Professor Rob Fender: Publications

An artist's impression of a relativistic jet propagating away from a black hole at close to the speed of light. Such jets are formed by the inner regions of the accretion flow: matter flowing inwards towards the black hole, via processes which are not yet fully understood. The accretion flow emits primarily in X-rays, the relativistic jet in the radio band: by combing observations in each band we can try and understand how such jets form and how much energy they carry away from the black hole.

What can we learn from neutron star X-ray binaries’ jets?

Chapter in Astrophysics and Space Science, Springer Nature (2005) 197-209

Authors:

Simone Migliari, Rob Fender

On the Origin of Radio Emission in the X-Ray States of XTE J1650–500 during the 2001-2002 Outburst

The Astrophysical Journal American Astronomical Society 617:2 (2004) 1272-1283

Authors:

S Corbel, RP Fender, JA Tomsick, AK Tzioumis, S Tingay

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

(2004)

Authors:

TJ Maccarone, JCA Miller-Jones, RP Fender, GG Pooley

Finding Faint Intermediate-mass Black Holes in the Radio Band

(2004)

Authors:

TJ Maccarone, RP Fender, AK Tzioumis

GRS 1915+105: The first three months with INTEGRAL

European Space Agency, (Special Publication) ESA SP (2004) 299-305

Authors:

DC Hannikainen, O Vilhu, J Rodriguez, NJ Westergaard, S Shaw, GG Pooley, T Belloni, AA Zdziarski, RW Hunstead, K Wu, S Brandt, A Castro-Tirado, PA Charles, AJ Dean, P Durouchoux, RP Fender, P Hakala, CR Kaiser, AR King, N Lund, IF Mirabel, J Poutanen

Abstract:

GRS 1915+105 is being observed as part of an Open Time monitoring program with INTEGRAL. Three out of six observations from the monitoring program are presented here, in addition to data obtained through an exchange with other observers. We also present simultaneous RXTE observations of GRS 1915+105. During INTEGRAL Revolution 48 (2003 March 6) the source was observed to be in a highly variable state, characterized by 5-minute quasi-periodic oscillations. During these oscillations, the rise is faster than the decline, and is harder. This particular type of variability has never been observed before. During subsequent INTEGRAL revolutions (2003 March-May), the source was in a steady or "plateau" state (also known as class χaccording to Belloni et al. 2000). Here we discuss both the temporal and spectral characteristics of the source during the first three months of observations. The source was clearly detected with all three gamma-ray and X-ray instruments onboard INTEGRAL.

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