The H I Tully-Fisher relation of early-type galaxies

Milan den Heijer (1, 2) , Tom A. Oosterloo (3) , Paolo Serra (4) , Gyula I. G. Józsa (2) , Jürgen Kerp (2) , Raffaella Morganti (3) , Michele Cappellari , Timothy A. Davis , Pierre-Alain Duc (5) , Eric Emsellem , Davor Krajnović , Richard M. Mcdermid , Torsten Naab , Anne-Marie Weijmans , P. Tim de Zeeuw

1 MPIFR - Max-Planck-Institut für Radioastronomie
2 AlfA - Argelander-Institut für Astronomie
3 Kapteyn Astronomical Institute [Groningen]
4 CSIRO Astronomy and Space Science
5 AIM (UMR7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation

We study the H iK-band Tully-Fisher relation and the baryonic Tully-Fisher relation for a sample of 16 early-type galaxies, taken from the ATLAS3D sample, which all have very regular H i disks extending well beyond the optical body (≳ 5 Reff). We use the kinematics of these disks to estimate the circular velocity at large radii for these galaxies. We find that the Tully-Fisher relation for our early-type galaxies is offset by about 0.5-0.7 mag from the relation for spiral galaxies, in the sense that early-type galaxies are dimmer for a given circular velocity. The residuals with respect to the spiral Tully-Fisher relation correlate with estimates of the stellar mass-to-light ratio, suggesting that the offset between the relations is mainly driven by differences in stellar populations. We also observe a small offset between our Tully-Fisher relation with the relation derived for the ATLAS3D sample based on CO data representing the galaxies’ inner regions (≲1 Reff). This indicates that the circular velocities at large radii are systematically 10% lower than those near 0.5−1 Reff, in line with recent determinations of the shape of the mass profile of early-type galaxies. The baryonic Tully-Fisher relation of our sample is distinctly tighter than the standard one, in particular when using mass-to-light ratios based on dynamical models of the stellar kinematics. We find that the early-type galaxies fall on the spiral baryonic Tully-Fisher relation if one assumes M/LK = 0.54 M⊙/L⊙ for the stellar populations of the spirals, a value similar to that found by recent studies of the dynamics of spiral galaxies. Such a mass-to-light ratio for spiral galaxies would imply that their disks are 60-70% of maximal. Our analysis increases the range of galaxy morphologies for which the baryonic Tully-Fisher relations holds, strengthening previous claims that it is a more fundamental scaling relation than the classical Tully-Fisher relation.

Mots clés: galaxies: kinematics and dynamics; galaxies: elliptical and lenticular; cD

Domaines: Astrophysique [astro-ph]

Milan den Heijer, Tom A. Oosterloo, Paolo Serra, Gyula I. G. Józsa, Jürgen Kerp, et al.. The H I Tully-Fisher relation of early-type galaxies. Astronomy and Astrophysics - A&A, 2015, 581, pp.A98. ⟨10.1051/0004-6361/201526879⟩. ⟨cea-01383683⟩