TY - JOUR
T1 - The HI Tully-Fisher relation of early-Type galaxies
AU - Den Heijer, Milan
AU - Oosterloo, Tom A.
AU - Serra, Paolo
AU - Józsa, Gyula I G
AU - Kerp, Jürgen
AU - Morganti, Raffaella
AU - Cappellari, Michele
AU - Davis, Timothy A.
AU - Duc, Pierre Alain
AU - Emsellem, Eric
AU - Krajnović, Davor
AU - McDermid, Richard M.
AU - Naab, Torsten
AU - Weijmans, Anne Marie
AU - Tim De Zeeuw, P.
PY - 2015/9/1
Y1 - 2015/9/1
N2 - We study the HiK-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 Hi 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/Lfor 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.
AB - We study the HiK-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 Hi 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/Lfor 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.
UR - http://www.scopus.com/inward/record.url?scp=84941345964&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201526879
DO - 10.1051/0004-6361/201526879
M3 - Article
AN - SCOPUS:84941345964
SN - 0004-6361
VL - 581
SP - 1
EP - 11
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A98
ER -