Discovery of 424 millisecond pulsations from the radio-quiet neutron star in the supernova remnant PKS 1209-51/52

V. E. Zavlin; G. G. Pavlov; D. Sanwal; J. Trümper

doi:10.1086/312866

Discovery of 424 millisecond pulsations from the radio-quiet neutron star in the supernova remnant PKS 1209-51/52

V. E. Zavlin, G. G. Pavlov, D. Sanwal, J. Trümper

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Abstract

The central source of the supernova remnant PKS 1209-51/52 was observed with the Advanced CCD Imaging Spectrometer aboard Chandra X-Ray Observatory on 2000 January 6-7. The use of the continuous clocking mode allowed us to perform the timing analysis of the data with a time resolution of 2.85 ms and to find a period P = 0.42412924 s ± 0.23 μs. The detection of this short period proves that the source is a neutron star. It may be either an active pulsar with an unfavorably directed radio beam or a truly radio-silent neutron star whose X-ray pulsations are caused by a nonuniform distribution of surface temperature. To infer the actual properties of this neutron star, the period derivative should be measured.

Original language	English (US)
Pages (from-to)	L25-L28
Journal	Astrophysical Journal
Volume	540
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/312866
State	Published - Sep 1 2000

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/312866

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title = "Discovery of 424 millisecond pulsations from the radio-quiet neutron star in the supernova remnant PKS 1209-51/52",

abstract = "The central source of the supernova remnant PKS 1209-51/52 was observed with the Advanced CCD Imaging Spectrometer aboard Chandra X-Ray Observatory on 2000 January 6-7. The use of the continuous clocking mode allowed us to perform the timing analysis of the data with a time resolution of 2.85 ms and to find a period P = 0.42412924 s ± 0.23 μs. The detection of this short period proves that the source is a neutron star. It may be either an active pulsar with an unfavorably directed radio beam or a truly radio-silent neutron star whose X-ray pulsations are caused by a nonuniform distribution of surface temperature. To infer the actual properties of this neutron star, the period derivative should be measured.",

author = "Zavlin, {V. E.} and Pavlov, {G. G.} and D. Sanwal and J. Tr{\"u}mper",

note = "Funding Information: We thank Glenn Allen, who provided the algorithm to correct the event times in CC mode. We are grateful to Gordon Gar-mire, John Nousek, Leisa Townsley, and George Chartas for the useful advice on the analysis of ACIS data. This work was partly supported by SAO grant GO0-1012X. Copyright: Copyright 2020 Elsevier B.V., All rights reserved.",

year = "2000",

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doi = "10.1086/312866",

language = "English (US)",

volume = "540",

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AU - Zavlin, V. E.

AU - Pavlov, G. G.

AU - Sanwal, D.

AU - Trümper, J.

N1 - Funding Information: We thank Glenn Allen, who provided the algorithm to correct the event times in CC mode. We are grateful to Gordon Gar-mire, John Nousek, Leisa Townsley, and George Chartas for the useful advice on the analysis of ACIS data. This work was partly supported by SAO grant GO0-1012X. Copyright: Copyright 2020 Elsevier B.V., All rights reserved.

PY - 2000/9/1

Y1 - 2000/9/1

N2 - The central source of the supernova remnant PKS 1209-51/52 was observed with the Advanced CCD Imaging Spectrometer aboard Chandra X-Ray Observatory on 2000 January 6-7. The use of the continuous clocking mode allowed us to perform the timing analysis of the data with a time resolution of 2.85 ms and to find a period P = 0.42412924 s ± 0.23 μs. The detection of this short period proves that the source is a neutron star. It may be either an active pulsar with an unfavorably directed radio beam or a truly radio-silent neutron star whose X-ray pulsations are caused by a nonuniform distribution of surface temperature. To infer the actual properties of this neutron star, the period derivative should be measured.

AB - The central source of the supernova remnant PKS 1209-51/52 was observed with the Advanced CCD Imaging Spectrometer aboard Chandra X-Ray Observatory on 2000 January 6-7. The use of the continuous clocking mode allowed us to perform the timing analysis of the data with a time resolution of 2.85 ms and to find a period P = 0.42412924 s ± 0.23 μs. The detection of this short period proves that the source is a neutron star. It may be either an active pulsar with an unfavorably directed radio beam or a truly radio-silent neutron star whose X-ray pulsations are caused by a nonuniform distribution of surface temperature. To infer the actual properties of this neutron star, the period derivative should be measured.

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ER -

Discovery of 424 millisecond pulsations from the radio-quiet neutron star in the supernova remnant PKS 1209-51/52

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