2012A&A...543A..66H

Query : 2012A&A...543A..66H

2012A&A...543A..66H - Astronomy and Astrophysics, volume 543A66-66 (2012/7-1)

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

HASSALL T.E., STAPPERS B.W., HESSELS J.W.T., KRAMER M., ALEXOV A., ANDERSON K., COENEN T., KARASTERGIOU A., KEANE E.F., KONDRATIEV V.I., LAZARIDIS K., VAN LEEUWEN J., NOUTSOS A., SERYLAK M., SOBEY C., VERBIEST J.P.W., WELTEVREDE P., ZAGKOURIS K., FENDER R., WIJERS R.A.M.J., BAEHREN L., BELL M.E., BRODERICK J.W., CORBEL S., DAW E.J., DHILLON V.S., EISLOEFFEL J., FALCKE H., GRIESSMEIER J.-M., JONKER P., LAW C., MARKOFF S., MILLER-JONES J.C.A., OSTEN R., ROL E., SCAIFE A.M.M., SCHEERS B., SCHELLART P., SPREEUW H., SWINBANK J., TER VEEN S., WISE M.W., WIJNANDS R., WUCKNITZ O., ZARKA P., ASGEKAR A., BELL M.R., BENTUM M.J., BERNARDI G., BEST P., BONAFEDE A., BOONSTRA A.-J., BRENTJENS M., BROUW W.N., BRUEGGEN M., BUTCHER H.R., CIARDI B., GARRETT M.A., GERBERS M., GUNST A.W., VAN HAARLEM M.P., HEALD G., HOEFT M., HOLTIES H., DE JONG A., KOOPMANS L.V.E., KUNIYOSHI M., KUPER G., LOOSE G.M., MAAT P., MASTERS J., McKEAN J.P., MEULMAN H., MEVIUS M., MUNK H., NOORDAM J.E., ORRU E., PAAS H., PANDEY-POMMIER M., PANDEY V.N., PIZZO R., POLATIDIS A., REICH W., ROETTGERING H., SLUMAN J., STEINMETZ M., STERKS C.G.M., TAGGER M., TANG Y., TASSE C., VERMEULEN R., VAN WEEREN R.J., WIJNHOLDS S.J. and YATAWATTA S.

Abstract (from CDS):

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 40-190MHz), the 76-m Lovell Telescope (at 1400MHz) and the Effelsberg 100-m Telescope (at 8000MHz) 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.

Abstract Copyright: ∼

Journal keyword(s): pulsars: general - ISM: general - magnetic fields - telescopes

CDS comments: Paragraph 6.3 B0832+26 is a misprint for PSR B0823+26.

Simbad objects: 13

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Number of rows : 13
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 PSR B0329+54 Psr 03 32 59.3370698592 +54 34 45.028206408           ~ 690 1
2 PSR B0525+21 Psr 05 28 52.308 +22 00 01.00     14.30     ~ 370 0
3 PSR B0809+74 Psr 08 14 59.500 +74 29 05.70           ~ 425 0
4 PSR B0823+26 Psr 08 26 51.5068 +26 37 21.297           ~ 541 1
5 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
6 PSR B0834+06 Psr 08 37 05.64620 +06 10 15.8700           ~ 472 0
7 PSR B1133+16 Psr 11 36 03.09460 +15 51 15.9000           ~ 715 0
8 PSR B1237+25 Psr 12 39 40.386 +24 53 49.87           ~ 497 1
9 PSR B1508+55 Psr 15 09 25.674 +55 31 32.90           ~ 322 1
10 PSR B1642-03 Psr 16 45 02.0330 -03 17 57.200           ~ 394 0
11 PSR B1919+21 Psr 19 21 44.815 +21 53 02.25           ~ 411 0
12 PSR B2036+53 Psr 20 38 03.16 +53 19 12.8           ~ 25 0
13 PSR J2044+4614 Psr 20 44 58.8 +46 14 54           ~ 14 0

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