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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Influential
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Gasperini, M., & VENEZIANO, G. (1998) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.59.043503 · Cited by 28
Effect of evolving physical constants on type Ia supernova luminosity
Gupta, R. P. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac254 · Cited by 29
Measuring neutron star mass and radius with three mass-radius relations
Zhang, C. M., Yin, H. X., Kojima, Y., et al. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.11133.x · Cited by 29
Evolution of white dwarfs as a probe of theories of gravitation: the case of Brans—Dicke
Benvenuto, O. G., Althaus, L. G., & Torres, D. F. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02486.x · Cited by 28
The minimum and maximum gravitational-wave background from supermassive binary black holes
Zhu, X. J., Cui, W., & Thrane, E. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2849 · Cited by 28
“The proposed binary system, with inferred total mass of 5.4 × 1010M and mass ratio of 0.1, was subsequently ruled out with 95% confidence by Jenet et al. (2004) using timing observations of PSR B1855+09 presented in Kaspi et al. (1994).”
MethodInfluential
Constraining cosmic superstrings with dilaton emission
Babichev, E., & Kachelrieß, M. (2005) · Physics Letters B · doi:10.1016/j.physletb.2005.03.053 · Cited by 28
“8 wave background [ 15 ]. However, this bounds is modified only by a factor < 3 in the range of dilaton masses m� < 150 TeV and cosmic string parameters, 10 3 < p ≤ 1 and 104 < ǫ < 10 6, therefore the Figs.”
Background
Constraining a possible time variation of the gravitational constant G with terrestrial nuclear laboratory data
Krastev, P. G., & Li, B.-A. (2007) · Physical Review C · doi:10.1103/physrevc.76.055804 · Cited by 28
On the precession constant: Values and constraints on the dynamical ellipticity; link with Oppolzer terms and tilt-over-mode
Dehant, V., & Capitaine, N. (1997) · Celestial Mechanics and Dynamical Astronomy · doi:10.1007/bf00049506 · Cited by 28
MERGERS OF LUMINOUS EARLY-TYPE GALAXIES IN THE LOCAL UNIVERSE AND GRAVITATIONAL WAVE BACKGROUND
Wen, Z. L., Liu, F. S., & Han, J. L. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/692/1/511 · Cited by 27
“(18) Using the eight year timing data of PSR B1855+09, Kaspi et al. (1994) obtainedΩh2 < 6× 10−8 for the cosmic GW background.”
Method
Temperature and cooling age of the white dwarf companion of PSR J0218+4232
Bassa, C., van Kerkwijk, M. H., & Kulkarni, S. R. (2003) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20030384/pdf · Cited by 27
Pulse Arrival Times from Binary Pulsars with Rotating Black Hole Companions
Laguna, P., & Wolszczan, A. (1997) · The Astrophysical Journal · doi:10.1086/310835 · Cited by 27
A 25.3 Day Periodicity in the Timing of the Pulsar PSR B1257+12: A Planet or a Heliospheric Propagation Effect?
Wolszczan, A., Hoffman, I. M., Konacki, M., et al. (2000) · The Astrophysical Journal · doi:10.1086/312872 · Cited by 27
The refractive index of relic gravitons
Massimo Giovannini, A. (2016) · Classical and Quantum Gravity · doi:10.1088/0264-9381/33/12/125002 · Cited by 27
Sensitivity of wideband detectors to quintessential gravitons
Babusci, D., & Giovannini, M. (1999) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.60.083511 · Cited by 27
The NANOGrav 11-year Data Set: Pulse Profile Variability
Brook, P. R., Karastergiou, A., McLaughlin, M. A., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae9e3 · Cited by 26
“Suggested interpretations of the red noise include intrinsic changes in the spindown rate of the pulsar (Kaspi et al. 1994), interstellar propagation effects (Armstrong 1984; Rickett 1990; Kaspi et al. 1994; Cognard et al. 1995) and the presence of a circumpulsar asteroid belt (Shannon et al. 2013).”
Background
Lutz-Kelker bias in pulsar parallax measurements
Verbiest, J. ;. H. O.-0.-4.-8., Lorimer, D. R., & McLaughlin, M. A. (2010) · The Research Repository @ WVU (West Virginia University) · Cited by 26
Radio Pulsars
Beskin, V. S., Чернов, С. В., Gwinn, C. R., et al. (2015) · Space Science Reviews · doi:10.1007/s11214-015-0173-8 · Cited by 26
Large High-precision X-Ray Timing of Three Millisecond Pulsars with NICER: Stability Estimates and Comparison with Radio
Siklér, F., Ray, P. S., Lommen, A. N., et al. (2019) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 26
Secondary graviton spectra and waterfall-like fields
Giovannini, M. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.82.083523 · Cited by 26
Pulsars and Gravitational Wave Detection
Hobbs, G. (2005) · Publications of the Astronomical Society of Australia · doi:10.1071/as04063 · Cited by 26
“This work was generalized for multiple pulsar data sets by Kaspi et al. (1994), but was criticized by Thorsett & Dewey (1996), who developed a technique based on the Neyman–Pearson test.”
Method
Pulsar Timing Arrays: Status and Techniques
Hobbs, G. B. (2012) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921312023526 · Cited by 25
The confrontation between general relativity and experiment
Will, C. M. (2004) · Pramana · doi:10.1007/bf02705195 · Cited by 29
Bayesian estimation of non-Gaussianity in pulsar timing analysis
Lentati, L., Hobson, M., & Alexander, P. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1721 · Cited by 24
Gravitational wave detection using high precision pulsar observations
Hobbs, G. B. (2008) · Classical and Quantum Gravity · doi:10.1088/0264-9381/25/11/114032 · Cited by 24
“In contrast with earlier techniques (e.g. Kaspi et al 1994) this method used the TEMPO2 software package (Hobbs et al 2006a) to account for all the fitting procedures undertaken during the pulsar timing process.”
Method

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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