R. N. Manchester

Commonwealth Scientific and Industrial Research Organisation

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Trends

Author Order

Document Type

Co-Authors

G. Hobbs

Australia Telescope National Facility

A. G. Lyne

University of Manchester

M. Bailes

Swinburne University of Technology

M. Krämer

Max Planck Institute for Radio Astronomy

S. Johnston

Australia Telescope National Facility

R. M. Shannon

Swinburne University of Technology

Andrea Possenti

Osservatorio Astronomico di Cagliari

F. Camilo

South African Radio Astronomy Observatory

M. Kerr

United States Naval Research Laboratory

Shi Dai

Western Sydney University

Cooperative Institutions

Commonwealth Scientific and Industrial Research Organisation

120

Max Planck Society

112

Australia Telescope National Facility

Campbell Collaboration

California Institute of Technology

Max Planck Institute for Radio Astronomy

Chinese Academy of Sciences

Stanford University

Centre National de la Recherche Scientifique

Goddard Space Flight Center

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Field

The Parkes multi-beam pulsar survey - I. Observing and data analysis systems, discovery and timing of 100 pulsars

Monthly Notices of the Royal Astronomical Society (2001)

R. N. Manchester A. G. Lyne F. Camilo J. F. Bell V. M. Kaspi

The Parkes multi-beam pulsar survey is a sensitive survey of a strip along the Galactic plane with and to . It uses a 13-beam receiver on the 64-m Parkes radio telescope, receiving two polarizations per beam over a 288-MHz bandwidth centred on 1374 MHz. The receiver and data acquisition systems are described in some detail. For pulsar periods in the range and dispersion measures of less than 300 cm−3 pc, the nominal limiting flux density of the survey is about 0.2 mJy. At shorter or longer periods or higher dispersions, the sensitivity is reduced. Timing observations are carried out for pulsars discovered in the survey for months after confirmation to obtain accurate positions, spin parameters, dispersion measures, pulse shapes and mean flux densities. The survey is proving to be extremely successful, with more than 600 pulsars discovered so far. We expect that, when complete, this one survey will come close to finding as many pulsars as all previous pulsar surveys put together. The newly discovered pulsars tend to be young, distant and of high radio luminosity. They will form a valuable sample for studies of pulsar emission properties, the Galactic distribution and evolution of pulsars, and as probes of interstellar medium properties. This paper reports the timing and pulse shape parameters for the first 100 pulsars timed at Parkes, including three pulsars with periods of less than 100 ms which are members of binary systems. These results are briefly compared with the parameters of the previously known population.

Galactic plane

X-ray pulsar

10.1046/j.1365-8711.2001.04751.x

Cite

Citations (569)

The Parkes Pulsar Timing Array and detection of gravitational waves

36th COSPAR Scientific Assembly (2006)

R. N. Manchester

Source

Cite

Citations (1)

A Census of Pulsar Emission

atnf (2006)

S. Johnston S. M. Ord R. N. Manchester M. Krämer R. T. Edwards

Source

Cite

Citations (0)

SNR G320.4-01.2 and PSR B1509-58: new radio observations of a complex interacting system

Monthly Notices of the Royal Astronomical Society (1999)

B. M. Gaensler K. T. S. Brazier R. N. Manchester S. Johnston A. J. Green

We describe radio continuum and spectral-line observations of the source G320.4-01.2 (MSH 15–52) and the coincident young pulsar B1509-58 made with the Australia Telescope Compact Array. Based on a comparison between X-ray and radio observations, we argue that the two main radio components of G320.4-01.2 are a single supernova remnant (SNR), which H i absorption indicates is at a distance of 5.2 ± 1.4 kpc. A high-resolution correspondence between radio and X-rays argues that the pulsar is interacting with the SNR via an opposed pair of collimated outflows. The outflow itself is seen as an elongated X-ray feature surrounded by a highly polarized radio sheath, while the interaction with the SNR manifests itself as a ring of radio/X-ray knots within the optical nebula RCW 89. We reject the hypothesis that the pulsar outflow powers the entire RCW 89 region.

Outflow

Collimated light

Radio spectrum

Line (geometry)

10.1046/j.1365-8711.1999.02500.x

Cite

Citations (103)

Correlation of gamma-ray fluxes with southern hemisphere CO data

Monthly Notices of the Royal Astronomical Society (1984)

P. A. Riley A. W. Wolfendale Xu Chun-xian R. N. Manchester B. J. Robinson

A new radio survey of the 12CO molecule in the Galactic plane covering the longitude range l:294°–358° is compared with the flux of high energy gamma rays in the same region. A good correlation between the two is found and it is shown that the data are consistent with the hypothesis that most of the gamma-ray flux is produced by the cosmic-ray irradiation of interstellar gas.

Longitude

Galactic plane

10.1093/mnras/206.2.423

Cite

Citations (7)

Binary supermassive black hole environments diminish the gravitational wave signal in the pulsar timing band

Monthly Notices of the Royal Astronomical Society (2014)

Vikram Ravi J. Stuart B. Wyithe R. M. Shannon G. Hobbs R. N. Manchester

We assess the effects of super-massive black hole (SMBH) environments on the gravitational-wave (GW) signal from binary SMBHs. To date, searches with pulsar timing arrays for GWs from binary SMBHs, in the frequency band $\sim1-100$\,nHz, include the assumptions that all binaries are circular and evolve only through GW emission. However, dynamical studies have shown that the only way that binary SMBH orbits can decay to separations where GW emission dominates the evolution is through interactions with their environments. We augment an existing galaxy and SMBH formation and evolution model with calculations of binary SMBH evolution in stellar environments, accounting for non-zero binary eccentricities. We find that coupling between binaries and their environments causes the expected GW spectral energy distribution to be reduced with respect to the standard assumption of circular, GW-driven binaries, for frequencies up to $\sim20$\,nHz. Larger eccentricities at binary formation further reduce the signal in this regime. We also find that GW bursts from individual eccentric binary SMBHs are unlikely to be detectable with current pulsar timing arrays. The uncertainties in these predictions are large, owing to observational uncertainty in SMBH-galaxy scaling relations and the galaxy stellar mass function, uncertainty in the nature of binary-environment coupling, and uncertainty in the numbers of the most massive binary SMBHs. We conclude, however, that low-frequency GWs from binary SMBHs may be more difficult to detect with pulsar timing arrays than currently thought.

10.1093/mnras/stu779

Cite

Citations (80)

H I aperture synthesis of the southern barred spiral NGC 1313

Monthly Notices of the Royal Astronomical Society (1994)

W. L. Peters K. C. Freeman J. R. Forster R. N. Manchester J. G. Ables

Aperture synthesis maps have been made of the late-type barred spiral NGC 1313 in the continuum at 1.4 GHz and in the atomic hydrogen line with resolutions of 1 kpc and 16 km s–1. Analysis of the hydrogen distribution and the velocity field indicates that, in addition to the normal emission from a galaxy of this type, there is a tidal interaction in progress between NGC 1313 and a nearby disrupted satellite galaxy. The interaction has resulted in a loop of hydrogen that may have been pulled out of the plane of NGC 1313. The rest of the velocity field can be interpreted in terms of pure circular rotation, and a rotation curve is derived. At the limit of the rotation data, the dark halo contributes about 85 per cent of the enclosed mass. Half of the continuum emission corresponds to the bar and spiral arms of the galaxy, while the rest is due to a compact object with an unusual (positive) spectral index. A recent analysis of archival optical and X-ray data has led Ryder et al. to identify this compact object as a very unusual Type II supernova (SN 1978K).

Hydrogen line

Barred spiral galaxy

10.1093/mnras/269.4.1025

Cite

Citations (20)

A second measurement of a pulsar braking index

Nature (1985)

R. N. Manchester J. M. Durdin L. M. Newton

Crab Pulsar

Constant (computer programming)

X-ray pulsar

10.1038/313374a0

Cite

Citations (60)

The Parkes Southern Pulsar Survey — III. Timing of long-period pulsars

Monthly Notices of the Royal Astronomical Society (1998)

N. D’Amico B. W. Stappers M. Bailes C. E. Martin J. F. Bell

The Parkes survey of the entire southern sky for millisecond and other low-luminosity pulsars has now been completed. The survey system and initial results were described by Manchester et al. and the final results and population studies are described by Lyne et al. A total of 298 pulsars were detected, including 101 new discoveries of which 17 were millisecond pulsars. Here we report on timing observations at Parkes and Jodrell Bank of the 84 long-period (non-millisecond) pulsars discovered in the survey, including timing solutions for 78 of them. Pulse profiles and arrival times were obtained at several different frequencies over intervals of more than a year, yielding a position, period, period derivative and dispersion measure for each pulsar. Pulse profiles at frequencies near 400 MHz and 600 or 1400 MHz are presented for most of the observed pulsars. Significant timing noise was detected for five pulsars and a glitch was observed in the period of PSR J1123–6259.

Glitch

X-ray pulsar

10.1046/j.1365-8711.1998.01397.x

Cite

Citations (53)

Mode switching and oscillations in PSR B1828–11

Monthly Notices of the Royal Astronomical Society (2019)

I. H. Stairs A. G. Lyne M. Krämer B. W. Stappers J. van Leeuwen

The young pulsar PSR B1828-11 has long been known to show correlated shape and spin-down changes with timescales of roughly 500 and 250 days, perhaps associated with large-scale magnetospheric switching. Here we present multi-hour observations with the Parkes and Green Bank Telescopes at multiple phases across the roughly 500-day cycle and show that the pulsar undergoes mode-changing between two stable, extreme profile states. The fraction of time spent in each profile state naturally accounts for the observed overall "shape parameter" (defined to be 0 for wide profiles and 1 for narrow ones); this and the variable rate of the mode transitions are directly related to the spin-down changes. We observe that the mode transition rate could plausibly function as an additional parameter governing the chaotic behaviour in this object which was proposed earlier by Seymour and Lorimer. Free precession is not needed to account for the variations.

Mode (computer interface)

Precession

10.1093/mnras/stz647

Cite

Citations (28)