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WALLABY Early Science – IV. ASKAP H i imaging of the nearby galaxy IC 5201

2019; Oxford University Press; Volume: 488; Issue: 4 Linguagem: Inglês

10.1093/mnras/stz2063

1365-2966

D. Kleiner, B. Koribalski, P. Serra, M. T. Whiting, T. Westmeier, O. I. Wong, P. Kamphuis, Attila Popping, G. Bekiaris, Ahmed Elagali, Bi‐Qing For, K. Lee-Waddell, Juan P. Madrid, T. Reynolds, J. Rhee, Li Shao, L. Staveley‐Smith, Jing Wang, C. S. Anderson, J. D. Collier, S. M. Ord, M. A. Voronkov,

Stellar, planetary, and galactic studies

We present a Wide-field ASKAP L-Band Legacy All-sky Blind surveY (WALLABY) study of the nearby ($v_{\rm sys}$ = 915 km s$^{-1}$) spiral galaxy IC 5201 using the Australian Square Kilometre Array Pathfinder (ASKAP). IC 5201 is a blue, barred spiral galaxy that follows the known scaling relations between stellar mass, SFR, HI mass and diameter. We create a four-beam mosaicked HI image cube, from 175 hours of observations made with a 12-antenna sub-array. The RMS noise level of the cube is 1.7 mJy beam$^{-1}$ per channel, equivalent to a column density of $N_{\rm HI}$ = 1.4 $\times$ 10$^{20}$ cm$^{-2}$ over 25 km s$^{-1}$. We report 9 extragalactic HI detections $-$ 5 new HI detections including the first velocity measurements for 2 galaxies. These sources are IC 5201, 3 dwarf satellite galaxies, 2 galaxies and a tidal feature belonging to the NGC 7232/3 triplet and 2 potential infalling galaxies to the triplet. There is evidence of a previous tidal interaction between IC 5201 and the irregular satellite AM 2220$-$460. A close fly-by is likely responsible for the asymmetric optical morphology of IC 5201 and warping its disc, resulting in the irregular morphology of AM 2220$-$460. We quantify the HI kinematics of IC 5201, presenting its rotation curve as well as showing that the warp starts at 14 kpc along the major axis, increasing as a function of radius with a maximum difference in position angle of 20$^\circ$. There is no evidence of stripped HI, triggered or quenched star formation in the system as measured using DECam optical and $GALEX$ UV photometry.