Pulsars in globular clusters

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

Total number of pulsars: 140, in 26 globular clusters. Check Scott Ransom's plot of discoveries per year and globular cluster (eps/png).

Added 3 new pulsars to previous version of this page: M28 L, M22 A and B.

Go to the plots

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)		 Notes References
47 Tuc (NGC 104)
 rc = 0.44 rh = 2.79 rt = 47.25 l = 305.90 b = -44.89 D = 4.5



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) mildly eccentric 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 low-mass mlr+91,rlm+95,fcl+01
J0023-7203J 1.00 2.10063 -0.97922(9) 24.5848(9) 0.12066 0.0404022(2) < 0.00004 0.024 eclipsing, low-mass 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 0.06 2.64334 +3.0354(9) 24.363(10) 0.13597 0.045151(2) < 0.00016 0.025 eclipsing, low-mass clf+00,fcl+01,fck+03
J0024-7204P * 3.64302 * 24.3 0.1472 0.0380 0.0 0.02 low-mass 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 * 3.48046 * 24.4 0.0662 0.0334 0.0 0.030 eclipsing, low-mass 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 * 4.810 * 24.1 0.227(16)(g) 0.85(13)(g) 0.0 ? eclipsing? clf+00
J0024-7204W 0.08 2.35234 * 24.3 0.1330 0.2435 0.0 0.14 eclipsing 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
J0024-7204Z * 4.554 * 24.47(1) i i i i (g)
NGC 1851
 rc = 0.06 rh = 0.52 rt = 11.70 l = 244.51 b = -35.04 D = 12.1



J0514-4002A 0.08 4.99058 0.117(14) 52.1489(6) 18.78518 36.296588(9) 0.8879773(3) 1.1 (ii) eccentric, massive fgri04, frg07
M53 (NGC 5024)
 rc = 0.36 rh = 1.11 rt = 21.75 l = 332.96 b = 79.76 D = 17.8



B1310+18 * 33.1632 * 24.0(1.5) 255.8(6) 84.2(7) 0.01 0.35 long orbit kapw91
M3 (NGC 5272)
 rc = 0.55 rh = 1.12 rt = 38.19 l = 42.41 b = 78.71 D = 10.4



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 * 2.166 * 26.5 * * * * needs confirmation hrs+07
J1342+2822D 0.23(12) 5.443 * 26.34(2) 128.752(5) 38.524(4) 0.0753(5) 0.21 long orbit,
mildly eccentric		 hrs+07
M5 (NGC 5904)
 rc = 0.42 rh = 2.11 rt = 12.07 l = 3.86 b = 46.80 D = 7.5



B1516+02A 0.50 5.55359 +4.122(6) 30.08(5) i i i i awkp97, fwbh08
B1516+02B 0.30 7.94694 -0.3306(12) 29.45(3) 6.85845 3.04856 0.137849(12) 0.13 (iii) mildly eccentric awkp97, fwbh08
J1518+0204C * 2.484 * 29.3 0.087 0.0573 0.0 0.038 eclipsing, low-mass 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 l = 350.97 b = 15.97 D = 2.2



B1620-26 0.767 11.0758 -5.4693(3) 62.8633(5) 191.44281 64.809460(4) 0.02531545(12) 0.33 long orbit, triple
system with planet		 lbb+88,ml88,tat+93,tacl99,srh+03
M13 (NGC 6205)
 rc = 0.78 rh = 1.49 rt = 25.19 l = 59.01 b = 40.91 D = 7.7



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 low-mass, eclipsing? hrs+07
M62 (NGC 6266)
 rc = 0.18 rh = 1.23 rt = 8.97 l = 353.57 b = 7.32 D = 6.9



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 0.028 3.59385 -34.978(7) 113.44(4) 0.14455 0.252775(13) <0.00007 0.14 eclipsing pdm+03
J1701-3006C 0.175 7.61285 -6.378(22) 114.56(7) 0.21500 0.192880(12) < 0.00006 0.08 P, Pdot twice published pdm+03
J1701-3006D * 3.41777 * 114.31(3) 1.11790 0.9880 0.00045(2) 0.14 cha03
J1701-3006E * 3.23374 * 113.78(1) 0.15848 0.0701 0.0 0.035 eclipsing, low-mass cha03
J1701-3006F * 2.294727 * 113.36(5) 0.20549 0.0573 0.0 0.024 low-mass cha03
NGC 6342
 rc = 0.05 rh = 0.88 rt = 14.86 l = 4.90 b = 9.73 D = 8.6



B1718-19 2.3 1004.04 +1.59(2)*10-15 71.0(2) 0.25827 0.3526(8) < 0.005 0.13 eclipsing, slow, young lbhb93,kkk+00
NGC 6397
 rc = 0.05 rh = 2.33 rt = 15.81 l = 338.17 b = -11.96 D = 2.3



J1740-5340 0.917 3.65033 +16.8(7) 71.8(2) 1.35406 1.65284(7) < 0.0001 0.22 (iv) eclipsing dlm+01,dpm+01,fpds01
Terzan 5
 rc = 0.18 rh = 0.83 rt = 9.84 l = 3.84 b = 1.69 D = 10.3



J1748-2446A 0.50 11.5632 -3.40(4) 242.1(2) 0.075646 0.11971(3) 0.0 0.10 eclipsing 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 long orbit 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) eccentric rhs+05
J1748-2446J * 80.3379 * 234.35 1.102 2.454 0.350 0.39 (vi) eccentric 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 * 1.67663 * 236.38 0.2595 0.112 0 0.04 eclipsing, low-mass rhs+05
J1748-2446P * 1.72862 * 238.79 0.3626 1.272 0 0.44 eclipsing rhs+05
J1748-2446Q * 2.812 * 234.50 30.295 28.602 0.722 0.53 eccentric, massive 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 * 3.28914 * 235.46 3.57026 5.97248 0.60498 0.45 eccentric 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 5.1071 0.3024 0.29 eccentric rhs+05
J1748-2446Y * 2.04816 * 239.11 1.16443 1.1785 0.00002 0.16 rhs+05
J1748-2446Z * 2.46259 * 238.85 3.48807 3.5304 0.7608 0.25 eccentric (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 eclipsing, fastest
pulsar known		 hrs+06
J1748-2446ae * 3.65859 * 238.75 0.17073 0.0406 0 0.019 low-mass (g)
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
 rc = 0.13 rh = 0.58 rt = 6.31 l = 7.73 b = 3.80 D = 8.4



B1745-20 0.04 288.603 +0.39933(10)*10-15 219.4(2) i i i i slow, young lmd96,frb+08
J1748-2021B 0.07 16.7601 -32.913(16) 220.922(11) 20.55001 4.46699 0.57016 0.090 (vii) eccentric frb+08
J1748-2021C 0.45 6.22693 -5.984(16) 226.95(6) i i i i frb+08
J1748-2021D 0.55 13.4958 58.678(16) 224.98(3) 0.28607 0.3972 0.00 0.14 eclipsing frb+08
J1748-2021E 0.13 16.2640 31.24(4) 224.10(4) i i i i frb+08
J1748-2021F 0.09 3.79363 -1.055(18) 220.43(8) 9.83397 9.49757 0.0531 0.35 mildly eccentric frb+08
NGC 6441
 rc = 0.11 rh = 0.64 rt = 8.00 l = 353.53 b = -5.01 D = 11.7



J1750-37A 0.21 111.608 566.1(8) 233.82(3) 17.3343 24.439 0.71243 0.7 (viii) eccentric, massive
slow 		pdm+01, frb+08
J1750-3703B 0.33 6.07454 1.92(4) 234.391(9) 3.60511 2.8659 0.00404 0.19 frb+08
J1750-3703C 0.11 26.5687 -99.6(3) 230.67(2) i i i i frb+08
J1750-3703D 0.05 5.13994 49.28(2) 230.09(17) i i i i frb+08
NGC 6517
 rc = 0.06 rh = 0.62 rt = 4.10 l = 19.23 b = 6.76 D = 10.8



J1801-0857A * 7.176 * 183.0 i i i i (g)
J1801-0857B * 28.961 * 182.5 * * * * (g)
J1801-0857C * 3.739 * 182.4 i i i i (g)
NGC 6522
 rc = 0.05 rh = 1.04 rt = 16.44 l = 1.02 b = -3.93 D = 7.8



J1803-30A * 7.101 * 192 i i i i pdm+01
J1803-3002B * 4.397 * 192.6 i i i i (g)
J1803-3002C * 5.840 * 194.5 i i i i (g)
NGC 6539
 rc = 0.54 rh = 1.67 rt = 21.46 l = 20.80 b = 6.78 D = 8.4



B1802-07 0.25 23.1009 +47.0(4) 186.38(1) 2.61676 3.92059(5) 0.21206(2) 0.35 (ix) mildly eccentric dbl+93,tamt93
NGC 6544
 rc = 0.05 rh = 1.77 rt = 2.05 l = 5.84 b = -2.20 D = 2.7



J1807-2459A * 3.05945 * 134.0(4) 0.071092 0.01220(3) 0.0 0.010 low-mass dlm+01,rgh+01
J1807-2459B * 4.186 * 134 * * * * cha03
NGC 6624
 rc = 0.06 rh = 0.82 rt = 20.55 l = 2.79 b = -7.91 D = 7.9



B1820-30A 0.05 5.44000 +338.5(1) 86.8(1) i i i i young MSP bbl+94
B1820-30B 0.23 378.596 +0.0315(3)*10-15 87.0(1) i i i i slow bbl+94
J1823-3021C * 405.934 * 87.0 i i i i slow cha03
J1823-3021D * 3.020 * 86.9 i i i i (g)
J1823-3021E * 4.394 * 91.4 i i i i (g)
J1823-3021F * 4.850 * 86.7 * * * * eclipsing (g)
M28 (NGC 6626)
 rc = 0.24 rh = 1.56 rt = 11.27 l = 7.80 b = -5.58 D = 5.6



B1821-24A 0.203 3.05431 +155(7) 120 i i i i young MSP lbm+87, fbtg88, cb04, rfk+04
J1824-2452B * 6.547 * 119.5 i i i i (g)
J1824-2452C * 4.159 * 120.7 8.078 7.356 0.847 0.30 eccentric (g)
J1824-2452D * 79.832 * 119.5 30.404 24.877 0.776 0.45 young, eccentric (g)
J1824-2452E * 5.420 * 119.8 i i i i (g)
J1824-2452F * 2.451 * 123.8 i i i i (g)
J1824-2452G * 5.909 * 119.4 0.1046 0.0165 0.0 0.011 low-mass (g)
J1824-2452H * 4.629 * 121.5 0.435 0.7195 0.0 0.20 eclipsing (g)
J1824-2452I * 3.93185 * 119.0 0.45941 0.7658 0.0 0.20 eclipsing (g)
J1824-2452J * 4.039 * 119.2 0.0974 0.0250 0.0 0.015 low-mass (g)
J1824-2452K * 4.46105 * 119.8 3.91034 2.6050 0.001524(4) 0.16 (g)
J1824-2452L * 4.10011 * 119.0 0.22571 0.0570 0.0 0.022 low-mass (g)
M22 (NGC 6656)
 rc = 0.77 rh = 1.10 rt = 5.21 l = 9.89 b = -7.55 D = 3.2



J1836-2354A * 3.35434 * 89.1 0.20276 0.0464 0.0 0.020 low-mass (g)
J1836-2354B * 3.23227 * 93.7 i i i i (g)
NGC 6749
 rc = 0.77 rh = 1.10 rt = 5.21 l = 36.20 b = -2.20 D = 7.9



J1905+0154A 0.51(38) 3.193 * 193.692(8) 0.81255 0.58862(4) 0.0 0.090 hrs+07
J1905+0154B * 4.968 * 192 * * * * needs confirmation hrs+07
NGC 6752
 rc = 0.17 rh = 2.34 rt = 55.34 l = 336.49 b = -25.63 D = 4.0



J1911-5958A 6.39 3.26619 +0.307(10) 33.68(1) 0.83711 1.206045(2) < 0.00001 0.22(x) 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 l = 36.11 b = -3.92 D = 7.4



J1911+0102A 0.42 3.61852 -0.658 202.678(3) 0.140996 0.037658(2) <0.00013 0.020 low-mass 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 l = 56.74 b = -4.56 D = 4.0



J1953+1846A * 4.888 * 117 0.1766 0.0782 0.0 0.032 low-mass, eclipsing hrs+07
M15 (NGC 7078)
 rc = 0.07 rh = 1.06 rt = 21.50 l = 65.01 b = -27.31 D = 10.3



B2127+11A 0.018 110.665 -2107(3) 67.31(5) i i i i slow 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 0.944 30.5293 +499.1(2.5) 67.13(5) 0.33528 2.5183(12) 0.681386(16) 1.13(xi) double neutron star,
eccentric		 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 l = 27.18 b = -46.83 D = 8.0



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

l: Galactic longitude (in degrees)

b: Galactic latitude (in degrees)

D: distance (in kpc)

(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.

(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 of M5B has been measured at 0.0142(7) degrees per year (one sigma, see fwbh08). Assuming the periastron advance is fully relativistic, the total binary mass is 2.29 +/- 0.17 M_sun. The maximum pulsar mass is 2.52 solar masses and the minimum companion mass is 0.13 solar masses. The pulsar mass is 2.08+0.18-0.19 solar masses (median and 1-sigma limits). The probability of having a pulsar mass between 1.2 and 1.44 solar masses is 0.77%.

(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+08), 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+08), 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 consistent 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.

Plots
Mass function plotted against orbital period for all the binary pulsars known in the Galactic system. The double neutron star binaries are indicated by the double circles, most of them are in the upper left corner. 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. 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, together with the three Galactic VLMBPs. 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.


Orbital eccentricity versus spin period for all the known binary pulsars. Only one Galactic MSP has an eccentric orbit (PSR J1903+03), all other eccentric binary pulsars with spin periods below 20 ms are in globular clusters. For a similar plot without the pulsar names click here.

The present version of this page was last updated: 2008 August 7
Paulo C. Freire