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Featured researches published by F. D. Seward.


The Astrophysical Journal | 2002

Discovery of X-Ray Pulsations from the Compact Central Source in the Supernova Remnant 3C 58

Stephen S. Murray; Patrick O. Slane; F. D. Seward; Scott M. Ransom; B. M. Gaensler

We report on high time and spatial resolution observations of the supernova remnant (SNR) 3C 58 using the High Resolution Camera (HRC) on the Chandra X-Ray Observatory. These data show a pointlike central source from which we detect 65.68 ms pulsations at 6.7 σ significance. We interpret these pulsations as corresponding to a young rotation-powered pulsar, PSR J0205+6449, that is associated with and powers SNR 3C 58. Analysis of archival Rossi X-Ray Timing Explorer (RXTE) data from 3 years earlier confirms these pulsations and allows us to determine a spin-down rate of = 1.93 × 10-13 s s-1. Assuming a magnetic dipole model for PSR J0205+6449, we infer a surface magnetic field of 3.6 × 1012 G. The historical age for the pulsar (based on its identification with SN 1181) is 820 yr. Taken with the observed period and spin-down rate, we derive an initial spin period of ~60 ms.


The Astrophysical Journal | 1999

DA 530: A Supernova Remnant in a Stellar Wind Bubble

T. L. Landecker; D. Routledge; Stephen P. Reynolds; R.J. Smegal; K. J. Borkowski; F. D. Seward

The high-latitude supernova remnant (SNR) DA 530 (G93.3+6.9), apparently a typical shell remnant, has highly polarized radio continuum emission and a very uniform circumferential magnetic field. We present new radio continuum (408 and 1420 MHz) and H I line observations, made with the Dominion Radio Astrophysical Observatory Synthesis Telescope, and we have made the first detection of X-ray emission from the SNR, using the ROSAT Position-Sensitive Proportional Counter. The SNR lies within a shell of H I, possibly created by an earlier stellar wind, whose kinematic distance is nominally 2.5 kpc but whose actual distance may be larger. The X-ray emission is extremely faint. A Raymond-Smith ionization-equilibrium model fits the data and suggests a very low density, ~0.05 cm-3, consistent with the occurrence of the supernova in a stellar wind cavity, but this model yields an explosion energy 100 times lower than the accepted value. A nonequilibrium shock model, incorporating a range of ionization timescales, is able to give more realistic physical parameters for the supernova remnant. On the balance of the evidence, we place DA 530 at a distance of 3.5 kpc, the largest distance permitted by the H I observations, where it lies 420 pc above the Galactic plane. The explosion, probably a Type Ia supernova, in a low-density cavity has resulted in weak X-ray emission and slow evolution. The explosion energy was 3.9 × 1050 ergs and the age is ~5000 years. The remnant, having swept up 3.9 M☉ in an ambient density of ~0.01 cm-3, is only now in the adiabatic phase, and this explains the absence of detected optical emission. Despite the low ambient density the efficiency of generation of synchrotron radio emission is ~0.4%, higher than in some historical SNRs. The ratio of radio to X-ray flux is about 100 times that for the remnant of SN 1006, which has comparable radio continuum properties. The very uniform magnetic field is not explained. DA 530 joins a small group of remnants at high Galactic latitude with unusual features, perhaps resulting from low ambient densities. Inhomogeneous nonequilibrium ionization models may be required for the interpretation of the X-ray emission from many other older SNRs.


The Astrophysical Journal | 1996

ROSAT Observations of two Southern Supernova Remnants

F. D. Seward; K. E. Kearns; K. L. Rhode

The supernova remnants G327.1 –1.1 and G327.4 + 0.4 (Kes 27) are located 15 apart in the constellation Norma. In 1980, Einstein IPC observations discovered that both were irregular filled-center X-ray sources with possible point sources superposed. This paper describes new ROSAT PSPC observations which both map the diffuse structure and clearly show several unresolved sources in each field. Both remnants have bright emitting regions inside the limb which might indicate the presence of high-energy electrons accelerated by a pulsar. The interior region is more prominent in G327.1-1.1 than in Kes 27. The spectra are relatively strongly absorbed, as expected from distant remnants close to the Galactic plane. Comparison of the X-ray and radio maps of each remnant allows us to attribute some emission to a shell and some to the interior. With this information, a blast-wave model is used to derive approximate ages and energy release. Indications are that the Kes 27 supernova deposited ~1051 ergs in the surrounding medium. The G327.1-1.1 event probably deposited a factor of 3-10 less.


The Astrophysical Journal | 2001

Chandra Observations of the Young Pulsar PSR B0540?69

Philip Kaaret; Herman L. Marshall; T. Aldcroft; Dale Edward Graessle; Margarita Karovska; S. S. Murray; Arnold H. Rots; Norbert S. Schulz; F. D. Seward


The Astrophysical Journal | 2004

CHANDRA VIEW OF KESTEVEN 79: A NEARLY ISOTHERMAL SUPERNOVA REMNANT WITH RICH SPATIAL STRUCTURE

Minghe Sun; F. D. Seward; Randall K. Smith; Patrick O. Slane


The Astrophysical Journal | 2005

Supernova remnants in the Magellanic Clouds. V. The complex interior structure of the N206 supernova remnant

Rosa Nina Murphy Williams; Y.-H. Chu; John R. Dickel; Robert A. Gruendl; F. D. Seward; M. A. Guerrero; G. Hobbs


The Astrophysical Journal | 1995

X-Ray Emission from the Supernova Remnant CTA 1

F. D. Seward; Brian Paul Schmidt; Patrick O. Slane


Monthly Notices of the Royal Astronomical Society | 1978

The Ariel V /SSI/ catalogue of high galactic latitude /absolute value of B greater than 10 deg/ X-ray sources

B. A. Cooke; Martin Ricketts; Tommaso Maccacaro; J. P. Pye; M. Elvis; M. G. Watson; Richard E. Griffiths; K. A. Pounds; I. M. McHardy; Dario Maccagni; F. D. Seward; C. G. Page; Martin J. L. Turner


X-ray Universe 2005 | 2006

New high resolution X-ray studies of magellanic cloud supernova remnants

Rosa Nina Murphy Williams; Y. H. Chu; C.-H. R. Chen; R. A. Gruendl; John R. Dickel; F. D. Seward; M. A. Guerrero; Robin L. Shelton


Archive | 2002

High-Precision X-ray Timing of the Pulsar in 3C 58

Scott M. Ransom; Victoria M. Kaspi; B. M. Gaensler; Stephen S. Murray; E. V. Gotthelf; Patrick O. Slane; F. D. Seward

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Scott M. Ransom

National Radio Astronomy Observatory

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Stephen S. Murray

Smithsonian Astrophysical Observatory

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M. A. Guerrero

Spanish National Research Council

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Andrew H. Szentgyorgyi

Smithsonian Astrophysical Observatory

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