Cited by 598Pulsars and Gravitational Waves ResearchAstrophysical Phenomena and ObservationsStellar, planetary, and galactic studies

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High-precision timing of millisecond pulsars. 3: Long-term monitoring of PSRs B1855+09 and B1937+21

Kaspi, V. M., Taylor, J. H., Ryba, M. F.·1994·The Astrophysical Journal

DOI 10.1086/174280

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Abstract

Biweekly timing observations of PSRs B1855+09 and B1937+21 have been made at the Arecibo Observatory for more than 7 and 8 year, respectively, with uniform procedures and only a few modest gaps. On each observing date we measure an equivalent pulse arrival time for PSR B1855+09 at 1.4 GHz, with typical accuracies of about 0.8 micrometers and for PSR B1937 + 21 at both 1.4 and 2.4 GHz, with accuracies around 0.2 micrometers. The pulse arrival times are fitted to a simple model for each pulsar, yielding high-precision astrometric, rotational, and orbital parameters, and a diverse range of conclusions. The celestial coordinates and proper motions of the two pulsars are determined with uncertainties less than or equal to 0.12 mas and less than or equal to 0.06 mas/year in the reference frame of the DE200 planetary ephemeris. The annual parallaxes are found to be pi=1.1 +/- 0.3 mas and pi less than 0.28 mas for PSRs B1855+09 and B1937+21, respectively. The general relativistic Shapiro delay is measured in the PSR B1855+09 system and used to obtain masses m1 = 1.50 +0.26 -0.14 solar mass and m (sub2) = 0.258 +0.028-0.016solar mass for the pulsar and its orbiting companion. The extremely stable orbital period of this system provides a phenomenological limit on the secular change of Newton's gravitational constant, dot-G/G=(-9 +/- 18) x 10-12/year. Variations in the dispersion measure of PSR B1937 + 21 indicate that the spectrum of electron-density fluctuations in the interstellar medi um has a power-law index beta = 3.874 +/- 0.011, slightly steeper than the Kolmogorov value of 11/3, and we find no strong evidence for an 'inner scale' greater than about 2 x 109cm. In the residual pulse arrival times for PSR B1937+21 we have observed small systematic trends not explained by our deterministic timing model. We discuss a number of possible causes; although the results are not yet conclusive, the most straightforward interpretation is that the unmodeled noise (a few microseconds over 8 yr, or Delta t/T approximately equals 10-14 is inherent to the pulsar itself. In the present data set, PSR B1855+09 exhibits no discernible timing noise. With conventional assumptions we derive a limit Omega g h2 less than 6 x 10-8 (95% confidence) for the energy density, per logarithmic frequency interval, in a cosmic background of stochastic gravitational waves. We discuss the feasibility of establishing a pulsar-based timescale that might be used to test the stabilities of the best available atomic clocks. In an Appendix, we propose guidelines for the archiving of pulsar timing observations. Instructions are provided for obtaining copies of our own archival data, via Internet.

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“We also indicate the locations of WD companions to some millisecond pulsars (see Table 6). which has been estimated quite precisely by using the Shapiro delay of the pulsar signal – see Kaspi et al. (1994) – and a Teff ≈ 4800 ± 800 K – see Bassa et al. (2003).”
Method
Precision Timing of PSR J0437−4715: An Accurate Pulsar Distance, a High Pulsar Mass, and a Limit on the Variation of Newton’s Gravitational Constant
Verbiest, J. ;. H. O.-0.-4.-8., Bailes, M., van Straten, W., et al. (2008) · PUB – Publications at Bielefeld University (Bielefeld University) · Cited by 171
Bounds on cosmic strings from WMAP and SDSS
Wyman, M., Pogosian, L., & Wasserman, I. (2005) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.72.023513 · Cited by 172
Neutron Star Population Dynamics. I. Millisecond Pulsars
Cordes, J. M., & Chernoff, D. F. (1997) · The Astrophysical Journal · doi:10.1086/304179 · Cited by 165
“To date, there are timing proper motions on eight MSPs: J0437-4715 (Bell et al. 1995), B1257+12 (Wolszczan 1994), J1713+0747 (Camilo, Foster & Wolszczan 1994), B1855+09 & B1937+21 (Kaspi et al. 1994), B1957+20 (Arzoumanian, Fruchter & Taylor 1994), J2019+2425 and J2322+2057 (Nice & Taylor 1995).”
Influential
SEARCHES FOR GRAVITATIONAL WAVES FROM KNOWN PULSARS WITH SCIENCE RUN 5 LIGO DATA
Abbott, B. P., Abbott, R., Acernese, F., et al. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/713/1/671 · Cited by 164
A COMPREHENSIVE STUDY OF RELATIVISTIC GRAVITY USING PSR B1534+12
Fonseca, E., Stairs, I. H., & Thorsett, S. E. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/787/1/82 · Cited by 169
“These long-term DM measurements are useful for a statistical analysis of turbulence within the interstellar medium (e.g., Kaspi et al. 1994), which usually assumes that the power spectrum of spatial variations in electron density is a power law within a range of length scales (Rickett 1990), P (q)…”
Background
The NANOGrav 15 yr Data Set: Bayesian Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
Agazie, G., Anumarlapudi, A., Archibald, A. M., Arzoumanian, Z., Baker, P. T., Bécsy, B., Blecha, L., Brazier, A., Brook, P. R., Burke-Spolaor, S., et al. (2023) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ace18a · Cited by 156
Self-citation
The Characteristics of Millisecond Pulsar Emission. III. From Low to High Frequencies
Krämer, M., Lange, C., Lorimer, D. R., et al. (1999) · The Astrophysical Journal · doi:10.1086/308042 · Cited by 153
Binary and Millisecond Pulsars
Lorimer, D. R. (2005) · Living Reviews in Relativity · doi:10.12942/lrr-2005-7 · Cited by 152
“From high quality observations spanning over a decade [274, 275, 155], these groups have demonstrated that the timing stability of millisecond pulsars over such time-scales is comparable to terrestrial atomic clocks.”
BackgroundInfluential
Searches For Gravitational Waves From Known Pulsars With Science Run 5 LIGO Data
Virgo, C. (2016) · MPG.PuRe (Max Planck Society) · doi:10.15781/t2xj7m · Cited by 150
Dispersion measure variations and their effect on precision pulsar timing
You, X. P., Hobbs, G., Coles, W. A., et al. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11617.x · Cited by 150
“Subsequently, the technique was applied to PSR J1939+2134 (B1937+21) by Cordes et al. (1990), Kaspi et al. (1994) and Ramachandran et al. (2006).”
BackgroundMethodInfluential
Phase Transitions in the Early and Present Universe
Boyanovsky, D., de Vega, H. J., & Schwarz, D. J. (2006) · Annual Review of Nuclear and Particle Science · doi:10.1146/annurev.nucl.56.080805.140539 · Cited by 146
Evidence from a processing pulsar orbit for a neutron-star birth kick
Kaspi, V. M., Bailes, M., Manchester, R. N., et al. (1996) · Nature · doi:10.1038/381584a0 · Cited by 147
Self-citation
The relativistic pulsar-white dwarf binary PSR J1738+0333 - I. Mass determination and evolutionary history
Antoniadis, J., van Kerkwijk, M. H., Koester, D., et al. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21124.x · Cited by 146
“…eccentric, allowing for a measurement of the rate of advance of periastron (Freire et al. 2011), or if the system has an orbit seen edge on (Kaspi et al. 1994; Jacoby et al. 2005; Demorest et al. 2010) which allows for a measurement of pulse time-of-arrival (TOA) delays due to the…”
Background
Timing stability of millisecond pulsars and prospects for gravitational-wave detection
Verbiest, J. P. W., Bailes, M., Coles, W. A., Hobbs, G. B., van Straten, W., Champion, D. J., Jenet, F. A., Manchester, R. N., Bhat, N. D. R., Sarkissian, J. M., et al. (2024) · Figshare · doi:10.25916/sut.26223230.v1 · Cited by 146
Proper Motion of Binary Pulsars as a Source of Secular Variations of Orbital Parameters
Kopeikin, S. M. (1996) · The Astrophysical Journal · doi:10.1086/310201 · Cited by 140
Precision Timing Measurements of PSR J1012+5307
Lange, C., Camilo, F. M., Wex, N., et al. (2001) · CERN Document Server (European Organization for Nuclear Research) · Cited by 140
Glitches in southern pulsars
Wang, N., Manchester, R. N., Pace, R. T., et al. (2000) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2000.03713.x · Cited by 138
“Positions were obtained using the so-called ‘pre-whitening’ method (Kaspi et al. 1994).”
BackgroundMethodSelf-citation
Masses, Parallax, and Relativistic Timing of the PSR J1713+0747 Binary System
Splaver, E. M., Nice, D. J., Stairs, I. H., et al. (2005) · The Astrophysical Journal · doi:10.1086/426804 · Cited by 136
“…gravitational wave background at frequencies of 10 6 to 10 5 Hz by searching for arrival time variations on timescales of years (Lommen et al. 2003; Kaspi et al. 1994), but such measurements require that the timing signal not be contaminated by ‘‘timing noise,’’ random variations of the pulsar…”
BackgroundMethod
Gravitational wave astronomy: the current status
Blair, D. G., Ju, L., Zhao, C., Wen, L., Chu, Q., Fang, Q., Cai, R.-G., Gao, J., Lin, X., Liu, D., et al. (2015) · Science China Physics Mechanics and Astronomy · doi:10.1007/s11433-015-5748-6 · Cited by 146
Hyper-efficient model-independent Bayesian method for the analysis of pulsar timing data
Lentati, L., Alexander, P. E., Hobson, M., et al. (2013) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.87.104021 · Cited by 132
Further results from the timing of the millisecond pulsars in 47 Tucanae
Freire, P. C. C., Camilo, F., Krämer, M., et al. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06392.x · Cited by 131
GRAVITATIONAL WAVES FROM INDIVIDUAL SUPERMASSIVE BLACK HOLE BINARIES IN CIRCULAR ORBITS: LIMITS FROM THE NORTH AMERICAN NANOHERTZ OBSERVATORY FOR GRAVITATIONAL WAVES
Arzoumanian, Z., Brazier, A., Burke-Spolaor, S., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/794/2/141 · Cited by 130
“Several upper limits have been placed on the strength of the stochastic background (Kaspi et al. 1994; Jenet et al. 2006; van Haasteren et al. 2011; Demorest et al. 2013; Shannon et al. 2013) and continuous waves (Jenet et al. 2004; Yardley et al. 2010) but no successful detection has yet been made.”
BackgroundSelf-citation
Relic gravitational waves from cosmic strings: Updated constraints and opportunities for detection
Caldwell, R. R., Battye, R. A., & Shellard, E. P. S. (1996) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.54.7146 · Cited by 129
Searching for anisotropic gravitational-wave backgrounds using pulsar timing arrays
Taylor, S. R., & Gair, J. R. (2013) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.88.084001 · Cited by 129
Gravitational waves from collapsing domain walls
Hiramatsu, T., Kawasaki, M., & Saikawa, K. (2010) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2010/05/032 · Cited by 124

Authors: Kaspi, V. M., Taylor, J. H., & Ryba, M. F.
ORCID: Kaspi, V. M.
Venue: The Astrophysical Journal
Publisher: American Astronomical Society
Published: 1994-06
Volume: 428
Pages: 713
ISSN: 0004-637X (ISSN-L)
1538-4357
DOI: 10.1086/174280
OpenAlex: W2025727932
Cited by: 595
References: 0
Citations by year: 2026: 8 · 2025: 16 · 2024: 21 · 2023: 13 · 2022: 9 · 2021: 17 · 2020: 13 · 2019: 14 · 2018: 33 · 2017: 7 · 2016: 20 · 2015: 21 · 2014: 17 · 2013: 17 · 2012: 22
FWCI: 25.02
Type: journal article
Language: en
Open access: closed
Locations: The Astrophysical Journal (publishedVersion)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Pulsars and Gravitational Waves Research
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords: millisecond pulsars, PSR B1937+21, pulsar timing, proper motions, annual parallax, Shapiro delay, varying gravitational constant, dispersion measure, Kolmogorov spectrum, pulsar astrometry, orbital elements, Arecibo Observatory

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High-precision timing of millisecond pulsars. 3: Long-term monitoring of PSRs B1855+09 and B1937+21

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