THE NANOGRAV NINE-YEAR DATA SET: MASS AND GEOMETRIC MEASUREMENTS OF BINARY MILLISECOND PULSARS

By E. Fonseca, T. Pennucci, J. Ellis, Ingrid Stairs, D. Nice, S. Ransom, P. Demorest, Z. Arzoumanian, K. Crowter, T. Dolch and 10 more. 2016

401 citations recorded by the source corpus.

We analyze 24 binary radio pulsars in the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) nine-year data set. We make 14 significant measurements of the Shapiro delay, including new detections in four pulsar-binary systems (PSRs J0613−0200, J2017+0603, J2302+4442, and J2317+1439), and derive estimates of the binary-component masses and orbital inclination for these MSP-binary systems. We find a wide range of binary pulsar masses, with values as low as for PSR J1918−0642 and as high as for PSR J1614−2230 (both 68.3% credibility). We make an improved measurement of the Shapiro timing delay in the PSR J1918−0642 and J2043+1711 systems, measuring the pulsar mass in the latter system to be (68.3% credibility) for the first time. We measure secular variations of one or more orbital elements in many systems, and use these measurements to further constrain our estimates of the pulsar and companion masses whenever possible. In particular, we used the observed Shapiro delay and periastron advance due to relativistic gravity in the PSR J1903+0327 system to derive a pulsar mass of (68.3% credibility). We discuss the implications that our mass measurements have on the overall neutron-star mass distribution, and on the “mass/orbital-period” correlation due to extended mass transfer.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/1c02f0252f0b4e29ee2fc5ffb4086e94004ef697

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Citations in the corpus

Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, background): “Recent measurement of NSs with masses close to 2M (Antoniadis et al. 2013; Demorest et al. 2010; Fonseca et al. 2016) has already put significant constraints on the EoS, and the requirement c© 0000 The Authors ar X iv :1 70 9.”
Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, background): “…causal at all pressures, that the lowest two pressures exceed the limit placed by two-nucleon interaction, and that all EOS must produce a neutron star of at least 1.97 M , in order to be within 1σ of the measurements of the most massive neutron stars (Antoniadis et al. 2013; Fonseca et al. 2016).”
The NANOGrav 11-year Data Set: High-precision Timing of 45 Millisecond Pulsars (2017, background): “…detection, high-precision pulsar data can be used for a variety of other applications, including studies of binary systems and neutron-star masses (Fonseca et al. 2016), measurements of pulsar astrometry and space velocities (Matthews et al. 2016), tests of general relativity (Zhu et al. 2015),…”
Equation of state sensitivities when inferring neutron star and dense matter properties (2018, neutral): “The complete CS parametrization can then be written as c2s (x)/c 2 = a1 e− 12 (x−a2)2/a23 + a6 + 1 3 − a6 1 + e−a5(x−a4) , (1) 1The mass of PSR J1614–2230 was recently updated from 1.97 ± 0.04 M (Demorest et al. 2010) to 1.928 ± 0.017 M (Fonseca et al. 2016).”
Formation of Double Neutron Star Systems (2017, background): “An extreme example is PSR J1918−0642, which is an MSP with P = 7.6 ms, in orbit with a low-mass He WD and Porb = 10.9 days, and yet it has a mass of only 1.18+0.10−0.09 M⊙ (Fonseca et al. 2016).”
From hadrons to quarks in neutron stars: a review (2017, background): “017M [40] (the original mass measurement was 1.”