The Local Volume HI Survey (LVHIS)

NGC 5102

NGC 5102 (HIPASS J1321-36) is a large lenticular galaxy of type SA0 at a TRGB distance of 3.40 ± 0.39 Mpc (Karachentsev et al. 2002) located in the outskirts of the Cen A group. Its nearest neighbours are HIPASS J1337-39 (267.5 arcmin), HIPASS J1305-40 (287.2 arcmin), and ESO 324-G024 (298.4 arcmin); projected distances are given in brackets. Our ATCA HI moment maps reveal a large, somewhat asymmetric HI disc with a central HI depression that coincides with the bright stellar body. Most of the galaxy's HI emission resides in a ring-like structure of 3.5 arcmin radius, also seen by van Woerden et al. (1993), surrounded by much fainter emission in the outskirts. A prominent HI extension to the south-west resembles a tidal arm, suggesting ongoing gas accretion. NGC 5102's HI velocity field highlights the lopsided and mildly warped nature of the disc. We measure FHI = 85.4 Jy km/s, within the uncertainties of the HIPASS FHI (Koribalski et al. 2004), resulting in MHI = 2.3 × 108 M. Using the VLA CnD-array van Woerden et al. (1993) only detect the HI emission within the inner disc/ring of NGC 5102 and measure FHI = 50 Jy km/s. Using 3D FAT Kamphuis et al. (2015) obtain an HI rotation curve indicating vrot = 94.3 km/s at Rmax = 10.5 kpc (for i = 75.3 degr and PA = 42.2 degr) and Mdyn = 2 × 1010 M. Based on a stellar population study Davidge (2008) find NGC 5102 to be a post-starburst galaxy. Mitzkus et al. (2016) provide an excellent literature overview and analyse the stellar population and kinematics in the central region of NGC 5102 via MUSE data, suggesting two counter-rotating stellar discs. Faint radio continuum emission is detected in the galaxy core (1.7 ± 0.5 mJy).

Reference: Koribalski et al. 2018 * LVHIS database * LVHIS homepage * next

Last updated on 18 Feb 2018. © Copyright CSIRO