Kinematics of the lens host S0 galaxy NGC 1553: Role of secular processes

¹ Indian Institute of Astrophysics, Kormangala II Block, Bengaluru 560034, India
² Department of Physics, Pondicherry University, R.V.Nagar, Kalapet, Puducherry 605014, India
³ Observatoire de Paris, LUX, College de France, CNRS, PSL University, Sorbonne University, F-75014 Paris, France

^⋆ Corresponding author: saili.keshri@iiap.res.in

Received: 10 July 2025
Accepted: 11 September 2025

Abstract

We investigated the central structure of the S0 galaxy NGC 1553, to understand its origin and the underlying dynamical processes that shape it. The high-resolution integral field spectroscopic data from the Multi Unit Spectroscopic Explorer (MUSE) reveal a well-ordered rotation pattern, consisting of a (i) rapidly rotating nuclear disc that is somewhat decoupled from the main disc, and (ii) an inner lens; we collectively refer to these structures as the ‘disc-lens’. The central peak in the velocity dispersion indicates the presence of a classical bulge. The nuclear disc is dynamically colder than the surrounding disc, while the lens is dynamically hotter. The higher-order Gauss–Hermite moments, h₃ and h₄, further characterise the stellar kinematics. An anti-correlation between the line-of-sight velocity and skewness (h₃) is consistent with regular rotation. In contrast, the ring-like increase in kurtosis (h₄) confirms the presence of the nuclear disc component. Unsharp masking of HST images has previously revealed a nuclear bar and faint spiral structures within the central ∼10 arcsec, supporting the role of secular evolution. The mass-weighted stellar age map reveals an old stellar population in the central regions, with a high metallicity that suggests the in situ formation of the disc–lens from disc material. We discuss possible formation scenarios for the disc–lens, including both minor mergers and secular processes, and examine the influence of the Dorado group environment on NGC 1553. Our findings suggest that the disc–lens in NGC 1553 formed during the early stages of the galaxy’s evolution. However, its subsequent development has been shaped by internal and external processes. These results provide new insights into the origin and evolution of kinematically distinct substructures in S0 galaxies.