Pulsars in globular clusters

The table below (see ASCII version) lists all known pulsars in globular clusters with the original references whenever available. We hope you find it useful. If you do, please footnote the URL in your paper and if possible cite the relevant references. Thanks!

Total number of pulsars: 144, in 28 globular clusters. Check Scott Ransom's plot of discoveries per year and globular cluster (eps/png).

Added 1 new pulsar to previous version of this page: NGC6652A.

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 mc (c)
(M)
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
NGC 5986
rc = 0.63 rh = 1.05 rt = 10.52 l = 337.02 b = 13.27 D = 10.4



J1546−3747A * 2.60567 * 92.17 1.34671 1.3833 0.0 0.18 lr11
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, lfrj12
J1701−3006B 0.028 3.59385 −34.978(7) 113.44(4) 0.14455 0.252775(13) <0.00007 0.14 eclipsing pdm+03, lfrj12
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, lfrj12
J1701−3006D 0.200 3.41777 12.57(24) 114.224(11) 1.11790 0.9880 0.00045(2) 0.14 lfrj12
J1701−3006E 0.111 3.23374 31.03(27) 113.79(2) 0.15848 0.07016 0.0 0.035 eclipsing, low-mass lfrj12
J1701−3006F 0.041 2.294727 22.21(18) 113.29(3) 0.20549 0.0573 0.0 0.024 low-mass lfrj12
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)
J1748−2446ai * 21.22838 * 233.9 0.85088 2.8088 0.4400 0.57 eccentric, massive (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 pdc+05, 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 0.022 7.17561 −51.310(4) 182.56(1) i i i i lrfs11
J1801−0857B 0.022 28.96159 +219.10(5) 182.39(6) 59.83645 33.87545 0.038 0.38 long orbit lrfs11
J1801−0857C 0.057 3.73870 −6.5(2) 182.26(3) i i i i lrfs11
J1801−0857D 1.202 4.22653 +0.69(6) 174.71(9) i i i i lrfs11
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 pdc+05
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 0.07 3.05945 −0.4335(3) 134.0040(6) 0.071091 0.01222 0.0 0.010 low-mass dlm+01,rgh+01, lfrj12
J1807−2500B 0.20 4.18618 8.23245(18) 137.1535(20) 9.95667 28.9204 0.74703 1.47 (x) eccentric, massive lfrj12
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) 86.880(6) i i i i young MSP, gamma-ray detection bbl+94, kbmo05, kni07, faa+11
B1820−30B 0.23 378.596 +0.0315(3)*10−15 87.0(1) i i i i slow, young bbl+94, lfrj12
J1823−3021C 0.134 405.934 +0.2240(25)*10−15 86.88(24) i i i i slow, young lfrj12
J1823−3021D 0.14 3.02006 * 86.8(1.1) i i i i lfrj12
J1823−3021E * 4.394 * 91.4 i i i i lfrj12
J1823−3021F * 4.850 * 86.7 * * * * eclipsing lfrj12
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, gamma-ray detection lbm+87, fbtg88, cb04, rfk+04, bbs+11, jgk+13
J1824−2452B * 6.547 * 119.5 i i i i (g), bbs+11
J1824−2452C * 4.159 * 120.7 8.078 7.356 0.847 0.30 eccentric (g), bbs+11
J1824−2452D * 79.832 * 119.5 30.404 24.877 0.776 0.45 young, eccentric (g), bbs+11
J1824−2452E * 5.420 * 119.8 i i i i (g), bbs+11
J1824−2452F * 2.451 * 123.8 i i i i (g), bbs+11
J1824−2452G * 5.909 * 119.4 0.1046 0.0165 0.0 0.011 low-mass (g), bbs+11
J1824−2452H * 4.629 * 121.5 0.435 0.7195 0.0 0.20 eclipsing (g), bbs+11, pdf+10
J1824−2452I * 3.93185 * 119.0 0.45941 0.7658 0.0 0.20 eclipsing, switches occasionally to accreting X-ray MSP (g), bbs+11, pfb+13
J1824−2452J * 4.039 * 119.2 0.0974 0.0250 0.0 0.015 low-mass (g), bbs+11
J1824−2452K * 4.46105 * 119.8 3.91034 2.6050 0.001524(4) 0.16 (g), bbs+11
J1824−2452L * 4.10011 * 119.0 0.22571 0.0570 0.0 0.022 low-mass (g), bbs+11
NGC 6652
rc = 0.10 rh = 0.48 rt = 6.3 l = 1.53 b = −11.38 D = 10.0



J1835−3259A * 3.889 * 63.35 * * * * drr11
M22 (NGC 6656)
rc = 0.77 rh = 1.10 rt = 5.21 l = 9.89 b = −7.55 D = 3.2



J1836−2354A 0.68 3.35434 +0.2318(3) 89.107(2) 0.20283 0.0464 0.0 0.020 low-mass lrfs11
J1836−2354B 0.21 3.23227 −0.048(6) 93.3(2) i i i i lrfs11
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(xi) dlm+01,dpf+02,bvkh03,fpsd03,bkkv06,cfpd06,fhc+14
J1910−5959B 0.10 8.35780 −79.9(5) 33.28(4) i i i i dpf+02,fhc+14
J1911−6000C 2.70 5.27733 +0.22(7) 33.21(4) i i i i dpf+02,fhc+14
J1910−5959D 0.19 9.03529 +96.3(3) 33.32(5) i i i i dpf+02,fhc+14
J1910−5959E 0.13 4.57177 −43.7(1) 33.29(5) i i i i dpf+02,fhc+14
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, and93,jcj+06
B2127+11B 0.079 56.1330 +956(6) 67.69(12) i i i i agk+90,and93,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(xii) double neutron star, eccentric agk+90,pakw91,and93,jcj+06
B2127+11D 0.019 4.80280 −107.5(1.2) 67.28(21) i i i i and93
B2127+11E 0.135 4.65144 +17.8(7) 66.51(12) i i i i and93
B2127+11F 0.279 4.02704 +3.2(8) 65.52(15) i i i i and93
B2127+11G 0.106 37.6602 +195(45) 66.43(24) i i i i and93
B2127+11H 0.038 6.74339 +2.4(1.3) 67.15(12) i i i i and93
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, which should be cited whenever possible. 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 °)

b: Galactic latitude (in °)

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 M and an inclination of 60°. 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) °/year (1-σ). This implies a total system mass of 1.61(4) M. From this, we can derive mp < 1.52 and mc > 0.164 M respectively. The median of the probability for the mass of the pulsar, assuming a flat cos i distribution, is 1.44 M.

(ii) The rate of advance of periastron of NGC 1851A has been measured (frg07), it is 0.01289(4) °/year (1-σ). This implies a total system mass of 2.453(14) M. From this, we can derive mp < 1.5 and mc > 0.96 M respectively. Furthermore, the median of the expected pulsar masses (assuming a flat cos i distribution) is 1.35 M.

(iii) The rate of advance of periastron of M5B has been measured at 0.0142(7) °/year (one σ, see fwbh08). Assuming the periastron advance is fully relativistic, the total binary mass is 2.29 ± 0.17 M. The maximum pulsar mass is 2.52 M and mc > 0.13 M. mp is 2.08+0.18−0.19 M (median and 1-σ limits). The probability of having a pulsar mass between 1.2 and 1.44 M 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 mp/mc = 5.85(13). Assuming mp between 1.4 and 1.9 M, this constrains the inclination to be between 47° and 56°.

(v) The rate of advance of periastron of Ter 5 I has been measured (rhs+05), it is 0.255(1) °/year (1-σ). This implies a total system mass of 2.17(2) M. From this, we can derive mp < 1.96 and mc > 0.24 M respectively. Furthermore, the median of the expected pulsar masses (assuming a flat cos i distribution) is 1.87 M.

(vi) The rate of advance of periastron of Ter 5 J has been measured (rhs+05), it is 0.327(4) °/year (1-σ). This implies a total system mass of 2.20(4) M. From this, we can derive mp < 1.96 and mc < 0.38 M respectively. The median of the expected pulsar masses (assuming a flat cos i distribution) is 1.73 M.

(vii) The rate of advance of periastron of NGC 6440B has been measured (frb+08), it is 0.00391(18) °/year (1-σ). This implies a total system mass of 2.92(20) M. From this, we can derive mp < 3.24 and mc > 0.11 M respectively. Furthermore, the median and 1-σ limits of the expected pulsar mass (assuming a flat cos i distribution) is 2.74 ± 0.20 M, there is a 1 % chance that the inclination is low enough to make the mass of the pulsar smaller than 2 M. 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) °/year (1-σ). This implies a total system mass of 1.97(15) M. From this, we can derive mp < 1.65 and mc > 0.53 M respectively. The medians for the pulsar and companion masses are 1.26 and 0.67 M. Another measurement of the rate of periastron has been published by pcm+06; this yields a total system mass of 2.15 ± 0.06 M, 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) °/year (1-σ). This implies a total system mass of 1.7(4) M. From this, we can derive mp < 1.7 and mc < 0.23 M respectively.

(x) Further constraints on the masses of the components of this system have been obtained from a detection of the rate of advance of periastron, which implies (assuming it is fully caused by relativistic effects) a total mass of 2.57190(73) M. The Shapiro delay was also detected and allows an estimate of the masses of the individual components: mc = 1.2064(20) M (the largest mass ever detected around a fully recycled pulsar, it could be a heavy white dwarf or another neutron star) and mp = 1.3655(21) M. This is the most precise mass ever derived for a millisecond pulsar.

(xi) 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 mc = 0.18 ± 0.02 M, and mp = 1.40+0.16−0.10 M. If the white-dwarf spectrum and the distance of NGC 6752 are used instead to determine the white-dwarf radius, they find rc = 0.058 ± 0.004 R. For the observed temperature, the mass-radius relations predict a white-dwarf mass of mc = 0.175 ± 0.010 M, constraining mp = 1.34 ± 0.08 M. These results are consistent with those of cfpd06.

(xii) 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). mp = 1.358 ± 0.010 M and mc = 1.354 ± 0.010 M.


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 < 3x10−5M, these have companions with masses of 0.01-0.03 M and generally present shorter orbital periods than the LMBPs (f > 10−4 M). 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+0327), 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: 2013 November 19
Paulo C. C. Freire