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Single Pulses from the Galactic Center Magnetar with the Very Large Array

Published online by Cambridge University Press:  04 June 2018

S. Chatterjee ,
R. S. Wharton ,
J. M. Cordes ,
G. C. Bower ,
B. J. Butler ,
A. T. Deller ,
P. Demorest ,
T. J. W. Lazio ,
W. A. Majid  and
S. M. Ransom
S. Chatterjee
Affiliation:
Cornell University, USA
R. S. Wharton
Affiliation:
Cornell University, USA Max-Planck-Institut für Radioastronomie, Germany
J. M. Cordes
Affiliation:
Cornell University, USA
G. C. Bower
Affiliation:
Academia Sinica Institute of Astronomy and Astrophysics, USA
B. J. Butler
Affiliation:
National Radio Astronomy Observatory, USA
A. T. Deller
Affiliation:
Swinburne University of Technology, Australia
P. Demorest
Affiliation:
National Radio Astronomy Observatory, USA
T. J. W. Lazio
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, USA
W. A. Majid
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, USA
S. M. Ransom
Affiliation:
National Radio Astronomy Observatory, USA
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Abstract

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Phased VLA observations of the Galactic center magnetar J1745-2900 over 8-12 GHz reveal rich single pulse behavior. The average profile is comprised of several distinct components and is fairly stable over day timescales and GHz frequencies. The average profile is dominated by the jitter of relatively narrow pulses. The pulses in each of the four profile components are uncorrelated in phase and amplitude, although the occurrence of pulse components 1 and 2 appear to be correlated. Using a collection of the brightest individual pulses, we verify that the index of the dispersion law is consistent with the expected cold plasma value of 2. The scattering time is weakly constrained, but consistent with previous measurements, while the dispersion measure DM = 1763+3−10 pc cm−3 is lower than previous measurements, which could be a result of time variability in the line-of-sight column density or changing pulse profile shape over time or frequency.

Keywords

instrumentation: interferometerstechniques: interferometricstars: neutronpulsars: individual (J1745–2900)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S337: Pulsar Astrophysics the Next Fifty Years , September 2017 , pp. 263 - 266
Copyright
Copyright © International Astronomical Union 2018 

References

Bower, G. C., Deller, A., Demorest, P., et al. 2015, ApJ, 798, 120CrossRefGoogle Scholar
Chatterjee, S., Law, C. J., Wharton, R. S., et al. 2017, Nature, 541, 58Google Scholar
Eatough, R., Karuppusamy, R., Kramer, M., et al. 2013, The Astronomer’s Telegram, 5040Google Scholar
Law, C. J., Bower, G. C., Burke-Spolaor, S., et al. 2015, ApJ, 807, 16CrossRefGoogle Scholar
Shannon, R. M., & Johnston, S., 2013, MNRAS, 435, L29CrossRefGoogle Scholar