期刊
ASTRONOMY & ASTROPHYSICS
卷 581, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201526879
关键词
galaxies: kinematics and dynamics; galaxies: elliptical and lenticular, cD
资金
- International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn
- International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne
- Deutsche Forschungsgemeinschaft (DFG) [KE 757/7-2, KE 757/9-1]
- Royal Society University Research Fellowship
- UK Research Councils [PP/E001114/1, ST/H002456/1, PPA/V/S/2002/00553, PP/E001564/1, ST/H504862/1]
- ESO fellowship
- DFG Cluster of Excellence Origin and Structure of the Universe
- Leverhulme Trust Early Career Fellowship
- European Community [229517]
- ESO
- Science and Technology Facilities Council [ST/L004496/2, ST/L004496/1] Funding Source: researchfish
- STFC [ST/H002456/1, ST/L004496/1, ST/L004496/2] Funding Source: UKRI
We study the Hi K-band Tully-Fisher relation and the baryonic Tully-Fisher relation for a sample of 16 early-type galaxies, taken from the ATLAS(3D) sample, which all have very regular Hi disks extending well beyond the optical body (greater than or similar to 5 R-eff). 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 ATLAS(3D) sample based on CO data representing the galaxies' inner regions (less than or similar to 1 R-eff). This indicates that the circular velocities at large radii are systematically 10% lower than those near 0.5-1 R-eff, 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/L-K = 0.54 M-circle dot/L-circle dot 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.
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