Using Long-term Millisecond Pulsar Timing to Obtain Physical Characteristics of the Bulge Globular Cluster Terzan 5

Prager, Brian; Ransom, S. M.; Freire, P. C. C.; Hessels, J. W. T.; Stairs, I. H.; Arras, Phil; Cadelano, Mario

doi:10.3847/1538-4357/aa7ed7

Cited by 89 publications

(142 citation statements)

References 79 publications

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“…For PSR J1748−2446ad it is not possible to determine the intrinsic ṅ of the neutron star because the observed change in spin rate with time is dominated by acceleration in the gravitational potential of Terzan5 (Prager et al 2016). Conversely, it will be possible to measure PSR J0952 −0607ʼs intrinsic spin-down rate and the inferred surface magnetic field, once a full timing solution is available.…”

Section: Discussionmentioning

confidence: 99%

LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic Field

Bassa

Pleunis

Hessels

et al. 2017

ApJL

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LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic FieldBassa, C.G.; Pleunis, Z.; Hessels, J.W.T.; Ferrara, E.C.; Breton, R.P.; Gusinskaia, N.; Kondratiev, V.I.; Sanidas, S.A.; Nieder, L.; Clark, C.J.; Li, T.; van Amesfoort, A.S.; Burnett, T.H.; Camilo, F.; Michelson, P.F.; Ransom, S.M.; Ray, P.S.; Wood, K. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. AbstractWe report the discovery of PSR J0952−0607, a 707 Hz binary millisecond pulsar that is now the fastest-spinning neutron star known in the Galactic field (i.e., outside of a globular cluster). PSR J0952−0607 was found using LOFAR at a central observing frequency of 135 MHz, well below the 300 MHz to 3 GHz frequencies typically used in pulsar searches. The discovery is part of an ongoing LOFAR survey targeting unassociated Fermi-Large Area Telescope γ-ray sources. PSR J0952−0607 is in a 6.42 hr orbit around a very low-mass companion, and we identify a strongly variable optical source, modulated at the orbital period of the pulsar, as the binary companion. The light curve of the companion varies by 1.6 mag from ¢ = r 22.2 at maximum to ¢ > r 23.8, indicating that it is irradiated by the pulsar wind. Swift observations place a 3σ upper limit on the -0.3 10 keV X-ray luminosity of <Ĺ 1.1 10 X 31 erg s −1 (using the 0.97 kpc distance inferred from the dispersion measure). Though no eclipses of the radio pulsar are observed, the properties of the system classify it as a black widow binary. The radio pulsed spectrum of PSR J0952−0607, as determined through flux density measurements at 150 and 350 MHz, is extremely steep with a~-3 (where n µ a S ). We discuss the growing evidence that the fastest-spinning radio pulsars have exceptionally steep radio spectra, as well as the prospects for finding more sources like PSR J0952−0607.

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Section: Discussionmentioning

confidence: 99%

LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic Field

Bassa

Pleunis

Hessels

et al. 2017

ApJL

Self Cite

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“…Unlike Brandt & Kocsis (2015), we take into account the merger history of globular clusters across the age of the Milky Way and the spindown of the MSPs due to magnetic-dipole braking selfconsistently. Unlike Hooper & Linden (2016), we adopt a spin-down distribution that is more consistent with observational constraints (Freire et al 2001a,b;Prager et al 2017). This allows us to estimate the present day gamma-ray luminosity from the bulge more accurately and compare it with the observed GC excess more consistently.…”

Section: Introductionmentioning

confidence: 99%

“…In model LON, we compute the spin-down rate via Eq. 14, by sampling magnetic fields from a log-normal distribution with mean of 10 8.47 G and standard deviation of 0.33 and by sampling periods from a log-normal distribution with P0 = 3 ms and σP = 0.234 (Prager et al 2017). In this model, the τ distribution has a mean around 1 Gyr, but also a nonnegligible tail at larger τ .…”

Section: Evolution Of Milli-second Pulsarsmentioning

confidence: 99%

Disrupted globular clusters and the gamma-ray excess in the Galactic Centre

Fragione

Antonini

Gnedin

2018

Monthly Notices of the Royal Astronomical Society

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The Fermi Large Area Telescope has provided the most detailed view toward the Galactic Centre (GC) in high-energy gamma rays. Besides the interstellar emission and point-source contributions, the data suggest a residual diffuse gamma-ray excess. The similarity of its spatial distribution with the expected profile of dark matter has led to claims that this may be evidence for dark matter particle annihilation. Here, we investigate an alternative explanation that the signal originates from millisecond pulsars (MSPs) formed in dense globular clusters and deposited at the GC as a consequence of cluster inspiral and tidal disruption. We use a semi-analytical model to calculate the formation, migration, and disruption of globular clusters in the Galaxy. Our model reproduces the mass of the nuclear star cluster and the present-day radial and mass distribution of globular clusters. For the first time, we calculate the evolution of MSPs from disrupted globular clusters throughout the age of the Galaxy and consistently include the effect of the MSP spin-down due to magnetic-dipole breaking. The final gamma-ray amplitude and spatial distribution are in good agreement with the Fermi observations and provide a natural astrophysical explanation for the GC excess.

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“…Two remaining possible origins are the jerk caused by the cluster potential (Phinney 1992(Phinney , 1993Prager et al 2017;Freire et al 2017) and that by a passing cluster star (Phinney 1992(Phinney , 1993Freire et al 2017). Following Freire et al (2017, equation 10) and using a maximum velocity of 49.5 km s −1 (Baumgardt & Hilker 2018, table 2), we find that the upper limit on | ν| from the cluster jerk is 3×10 −25 s −3 .…”

Section: Psr B1821−24amentioning

confidence: 54%

Correlated timing noise and high-precision pulsar timing: measuring frequency second derivatives as an example

Liu

Keith

Bassa

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the impact of noise processes on high-precision pulsar timing. Our analysis focuses on the measurability of the second spin frequency derivative ν. This ν can be induced by several factors including the radial velocity of a pulsar. We use Bayesian methods to model the pulsar times-of-arrival in the presence of red timing noise and dispersion measure variations, modelling the noise processes as power laws. Using simulated times-of-arrival that both include red noise, dispersion measure variations and non-zero ν values, we find that we are able to recover the injected ν, even when the noise model used to inject and recover the input parameters are different. Using simulations, we show that the measurement uncertainty on ν decreases with the timing baseline T as T γ , where γ = −7/2 + α/2 for power law noise models with shallow power law indices α (0 < α < 4). For steep power law indices (α > 8), the measurement uncertainty reduces with T −1/2 . We applied this method to times-of-arrival from the European Pulsar Timing Array and the Parkes Pulsar Timing Array and determined ν probability density functions for 49 millisecond pulsars. We find a statistically significant ν value for PSR B1937+21 and consider possible options for its origin. Significant (95 per cent C.L.) values for ν are also measured for PSRs J0621+1002 and J1022+1001, thus future studies should consider including it in their ephemerides. For binary pulsars with small orbital eccentricities, like PSR J1909−3744, extended ELL1 models should be used to overcome computational issues. The impacts of our results on the detection of gravitational waves are also discussed.

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Using Long-term Millisecond Pulsar Timing to Obtain Physical Characteristics of the Bulge Globular Cluster Terzan 5

Cited by 89 publications

References 79 publications

LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic Field

LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic Field

Disrupted globular clusters and the gamma-ray excess in the Galactic Centre

Correlated timing noise and high-precision pulsar timing: measuring frequency second derivatives as an example

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