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Monitoring and rapid follow-up of galactic transients and variables with AMI

Rob Fender (Southampton) Guy Pooley (Cambridge) + many others


Variable and transient source astrophysics with an S-Z telescope...

Pooley & Fender (1997) 2-3000 citations on variable source work (e.g. Gallo, Fender & Pooley 2003: >300 citations)


GRS 1915+105
Tight connection between accretion states and radio emission in black hole X-ray binary These are the best data we have on understanding the connection between accretion flows and jet production in black hole systems

Pooley & Fender (1997) Klein-Wolt, Fender, Pooley + (2002)


Cygnus X-1 Orbital modulation of radio emission

Modelling of modulation in wind of OB companion equivalent to angular resolution of ~50 µ arcsec

Pooley, Fender & Brocksopp (1999) Brocksopp, Fender & Pooley (2002)


Cygnus X-3
AMI-Large part of multiwavelength campaign that demonstrates very high energy (>100 MeV) gamma-ray emission from Cygnus X-3 during phases of radio flaring ­ 'extreme' particle acceleration in the jet (via interaction with the mass donor) Highlight result for Fermi Abdo ... Pooley ++ Science 2009


As well as monitoring bright sources, follow-up of new transients and rapid reporting of events, e.g. recently


Rapid follow-up of possible tidal disruption event (Nature 2011) Radio flare of M81 (see McHardy later)



Over the past decade discovery of radio counterpart of ~10 new black hole candidate binaries, follow-up of symbiotic stars, etc More rapid follow-up and successful detections than any other radio telescope (except maybe VL A) Continue into the future


Radio Transients
All 'next generation' (LOFAR, MeerKAT, ASKAP) have adopted search (and follow-up) of radio transients as key science projects. AMI(-Large) has proved itself to be very suitable for rapid followup and monitoring work How can it fit into this ? MeerKAT and ASKAP are southern hemisphere. LOFAR has an extensive transients key science programme, but 15 GHz is not really optimum for follow up of LOFAR transients because either


Sources are coherent steep spectrum too weak at 15 GHz (and possibly already gone) Sources are synchrotron by the time detected with LOFAR much of the fireworks over




Coordination with APERTIF / SWATS (PI Martin Bell)

If approved, SWATS will be the largest survey for synchrotron radio transients in the northern hemisphere. For a 12hr APERTIF observation ~10Jy we expect 1--10 transients per square degree 10--100 transients per day AMI very well placed to follow the most interesting of these up



Proposal:
AMI to have an official programme ­ including ToO ­ for the follow-up and monitoring of interesting transients. Time allocation of order hours per day. High science return. (we can probably use the rainy periods time samping) Close coordination with LOFAR and WSRT/APERTIF.

Fin.