  We present the discovery of a 100 kpc low-frequency radio tail behind the
nearby group galaxy, NGC 2276. The extent of this tail is a factor of ten
larger than previously reported from higher-frequency radio and X-ray imaging.
The radio morphology of the galaxy disc and tail suggest that the tail was
produced via ram-pressure stripping, cementing NGC 2276 as the clearest known
example of ram-pressure stripping in a low-mass group. With multi-frequency
imaging, we extract radio continuum spectra between ~50 MHz and 1.2 GHz as a
function of projected distance along the tail. All of the spectra are well fit
by a simple model of spectral ageing due to synchrotron and inverse-Compton
losses. From these fits we estimate a velocity of 870 km/s for the stripped
plasma across the plane of the sky, and a three-dimensional orbital velocity of
970 km/s for NGC 2276. The orbital speed that we derive is in excellent
agreement with the previous estimate from Rasmussen et al., despite it being
derived with a completely independent methodology.
