Einstein@Home pulsar discoveries in Parkes Multibeam Survey data

Background

Einstein@Home is currently re-analysing the Parkes Multibeam Survey (PMsurv) data. Observations of 35 minutes length are coherently searched for radio pulsars in binary systems. This is the first search of this data set using coherent binary search methods over the full observation time of each beam.

Results

So far, the Einstein@Home-PMsurv re-analysis has found twenty new pulsars, which were confirmed with recent observations. The properties of the pulsars in the PMsurv discovery beams are listed in the table below.

Pulsar Table

pulsar beam RA beam DEC Pbary DM prepf sig E@H sgnf plots volunteers date added notes
J0811-38 08:11.7 -38:57 482.5939(16)
 336.2 9.8 15.6 E@H - prepfold Nemo/ATLAS AEI Hannover 24 Apr 2012 --
J1227-62 12:27.6 -62:10 34.5296853(77)
 363.2 12.6 17.9 E@H - prepfold Rolf Schuster/Darren Chase 27 Feb 2012 MSP
J1305-66 13:05.6 -66:39 197.27629(20)
 316.1 8.2 15.5 E@H - prepfold Victor1st/Dussan 23 Apr 2012 --
J1322-63 13:22.9 -63:21 1044.8511(38)
 733.6 11.5 23.1 E@H - prepfold Vadim Gusev/David 06 Jul 2011 intermittent
J1455-59 14:55.1 -59:23 176.19117(16)
 498.0 7.6 14.0 E@H - prepfold Arax/UW-Madison CAE 12 Jul 2011 -
J1601-50 16:01.4 -50:23 860.7771(40)
 59.0 13.5 29.1 E@H - prepfold Sirko Rosenberg/Ton van Born 27 Feb 2012 -
J1619-42 16:19.1 -42:02 1023.1524(36)
 172.0 18.1 35.4 E@H - prepfold Metod, S56RKO/RAMA 19 Aug 2011 -
J1637-46 16:37.6 -46:13 493.0910(18)
 660.4 8.8 17.2 E@H - prepfold Riaan Strydom/Edelgas 23 Apr 2012 --
J1644-44 16:44.6 -44:10 173.91055(17)
 535.1 7.3 14.1 E@H - prepfold Jesse Charles Wagner II [USA]/Ras 18 Jul 2011 -
J1652-48 16:52.9 -48:45 3.78512377(36)
 187.8 8.6 22.3 E@H - prepfold Craig G/Brian Adrian 23 Apr 2012 MSP
J1726-31 17:26.6 -31:57 123.470178(87)
 264.4 8.4 15.9 E@H - prepfold Bogusław Sobczak/Steve Mellor 27 Feb 2012 -

J1750-25
 17:50.5 -25:36 34.7490529(77)
 179.0 7.5 15.9 E@H - prepfold F Pfitzer/boinc_qc
24 Apr 2012
MSP
17:50.3 -25:34 34.749138(15)
 177.8 8.4 15.9 E@H - prepfold Masor_DC/Gordon Hartman

J1755-33
 17:55.1 -33:25 959.4568(42)
 249.0 10.4 21.2 E@H - prepfold Omega Sector - Game Systems/Dwaine
26 Jul 2011
in 3 beams
17:55.7 -33:39 959.4524(22)
 248.9 7.9 9.7 E@H - prepfold revoluzzer/Jacek Richter
J1811-10 18:11.4 -10:47 2623.916(22)
 239.7 19.7 29.2 E@H - prepfold ingo/Paul Serban 19 Aug 2011 -

J1817-19
 18:17.2 -19:37 2046.742(12)
 463.9 10.4 16.9 E@H - prepfold Jaska/Family
06 Jul 2011
intermittent
18:19.2 -19:36 2046.916(17)
 523.7 10.1 14.1 E@H - prepfold cjsturgess/Companion_Cube
J1821-03 18:21.7 -03:25 902.3136(30)
 171.5 14.0 28.3 E@H - prepfold Robert Hoyt/Kevin Battaile 06 Sep 2011 intermittent?
J1838-01 18:38.5 -01:01 183.29478(26)
 320.4 9.0 16.7 E@H - prepfold Eric/Tim Taylor 23 Apr 2012 --
J1838-18 18:38.3 -18:48 488.2396(18)
 167.3 14.2 31.7 E@H - prepfold gwyll/IG_the_cheetah 19 Aug 2011 -

J1840-06
 18:40.2 -06:51 35.5775996(73)
 492.6 7.4 15.4 E@H - prepfold terrydudley/nemo
06 Jul 2011
binary MSP
18:40.6 -06:38 35.578184(15)
 495.9 7.6 18.2 E@H - prepfold Trey/nemo
J1858-07 18:58.6 -07:37 551.0553(13)
 201.4 11.1 16.7 E@H - prepfold bench-seater/gone 15 May 2011 -


Info

[1] Names will be provided shortly - still waiting for permission from the volunteers.
“pulsar” preliminary pulsar name.
“beam RA”: right ascension of the discovery beam
“beam DEC”: declination of the discovery beam
“Pbary”: barycentric spin period in ms (1-sigma error in parentheses).
“DM”: dispersion measure in pc/cc.
“prepf sig”: significance in sigma from prepfold.
“E@H sgnf”: Einstein@Home significance (S=-log10 (pfA))
“plots”: plots of E@H results and prepfold plot
“volunteers”: the volunteers, whose computers found the new pulsar
“date added”: date when this pulsar was published on this webpage
“notes” contains identifications and other notes: “MSP” stands for “millisecond pulsar”, i.e. a pulsar with a spin period of tens of milliseconds or faster. “binary” pulsars are those that orbit the common centre of mass with a companion star. “intermittent” pulsars show interruptions in their emissions. You can see them switch on and/or off in the cause of one observation.



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Last Updated: May 15, 2012