +0.400(1)*10-15 220(1) i i i i lmd96
J1748-2021B * 16.760 * 221 20.550 4.466 0.570 0.090 rhs+06
J1748-2021C * 6.227 * 227 i i i i rhs+06
J1748-2021D (e) * 13.496 * 225 0.286 0.397 0.00 0.14 rhs+06
J1748-2021E * 16.264 * 224 i i i i rhs+06
NGC 6441
 rc = 0.11 rh = 0.64 rt = 8.00





J1750-37A * 111.609 * 233 17.3 24.4 0.71 0.7 pdm+01
J1750-3703B * 6.074 * 234 3.61 2.85 0.0 0.19 rhs+06
J1750-3703C * 26.569 * 230 i i i i rhs+06
J1750-3703D * 5.140 * 230 i i i i rhs+06
NGC 6522
 rc = 0.05 rh = 1.04 rt = 16.44





J1803-30A * 7.101 * 192 i i i i pdm+01
J1803-3002B * 4.397 * 192.6 i i i i rhs+06
J1803-3002C * 5.840 * 194.5 i i i i rhs+06
NGC 6539
 rc = 0.54 rh = 1.67 rt = 21.46





B1802-07 0.25 23.1009 +47.0(4) 186.38(1) 2.61676 3.92059(5) 0.21206(2) 0.35 (vii) dbl+93,tamt93
NGC 6544
 rc = 0.05 rh = 1.77 rt = 2.05





J1807-2459A * 3.05945 * 134.0(4) 0.071092 0.01220(3) 0.0 0.010 dlm+01,rgh+01
J1807-2459B * 4.186 * 134 * * * * cha03
NGC 6624
 rc = 0.06 rh = 0.82 rt = 20.55





B1820-30A 0.05 5.44000 +338.5(1) 86.8(1) i i i i bbl+94
B1820-30B 0.23 378.596 +0.0315(3)*10-15 87.0(1) i i i i bbl+94
B1820-30C * 405.9 * 87 * * * * cha03
J1823-3021D * 3.020 * 86.9 i i i i rhs+06
J1823-3021E * 4.394 * 91.4 i i i i rhs+06
J1823-3021F (e) * 4.850 * 86.7 * * * * rhs+06
M28 (NGC 6626)
 rc = 0.24 rh = 1.56 rt = 11.27





B1821-24A 0.203 3.05431 +155(7) 120 i i i i lbm+87, fbtg88, cb04, rfk+04
J1824-2452B * 6.547 * 119.5 i i i i rhs+06
J1824-2452C * 4.159 * 120.7 * * * * rhs+06
J1824-2452D * 79.832 * 119.5 * * * * rhs+06
J1824-2452E * 5.420 * 119.8 i i i i rhs+06
J1824-2452F * 2.451 * 123.8 i i i i rhs+06
J1824-2452G * 5.909 * 119.4 0.105 0.017 0.0 0.011 rhs+06
J1824-2452H (e) * 4.629 * 121.5 ~0.4 ~0.7 ~0.0 ~0.17 rhs+06
NGC 6749
 rc = 0.77 rh = 1.10 rt = 5.21





J1905+0154A 0.51(38) 3.193 * 193.692(8) 0.81255 0.58862(4) 0.0 0.090 hrs+07
J1905+0154B (f) * 4.968 * 192 * * * * hrs+07
NGC 6752
 rc = 0.17 rh = 2.34 rt = 55.34





J1911-5958A 6.39 3.26619 +0.307(10) 33.68(1) 0.83711 1.206045(2) < 0.00001 0.22 (viii) dlm+01,dpf+02,bvkh03,fpsd03,bkkv06,cfpd06
J1910-5959B 0.10 8.35780 -79.9(5) 33.28(4) i i i i dpf+02
J1911-6000C 2.70 5.27733 +0.22(7) 33.21(4) i i i i dpf+02
J1910-5959D 0.19 9.03529 +96.3(3) 33.32(5) i i i i dpf+02
J1910-5959E 0.13 4.57177 -43.7(1) 33.29(5) i i i i dpf+02
NGC 6760
 rc = 0.33 rh = 2.18 rt = 12.96





J1911+0102A 0.42 3.61852 -0.658 202.678(3) 0.140996 0.037658(2) < 0.00013 0.020 dma+93,fhn+05
J1911+0101B 0.12 5.38432 -0.2 196.69(2) i i i i fhn+05
M71 (NGC 6838)
 rc = 0.63 rh = 1.65 rt = 8.96





J1954+1847A (e) * 4.888 * 117 0.1766 0.0782 0.0 0.032 hrs+07
M15 (NGC 7078)
 rc = 0.07 rh = 1.06 rt = 21.50





B2127+11A 0.018 110.665 -2107(3) 67.31(5) i i i i wkm+89, and92,jcj+06
B2127+11B 0.079 56.1330 +956(6) 67.69(12) i i i i agk+91,and92,jcj+06
B2127+11C (d) 0.944 30.5293 +499.1(2.5) 67.13(5) 0.33528 2.5183(12) 0.681386(16) 1.13(ix) agk+91,and92,jcj+06
B2127+11D 0.019 4.80280 -107.5(1.2) 67.28(21) i i i i and92
B2127+11E 0.135 4.65144 +17.8(7) 66.51(12) i i i i and92
B2127+11F 0.279 4.02704 +3.2(8) 65.52(15) i i i i and92
B2127+11G 0.106 37.6602 +195(45) 66.43(24) i i i i and92
B2127+11H 0.038 6.74339 +2.4(1.3) 67.15(12) i i i i and92
M30 (NGC 7099)
 rc = 0.06 rh = 1.15 rt = 18.34





J2140-2310A (e) 0.067 11.0193 -5.181(20) 25.0640(41) 0.17399 0.2349416(48) < 0.00012 0.11 rsb+04
J2140-2310B * 13.0 * 25.09(0.12) > 0.8 > 0.1 > 0.52 > 0.02 rsb+04

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.

rc: cluster core radius (in arcmin)

rh: cluster half-mass radius (in arcmin)

rt: cluster tidal radius (in arcmin)

(a) The period and period derivative refer to the epochs indicated in the references.

(b) Unit is 10-20, except where a power of 10 is indicated.

(c) Listed companion masses are calculated assuming a pulsar mass of 1.35 solar masses and an inclination of 60 degrees. For the cases listed below in red there is further information on the masses of the components, that overrules the values listed in the table.

(d) Double neutron star system.

(e) Eclipses were detected for this system at some radio frequency.

(f) Needs to be confirmed.

(g) This parameter has not been published, or presented to this level of precision, anywhere else.

(h) Ransom et al. (2006), in preparation. Data for Terzan 5 U is the most recent estimate (Ingrid Stairs).

(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 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.

(viii) 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.

(ix) 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.

Orbital Plots
Mass function plotted against orbital period for all the binary pulsars known in the Galactic system. The binaries in globular clusters are represented inside 4-pointed stars and named; we highlight those in 47 Tuc with a ``+'' and those in Terzan 5 with a "x" and indicate them only by their letter, we name most of them in the plot below. A black dot inside the symbol indicates a binary pulsar that is known to eclipse at some radio frequency. PSR J0045-7319 is one of these systems, it is not circled because it belongs to the Small Magellanic Cloud. Some double-neutron star systems can be seen in the upper left corner. The inclined lines indicate constant projected semi-major axis x. For a similar plot without the pulsar names, click here.


Same as above, now zooming in the lower left corner. All GC pulsars are now named, we also name the three Galactic VLMBPs are also named. A VLMBP is a binary with f < 3x10-5Msun , these have companions with masses of 0.01-0.03 Msun, and generally present shorter orbital periods than the LMBPs (f > 10-4 Msun). About half of the VLMBPs display eclipses at 1400 MHz, these tend to have a larger mass function than the VLMBPs that are not known to display eclipses at this frequency. For more information on the eclipsing binaries, click here. For a similar plot without the pulsar names, click here.

The present version of this page was last updated: 2007 August 21
Paulo C. Freire