Roberts, I. D.I. D.Roberts0000-0003-1581-0092van Weeren, R. J.R. J.van Weerende Gasperin, F.F.de GasperinBotteon, A.A.BotteonEdler, H. W.H. W.EdlerIgnesti, A.A.IgnestiMatijević, L.L.MatijevićTomičić, N.N.Tomičić2024-12-092024-12-092024http://hdl.handle.net/20.500.12386/39908We 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<SUP>‑1</SUP> for the stripped plasma across the plane of the sky, and a three-dimensional orbital velocity of 970 km s<SUP>‑1</SUP> for NGC 2276. The orbital speed that we derive is in excellent agreement with the previous estimates from an X-ray shock analysis, despite the completely independent methodology.galaxies: groups: individual: NGC 2300galaxies: individual: NGC 2276galaxies: magnetic fieldsgalaxies: spiralgalaxies: starburstgalaxies: star formationAstrophysics - Astrophysics of Galaxiesarticle10.1051/0004-6361/20245067210.48550/arXiv.2406.092212024A&A...689A..22R