Large High-precision X-Ray Timing of Three Millisecond Pulsars with NICER:Stability Estimates and Comparison with Radio

Deneva, J. S., Ray, P. S., Lommen, A., Ransom, S. M., Bogdanov, S., Kerr, M., Wood, K. S., Arzoumanian, Z., Black, K., Doty, J., Gendreau, K. C., Guillot, S., Harding, A., Lewandowska, N., Malacaria, C., Markwardt, C. B., Price, S., Winternitz, L., Wolff, M. T., Guillemot, L., Cognard, I., Baker, P. T., Blumer, H., Brook, P. R., Cromartie, H. T., Demorest, P. B., Decesar, M. E., Dolch, T., Ellis, J. A., Ferdman, R. D., Ferrara, E. C., Fonseca, E., Garver-Daniels, N., Gentile, P. A., Jones, M. L., Lam, M. T., Lorimer, D. R., Lynch, R. S., McLaughlin, M. A., Ng, C., Nice, D. J., Pennucci, T. T., Spiewak, R., Stairs, I. H., Stovall, K., Swiggum, J. K., Vigeland, S. J. and Zhu, W. W. (2019) Large High-precision X-Ray Timing of Three Millisecond Pulsars with NICER:Stability Estimates and Comparison with Radio. Astrophysical Journal, 874 (2). ISSN 0004-637X

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Abstract

The Neutron Star Interior Composition Explorer (NICER) is an X-ray astrophysics payload on the International Space Station. It enables unprecedented high-precision timing of millisecond pulsars (MSPs) without the pulse broadening and delays due to dispersion and scattering within the interstellar medium that plague radio timing. We present initial timing results from a year of data on the MSPs PSR B1937+21 and PSR J0218+4232, and nine months of data on PSR B1821-24. NICER time-of-arrival uncertainties for the three pulsars are consistent with theoretical lower bounds and simulations based on their pulse shape templates and average source and background photon count rates. To estimate timing stability, we use the σ z measure, which is based on the average of the cubic coefficients of polynomial fits to subsets of timing residuals. So far we are achieving timing stabilities σ z ≈ 3 ×10 -14 for PSR B1937+21 and on the order of 10 -12 for PSRs B1821-24 and J0218+4232. Within the span of our NICER data we do not yet see the characteristic break point in the slope of σ z ; detection of such a break would indicate that further improvement in the cumulative root-mean-square timing residual is limited by timing noise. We see this break point in our comparison radio data sets for PSR B1821-24 and PSR B1937+21 on timescales of >2 yr.

Item Type: Article
Uncontrolled Keywords: pulsars: general,pulsars: individual (psr b1821-24, psr b1937+21, psr j0218+4232),stars: neutron,astronomy and astrophysics,space and planetary science ,/dk/atira/pure/subjectarea/asjc/3100/3103
Faculty \ School: Faculty of Science > School of Chemistry
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Depositing User: LivePure Connector
Date Deposited: 13 Jun 2019 13:30
Last Modified: 29 Jul 2020 23:46
URI: https://ueaeprints.uea.ac.uk/id/eprint/71392
DOI: 10.3847/1538-4357/ab0966

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