TY - JOUR
T1 - The H I 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 - de Zeeuw, P. Tim
PY - 2015/9
Y1 - 2015/9
N2 - 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.
AB - 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.
KW - galaxies: kinematics and dynamics
KW - galaxies: elliptical and lenticular
KW - cD
UR - http://adsabs.harvard.edu/abs/2015A%26A...581A..98D
U2 - 10.1051/0004-6361/201526879
DO - 10.1051/0004-6361/201526879
M3 - Article
VL - 581
JO - Astronomy & astrophysics
JF - Astronomy & astrophysics
SN - 0004-6361
M1 - A98
ER -