2014ApJ...794...21D

Query : 2014ApJ...794...21D

2014ApJ...794...21D - Astrophys. J., 794, 21 (2014/October-2)

A 24 hr global campaign to assess precision timing of the millisecond pulsar J1713+0747.

DOLCH T., LAM M.T., CORDES J., CHATTERJEE S., BASSA C., BHATTACHARYYA B., CHAMPION D.J., COGNARD I., CROWTER K., DEMOREST P.B., HESSELS J.W.T., JANSSEN G., JENET F.A., JONES G., JORDAN C., KARUPPUSAMY R., KEITH M., KONDRATIEV V., KRAMER M., LAZARUS P., LAZIO T.J.W., LEE K.J., McLAUGHLIN M.A., ROY J., SHANNON R.M., STAIRS I., STOVALL K., VERBIEST J.P.W., MADISON D.R., PALLIYAGURU N., PERRODIN D., RANSOM S., STAPPERS B., ZHU W.W., DAI S., DESVIGNES G., GUILLEMOT L., LIU K., LYNE A., PERERA B.B.P., PETROFF E., RANKIN J.M. and SMITS R.

Abstract (from CDS):

The radio millisecond pulsar J1713+0747 is regarded as one of the highest-precision clocks in the sky and is regularly timed for the purpose of detecting gravitational waves. The International Pulsar Timing Array Collaboration undertook a 24 hr global observation of PSR J1713+0747 in an effort to better quantify sources of timing noise in this pulsar, particularly on intermediate (1-24 hr) timescales. We observed the pulsar continuously over 24 hr with the Arecibo, Effelsberg, GMRT, Green Bank, LOFAR, Lovell, Nanay, Parkes, and WSRT radio telescopes. The combined pulse times-of-arrival presented here provide an estimate of what sources of timing noise, excluding DM variations, would be present as compared to an idealized sqrt( [****UnclosedBrace??****]N) improvement in timing precision, where N is the number of pulses analyzed. In the case of this particular pulsar, we find that intrinsic pulse phase jitter dominates arrival time precision when the signal-to-noise ratio of single pulses exceeds unity, as measured using the eight telescopes that observed at L band/1.4 GHz. We present first results of specific phenomena probed on the unusually long timescale (for a single continuous observing session) of tens of hours, in particular interstellar scintillation, and discuss the degree to which scintillation and profile evolution affect precision timing. This paper presents the data set as a basis for future, deeper studies. [****ClosingBrace(s)Inserted****]N) improvement in timing precision, where N is the number of pulses analyzed. In the case of this particular pulsar, we find that intrinsic pulse phase jitter dominates arrival time precision when the signal-to-noise ratio of single pulses exceeds unity, as measured using the eight telescopes that ob ∼

Journal keyword(s): gravitational waves - ISM: structure - pulsars: individual: PSR J1713+0747

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 PSR J0437-47 Psr 04 37 15.7994581776 -47 15 08.544351636           DC 1032 0
2 MCG-02-24-007 LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1077 1
3 FIRST J141341.6+150939 Q? 14 13 41.6607 +15 09 39.515           ~ 13 1
4 QSO B1445+101 Bla 14 45 16.46525080 +09 58 36.0727447   18.58 17.78     ~ 408 2
5 PSR B1534+11 Psr 15 37 09.9603 +11 55 55.554           ~ 453 1
6 PSR J1713+0747 Psr 17 13 49.5367813 +07 47 37.450240           ~ 530 1
7 PMN J1822-0939 Rad 18 22 28.792 -09 38 57.03           ~ 49 1
8 PSR J1909-3744 Psr 19 09 47.42820 -37 44 14.7740           ~ 343 2
9 PSR B1937+21.4 Psr 19 39 38.560096 +21 34 59.13552           ~ 1142 0

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