The extended structure of the dwarf irregular galaxies Sextans A and Sextans B

Signatures of tidal distortion in the outskirts of the Local Group^{⋆,⋆⋆,⋆⋆⋆}

¹ INAF − Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
e-mail: michele.bellazzini@oabo.inaf.it
² European Southern Observatory, Av. Alonso de Córdova, 3107, 19001 Casilla, Santiago, Chile
³ Dipartimento di Astronomia − Università degli Studi di Bologna, via Ranzani 1, 40127 Bologna, Italy
⁴ Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands
⁵ Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
⁶ INAF − Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio, Italy
⁷ Institute of Astrophysics, Pontificia Universidad Catolica de Chile, avenida Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile

Received: 17 February 2014
Accepted: 20 March 2014

Abstract

We present a detailed study of the stellar and H i structure of the dwarf irregular galaxies Sextans A and Sextans B, members of the NGC 3109 association. We use newly obtained deep (r ≃ 26.5) and wide-field g and r photometry to extend the surface brightness (SB) profiles of the two galaxies down to μ_V ≃ 31.0 mag/arcsec². We find that both galaxies are significantly more extended than previously traced with surface photometry, out to ~4 kpc from their centres along their major axes. Older stars are found to have more extended distribution than younger populations. We obtain the first estimate of the mean metallicity for the old stars in Sex B, from the colour distribution of the red giant branch, ⟨[Fe/H]⟩ = −1.6. The SB profiles show significant changes of slope and cannot be fitted with a single Sérsic model. Both galaxies have HI discs as massive as their respective stellar components. In both cases the H i discs display solid-body rotation with maximum amplitude of ~50 km s^-1 (albeit with significant uncertainty due to the poorly constrained inclination), implying a dynamical mass ~10⁹ M_⊙, a mass-to-light ratio M / L_V ~ 25, and a dark-to-baryonic mass ratio of ~10. The distribution of the stellar components is more extended than the gaseous disc in both galaxies. We find that the main, approximately round, stellar body of Sex A is surrounded by an elongated low-SB stellar halo that can be interpreted as a tidal tail, similar to that found in another member of the same association (Antlia). We discuss these, as well as other evidence of tidal disturbance, in the framework of a past passage of the NGC 3109 association close to the Milky Way, which has been hypothesised by several authors and is also supported by the recently discovered filamentary configuration of the association itself.