Pulsars, transients and relativistic astrophysics

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Was the Narrow Line Seyfert 1 RGB J0044+193 ever radio loud?

Astronomy & Astrophysics EDP Sciences 433:2 (2005) 531-533

Authors:

TJ Maccarone, JCA Miller-Jones, RP Fender, GG Pooley
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The VLT-FLAMES Survey of Massive Stars: Observations in the Galactic Clusters NGC 3293, NGC 4755 and NGC 6611

(2005)

Authors:

CJ Evans, SJ Smartt, J-K Lee, DJ Lennon, A Kaufer, PL Dufton, C Trundle, A Herrero, S Simon-Diaz, A de Koter, W-R Hamann, MA Hendry, IK Hunter, MJ Irwin, AJ Korn, R-P Kudritzki, N Langer, MR Mokiem, F Najarro, AWA Pauldrach, N Przybilla, J Puls, RSI Ryans, MA Urbaneja, KA Venn, MR Villamariz
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The distribution of radio plasma in time and space.

Philos Trans A Math Phys Eng Sci 363:1828 (2005) 645-654

Abstract:

The influence of jet-ejected plasma has been an important theme of this meeting; I draw attention to the prevalence of jet-ejected plasma, in particular that which has not been properly accounted for in the past. There are three strands to this paper: important emission which is prominent only at the lowest radio frequencies; relic radio plasma which must exist if even the most basic aspects of radio source evolutionary models are correct; and evidence that some 'radio-quiet' quasars could be FR-I radio sources.
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An expanding radio nebula produced by a giant flare from the magnetar SGR 1806-20

(2005)

Authors:

BM Gaensler, C Kouveliotou, JD Gelfand, GB Taylor, D Eichler, RAMJ Wijers, J Granot, E Ramirez-Ruiz, YE Lyubarsky, RW Hunstead, D Campbell-Wilson, AJ van der Host, MA McLaughlin, RP Fender, MA Garrett, KJ Newton-McGee, DM Palmer, N Gehrels, PM Woods
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Polarisation profiles of southern pulsars at 3.1 GHz

ArXiv astro-ph/0502337 (2005)

Authors:

A Karastergiou, S Johnston, RN Manchester

Abstract:

We present polarisation profiles for 48 southern pulsars observed with the new 10-cm receiver at the Parkes telescope. We have exploited the low system temperature and high bandwidth of the receiver to obtain profiles which have good signal to noise for most of our sample at this relatively high frequency. Although, as expected, a number of profiles are less linearly polarised at 3.1 GHz than at lower frequencies, we identify some pulsars and particular components of profiles in other pulsars which have increased linear polarisation at this frequency. We discuss the dependence of linear polarisation with frequency in the context of a model in which emission consists of the superposition of two, orthogonally polarised modes. We show that a simple model, in which the orthogonal modes have different spectral indices, can explain many of the observed properties of the frequency evolution of both the linear polarisation and the total power, such as the high degree of linear polarisation seen at all frequencies in some high spin-down, young pulsars. Nearly all the position angle profiles show deviations from the rotating vector model; this appears to be a general feature of high-frequency polarisation observations.
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