Wide-band simultaneous observations of pulsars: disentangling dispersion measure and profile variations

被引:88
作者
Hassall, T. E. [1 ]
Stappers, B. W. [1 ]
Hessels, J. W. T. [2 ,3 ]
Kramer, M. [1 ,4 ]
Alexov, A. [3 ]
Anderson, K. [3 ]
Coenen, T. [3 ]
Karastergiou, A. [5 ]
Keane, E. F. [4 ]
Kondratiev, V. I. [2 ]
Lazaridis, K. [4 ]
van Leeuwen, J. [2 ,3 ]
Noutsos, A. [4 ]
Serylak, M. [6 ,7 ]
Sobey, C. [4 ]
Verbiest, J. P. W. [4 ]
Weltevrede, P. [1 ]
Zagkouris, K. [5 ]
Fender, R. [8 ]
Wijers, R. A. M. J. [3 ]
Bahren, L. [3 ]
Bell, M. E. [8 ,9 ]
Broderick, J. W. [8 ]
Corbel, S. [10 ,11 ,12 ]
Daw, E. J. [13 ]
Dhillon, V. S. [13 ]
Eisloeffel, J. [14 ]
Falcke, H. [2 ,4 ,15 ]
Griessmeier, J. -M. [7 ]
Jonker, P. [15 ,16 ,17 ]
Law, C. [3 ,18 ]
Markoff, S. [3 ]
Miller-Jones, J. C. A. [3 ,19 ]
Osten, R. [20 ]
Rol, E. [3 ]
Scaife, A. M. M. [8 ]
Scheers, B. [3 ,21 ]
Schellart, P. [15 ]
Spreeuw, H. [3 ]
Swinbank, J. [3 ]
ter Veen, S. [15 ]
Wise, M. W. [2 ,3 ]
Wijnands, R. [3 ]
Wucknitz, O. [22 ]
Zarka, P. [23 ]
Asgekar, A. [2 ]
Bell, M. R. [24 ]
Bentum, M. J. [2 ]
Bernardi, G. [17 ]
Best, P. [25 ]
机构
[1] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England
[2] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands
[3] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands
[4] Max Planck Inst Radioastron, D-53121 Bonn, Germany
[5] Univ Oxford, Oxford OX1 3RH, England
[6] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France
[7] CNRS, UMR 7328, LPC2E, F-45071 Orleans 02, France
[8] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England
[9] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia
[10] Univ Paris 07, F-91191 Gif Sur Yvette, France
[11] CEA Saclay, UMR AIM, Serv Astrophys, F-91191 Gif Sur Yvette, France
[12] Inst Univ France, F-75005 Paris, France
[13] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England
[14] Thuringer Landessternwarte, D-07778 Tautenburg, Germany
[15] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands
[16] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands
[17] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[18] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA USA
[19] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia
[20] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[21] CWI, NL-1090 GB Amsterdam, Netherlands
[22] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany
[23] UPMC, CNRS, Observ Paris, LESIA, F-92195 Meudon, France
[24] Max Planck Inst Astrophys, D-85741 Garching, Germany
[25] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland
[26] Jacobs Univ Bremen, D-28759 Bremen, Germany
[27] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands
[28] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia
[29] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands
[30] NRAO Headquarters, Charlottesville, VA 22903 USA
[31] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France
[32] Leibniz Inst Fr Astrophys Potsdam AIP, D-14482 Potsdam, Germany
[33] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands
关键词
pulsars: general; ISM: general; magnetic fields; telescopes; EMPIRICAL-THEORY; RADIO-EMISSION; INTERSTELLAR SCATTERING; SUPERDISPERSION DELAY; FREQUENCY-DEPENDENCE; SPECTRAL BEHAVIOR; PULSES; REFRACTION; PROPAGATION; ABSORPTION;
D O I
10.1051/0004-6361/201218970
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Dispersion in the interstellar medium is a well known phenomenon that follows a simple relationship, which has been used to predict the time delay of dispersed radio pulses since the late 1960s. We performed wide-band simultaneous observations of four pulsars with LOFAR (at 40-190 MHz), the 76-m Lovell Telescope (at 1400 MHz) and the Effelsberg 100-m Telescope (at 8000 MHz) to test the accuracy of the dispersion law over a broad frequency range. In this paper we present the results of these observations which show that the dispersion law is accurate to better than 1 part in 105 across our observing band. We use this fact to constrain some of the properties of the interstellar medium along the line-of-sight and use the lack of any aberration or retardation effects to determine upper limits on emission heights in the pulsar magnetosphere. We also discuss the effect of pulse profile evolution on our observations, and the implications that it could have for precision pulsar timing projects such as the detection of gravitational waves with pulsar timing arrays.
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页数:20
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