Effelsberg multifrequency pulsar polarimetry

Hoensbroech, A. von; Xilouris, K. M.

doi:10.1051/aas:1997255

Cited by 98 publications

(83 citation statements)

References 2 publications

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“…Of the 26 pulsars, 19 have two or more clearly resolved components, allowing a measurement of ∆φ as listed in Table 1. * These component separations are compared with other measurements made over a range of frequencies (Seiradakis et al 1995;von Hoensbroech & Xilouris 1997;Gould & Lyne 1998;Weisberg et al 1999;Dai et al 2015) in Fig. 4.…”

Section: Frequency Dependence Of Profile Widthsmentioning

confidence: 86%

TMRT Observations of 26 Pulsars at 8.6 GHz

Zhao

Yan

et al. 2017

ApJ

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Integrated pulse profiles at 8.6 GHz obtained with the Shanghai Tian Ma Radio Telescope (TMRT) are presented for a sample of 26 pulsars. Mean flux densities and pulse width parameters of these pulsars are estimated. For eleven pulsars these are the first high-frequency observations and for a further four, our observations have a better signal-to-noise ratio than previous observations. For one (PSRs J0742−2822) the 8.6 GHz profiles differs from previously observed profiles. A comparison of 19 profiles with those at other frequencies shows that in nine cases the separation between the outmost leading and trailing components decreases with frequency, roughly in agreement with radius-to-frequency mapping, whereas in the other ten the separation is nearly constant. Different

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Section: Frequency Dependence Of Profile Widthsmentioning

confidence: 86%

TMRT Observations of 26 Pulsars at 8.6 GHz

Zhao

Yan

et al. 2017

ApJ

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“…At higher frequencies, a different and quite unusual phenomenon appears, where the leading edge of the profile becomes almost fully linearly polarized. This can be seen at and above 925 MHz in Gould & Lyne and is very finely exhibited in the 1.41-and 1.71-GHz polarimetry of von Hoensbroech & Xilouris (1997). Nearly complete linear polarization is virtually unknown among conal single (S d ) stars, and remarkably suggests (a) that only one polarization mode is observed in this longitude range; and (b) that it is almost fully linearly polarized!…”

Section: ) Folded At 60mentioning

confidence: 91%

“…Properties of these drifting subpulses have been investigated by many authors over the past three decades (e.g., Cole 1970;Taylor & Huguenin 1971;Backer et al 1975). Its polarization properties have also been studied in detail by various investigators von Hoensbroech & Xilouris 1997;Gould & Lyne 1998).…”

Section: Introductionmentioning

confidence: 99%

PSR B0809+74: Understanding its perplexing subpulse-separation (P$_\mathsf{2}$) variations

Rankin¹,

Ramachandran

Suleymanova

2005

A&A

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Abstract. The longitude separation between adjacent drifting subpulses, P 2 , is roughly constant for many pulsars. It was then perplexing when pulsar B0809+74 was found to exhibit substantial variations in this measure, both with wavelength and with longitude position within the pulse window. We analyze these variations between 40 and 1400 MHz, and we show that they stem primarily from the incoherent superposition of the two orthogonal modes of polarization.

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“…(1) Hobbs et al (2004); (2) using the model in Cordes & Lazio (2002); (3) Kijak et al (2007); (4) Lorimer et al (1995); (5) Von Hoensbroech (1998).…”

Section: The Nearby Isolated Pulsar Psr J1825−1446mentioning

confidence: 99%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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Context. The gamma-ray binary LS 5039 and the isolated pulsar PSR J1825−1446 were proposed to have been formed in the supernova remnant (SNR) G016.8−01.1. Aims. We aim to obtain the Galactic trajectory of LS 5039 and PSR J1825−1446 to find their origin in the Galaxy, and in particular to check their association with SNR G016.8−01.1 to restrict their age. Methods. By means of radio and optical observations we obtained the proper motion and the space velocity of the sources. Results. The proper motion of PSR J1825−1446 corresponds to a transverse space velocity of 690 km s −1 at a distance of 5 kpc. Its Galactic velocity at different distances is not compatible with the expected Galactic rotation. The velocity and characteristic age of PSR J1825−1446 make it incompatible with SNR G016.8−01.1. There are no clear OB associations or SNRs crossing the past trajectory of PSR J1825−1446. We estimate the age of the pulsar to be 80-245 kyr, which is compatible with its characteristic age. The proper motion of LS 5039 is μ α cos δ = 7.09 and μ δ = −8.82 mas yr −1 . The association of LS 5039 with SNR G016.8−01.1 is unlikely, although we cannot discard it. The system would have had to be formed in the association Ser OB2 (at 2.0 kpc) if the age of the system is 1.0-1.2 Myr, or in the association Sct OB3 (distance 1.5-2 kpc) for an age of 0.1-0.2 Myr. If the system were not formed close to Ser OB2, the pseudo-synchronization of the orbit would be unlikely. Conclusions. PSR J1825−1446 is a high-velocity isolated pulsar ejected from the Galaxy. The distance to LS 5039, which needs to be constrained by future astrometric missions such as Gaia, is a key parameter for restricting its origin and age.

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Effelsberg multifrequency pulsar polarimetry

Cited by 98 publications

References 2 publications

TMRT Observations of 26 Pulsars at 8.6 GHz

TMRT Observations of 26 Pulsars at 8.6 GHz

PSR B0809+74: Understanding its perplexing subpulse-separation (P$_\mathsf{2}$) variations

On the origin of LS 5039 and PSR J1825−1446

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