The MeerKAT Fornax Survey. III. Ram-pressure stripping of the tidally interacting galaxy NGC 1427A in the Fornax cluster

• Published in: arXiv.org 2024-07
• Main Authors: Serra, P, Oosterloo, T A, Kamphuis, P, Jozsa, G I G, W J G de Blok, Bryan, G L, van Gorkom, J H, Iodice, E, Kleiner, D, Loni, A, Loubser, S I, Maccagni, F M, Molnar, D, Peletier, R, Pisano, D J, Ramatsoku, M, Smith, M W L, Verheijen, M A W, Zabel, N
• Format: Article
• Language: English
• Subjects: Clusters; Galaxy distribution; Interacting galaxies; Irregular galaxies; Kinematics; Pressure effects; Ram pressure; Stellar mass; Velocity gradient
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2407.09082

We present MeerKAT Fornax Survey HI observations of NGC 1427A, a blue irregular galaxy with a stellar mass of 2e+9 Msun located near the centre of the Fornax galaxy cluster. Thanks to the excellent resolution (1 to 6 kpc spatially, 1.4 km/s in velocity) and HI column density sensitivity (4e+19/cm^2 to 1e+18/cm^2 depending on resolution), our data deliver new insights on the long-debated interaction of this galaxy with the cluster environment. We confirm the presence of a broad, one-sided, starless HI tail stretching from the outer regions of the stellar body and pointing away from the cluster centre. We find the tail to have 50% more HI (4e+8 Msun) and to be 3 times longer (70 kpc) than in previous observations. In fact, we detect scattered HI clouds out to 300 kpc from the galaxy in the direction of the tail -- possibly the most ancient remnant of the passage of NGC 1427A through the intracluster medium of Fornax. Both the velocity gradient along the HI tail and the peculiar kinematics of HI in the outer region of the stellar body are consistent with the effect of ram pressure given the line-of-sight motion of the galaxy within the cluster. However, several properties cannot be explained solely by ram pressure and suggest an ongoing tidal interaction. This includes: the close match between dense HI and stars within the disturbed stellar body; the abundant kinematically-anomalous HI; and the inversion of the HI velocity gradient near the base of the HI tail. We rule out an interaction with the cluster tidal field, and conclude that NGC 1427A is the result of a high-speed galaxy encounter or of a merger started at least 300 Myr ago, where ram pressure shapes the distribution and kinematics of the HI in the perturbed outer stellar body and in the tidal tails.