A LOFAR census of non-recycled pulsars: average profiles, dispersion measures, flux densities, and spectra

被引：105

作者：

Bilous, A. V. ^{[1
,2
]}

Kondratiev, V. I. ^{[3
,4
]}

Kramer, M. ^{[5
,6
]}

Keane, E. F. ^{[7
,8
,9
]}

Hessels, J. W. T. ^{[2
,3
]}

Stappers, B. W. ^{[6
]}

Malofeev, V. M. ^{[10
]}

Sobey, C. ^{[3
]}

Breton, R. P. ^{[11
]}

Cooper, S. ^{[6
]}

Falcke, H. ^{[1
,3
]}

Karastergiou, A. ^{[12
,13
,14
]}

Michilli, D. ^{[2
,3
]}

Oslowski, S. ^{[5
,15
]}

Sanidas, S. ^{[2
]}

ter Veen, S. ^{[3
]}

van Leeuwen, J. ^{[2
,3
]}

Verbiest, J. P. W. ^{[5
,15
]}

Weltevrede, P. ^{[6
]}

Zarka, P. ^{[16
,17
]}

Griessmeier, J. -M. ^{[17
,18
]}

Serylak, M. ^{[13
,17
]}

Bell, M. E. ^{[8
,19
]}

Broderick, J. W. ^{[12
]}

Eisloeffel, J. ^{[20
]}

Markoff, S. ^{[2
]}

Rowlinson, A. ^{[2
,3
]}

机构：

[1] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands

[2] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[3] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands

[4] Russian Acad Sci, Lebedev Phys Inst, Ctr Astro Space, Profsoyuznaya Str 84-32, Moscow 117997, Russia

[5] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[6] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England

[7] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Mail H30,POB 218, Hawthorn, Vic 3122, Australia

[8] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, 44 Rosehill St, Redfern 2016, Australia

[9] SKA Org, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England

[10] Pushchino Radio Astron Observ, Pushchino 142290, Moscow Region, Russia

[11] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[12] Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[13] Univ Western Cape, Dept Phys & Astron, Private Bag X17, ZA-7535 Bellville, South Africa

[14] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

[15] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany

[16] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France

[17] Univ Orleans, CNRS, PSL Res Univ, Stn Radioastron Nancay,Observ Paris,OSUC, F-18330 Nancay, France

[18] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France

[19] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia

[20] Thuringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2016年 / 591卷

基金：

欧洲研究理事会;

关键词：

pulsars: general; telescopes; ISM: general; LOW-FREQUENCY; RADIO PULSARS; CRAB PULSAR; SKY SURVEY; WIDE-BAND; GALACTIC DISTRIBUTION; TIMING OBSERVATIONS; TURN-OVER; X-RAY; DISCOVERY;

D O I：

10.1051/0004-6361/201527702

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present first results from a LOFAR census of non-recycled pulsars. The census includes almost all such pulsars known (194 sources) at declinations Dec > 8 degrees and Galactic latitudes vertical bar Gb vertical bar > 3 degrees, regardless of their expected flux densities and scattering times. Each pulsar was observed for >= 20 min in the contiguous frequency range of 110-188 MHz. Full-Stokes data were recorded. We present the dispersion measures, flux densities, and calibrated total intensity profiles for the 158 pulsars detected in the sample. The median uncertainty in census dispersion measures (1.5 X 10(-3) pc cm(-3)) is ten times smaller, on average, than in the ATNF pulsar catalogue. We combined census flux densities with those in the literature and fitted the resulting broadband spectra with single or broken power-law functions. For 48 census pulsars such fits are being published for the first time. Typically, the choice between single and broken power-laws, as well as the location of the spectral break, were highly influenced by the spectral coverage of the available flux density measurements. In particular, the inclusion of measurements below 100MHz appears essential for investigating the lowfrequency turnover in the spectra for most of the census pulsars. For several pulsars, we compared the spectral indices from different works and found the typical spread of values to be within 0.5-1.5, suggesting a prevailing underestimation of spectral index errors in the literature. The census observations yielded some unexpected individual source results, as we describe in the paper. Lastly, we will provide this unique sample of wide-band, low-frequency pulse profiles via the European Pulsar Network Database.

引用

页数：34

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