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Accretion states and radio loudness in active galactic nuclei: analogies with X-ray binaries

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 372:3 (2006) 1366-1378

Authors:

Elmar G Körding, Sebastian Jester, Rob Fender
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RXTE observations of the first transient Z source XTE J1701-462: shedding new light on mass accretion in luminous neutron star LMXBs

(2006)

Authors:

Jeroen Homan, Michiel van der Klis, Rudy Wijnands, Tomaso Belloni, Rob Fender, Marc Klein-Wolt, Piergiorgio Casella, Mariano Mendez, Elena Gallo, Walter HG Lewin, Neil Gehrels
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A very brief description of LOFAR - the Low Frequency Array

(2006)

Authors:

H Falcke, MP van Haarlem, AG de Bruyn, R Braun, HJA Röttgering, B Stappers, WHWM Boland, HR Butcher, EJ de Geus, L Koopmans, R Fender, J Kuijpers, GK Miley, RT Schilizzi, C Vogt, RAMJ Wijers, M Wise, WN Brouw, JP Hamaker, JE Noordam, T Oosterloo, L Bähren, MA Brentjens, SJ Wijnholds, JD Bregman, WA van Cappellen, AW Gunst, GW Kant, J Reitsma, K van der Schaaf, CM de Vos
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The modulated emission of the ultraluminous X-ray source in NGC 3379

Astrophysical Journal 650:2 I (2006) 879-884

Authors:

G Fabbiano, DW Kim, T Fragos, V Kalogera, AR King, L Angelini, RL Davies, JS Gallagher, S Pellegrini, G Trinchieri, SE Zepf, A Zezas

Abstract:

We report recent Chandra observations of the ULX in the elliptical galaxy NGC 3379 that clearly detect two flux variability cycles. Comparing these data with the Chandra observation of ∼5 years ago, we measure a flux modulation with a period of ∼12.6 hr. Moreover, we find that the emission undergoes a correlated spectral modulation, becoming softer at low flux. We argue that our results establish this source as a ULX binary in NGC 3379. Given the old stellar population of this galaxy, the ULX is likely to be a soft transient; however, historical X-ray sampling suggests that the current "on" phase has lasted ∼10yr. We discuss our results in terms of ADC and wind-feedback models. If the flux modulation is orbital, we can constrain the donor mass and orbital period at the onset of mass transfer within 1.15-1.4 Ṁ and 12.5-17 hr, respectively. The duration of the mass transfer phase so far is probably ∼ 1 Gyr, and the binary has been a soft X-ray transient throughout this time. These constraints are insensitive to the mass of the accretor. © 2006. The American Astronomical Society. All rights reserved.
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LOFAR - Opening up a new window on the Universe

(2006)

Authors:

HJA Rottgering, R Braun, PD Barthel, MP van Haarlem, GK Miley, R Morganti, I Snellen, H Falcke, AG de Bruyn, RB Stappers, WHWM Boland, HR Butcher, EJ de Geus, L Koopmans, R Fender, J Kuijpers, RT Schilizzi, C Vogt, RAMJ Wijers, M Wise, WN Brouw, JP Hamaker, JE Noordam, T Oosterloo, L Bahren, MA Brentjens, SJ Wijnholds, JD Bregman, WA van Cappellen, AW Gunst, GW Kant, J Reitsma, K van der Schaaf, CM de Vos
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