2015A&A...581A..98D


Query : 2015A&A...581A..98D

2015A&A...581A..98D - Astronomy and Astrophysics, volume 581A, 98-98 (2015/9-1)

The HI Tully-Fisher relation of early-type galaxies.

DEN HEIJER M., OOSTERLOO T.A., SERRA P., JOZSA G.I.G., KERP J., MORGANTI R., CAPPELLARI M., DAVIS T.A., DUC P.-A., EMSELLEM E., KRAJNOVIC D., McDERMID R.M., NAAB T., WEIJMANS A.-M. and DE ZEEUW P.T.

Abstract (from CDS):

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 ATLAS3D sample, which all have very regular Hi disks extending well beyond the optical body (>5Reff). 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 0.5-0.7mag 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 (≲1Reff). This indicates that the circular velocities at large radii are systematically 10% lower than those near 0.5-1Reff, 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=0.54M/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.

Abstract Copyright:

Journal keyword(s): galaxies: kinematics and dynamics - galaxies: elliptical and lenticular, cD

Simbad objects: 36

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Number of rows : 36
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 UGC 3960 G 07 40 22.7432879424 +23 16 29.952956244   15.0       ~ 61 0
2 NGC 2594 G 08 27 17.1616179576 +25 52 43.686523164   15.0       ~ 49 0
3 NGC 2685 Sy2 08 55 34.7027817000 +58 44 03.876540108   13.68 12.70     ~ 421 1
4 NGC 2764 GiG 09 08 17.5023934176 +21 26 36.007547028   13.9       ~ 113 0
5 NGC 2824 AGN 09 19 02.2176446256 +26 16 11.997810444   14.3       ~ 114 1
6 NGC 2859 G 09 24 18.5266762368 +34 30 48.561305832   11.8       ~ 247 0
7 NGC 2974 Sy2 09 42 33.2918467632 -03 41 57.038311068   12.19   10.77   ~ 426 0
8 NGC 3032 AGN 09 52 08.1524118072 +29 14 10.364182440   13.87 13.28     ~ 244 0
9 Mrk 25 AGN 10 03 51.9487763664 +59 26 10.665521556   14.96 14.42     ~ 127 0
10 NGC 3182 Sy2 10 19 33.0239134272 +58 12 20.586154752   13.0       ~ 104 0
11 NGC 3414 GiP 10 51 16.2099174408 +27 58 30.297624852   12.1       ~ 316 0
12 NGC 3489 GiG 11 00 18.5483994744 +13 54 04.206202668 11.46 11.12 10.29     ~ 385 1
13 NGC 3499 GiG 11 03 11.0483985840 +56 13 18.448285980   14.3       ~ 71 0
14 NGC 3522 GiG 11 06 40.4644062552 +20 05 07.900946304   14.13       ~ 99 1
15 Mrk 1282 GiC 11 07 24.6828148008 +21 39 25.578974664   14.8       ~ 67 0
16 NGC 3619 GiG 11 19 21.5781353400 +57 45 28.018459368   12.6       ~ 163 0
17 NGC 3626 GiG 11 20 03.8069651160 +18 21 24.543304164   11.2       ~ 247 0
18 NGC 3838 GiP 11 44 13.7648109936 +57 56 53.538816012   12.7       ~ 83 0
19 NGC 3941 Sy2 11 52 55.3609498656 +36 59 10.716212904   11.45 11.62 9.97   ~ 237 0
20 NGC 3945 GiG 11 53 13.6081388304 +60 40 32.125024704   11.6       ~ 232 0
21 NGC 3998 SyG 11 57 56.1334044408 +55 27 12.922443432   11.64 12.10 10.09   ~ 615 2
22 NGC 4036 LIN 12 01 26.7603659808 +61 53 44.625848784   12.18 11.20     ~ 249 0
23 NGC 4150 GiG 12 10 33.655 +30 24 05.35 12.72 12.44 11.64     ~ 300 2
24 NGC 4203 LIN 12 15 05.0549203560 +33 11 50.383965120   12.98 11.99     ~ 477 2
25 NGC 4262 GiG 12 19 30.5694336288 +14 52 39.517143276 13.00 12.49 11.55     ~ 346 1
26 NGC 4278 LIN 12 20 06.82538739 +29 16 50.7134758 11.54 11.09 10.16     ~ 918 2
27 NGC 4710 H2G 12 49 38.958 +15 09 55.76   11.6       ~ 300 0
28 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4599 2
29 NGC 5103 GiG 13 20 30.1029602496 +43 05 02.219249040   13.6       ~ 89 0
30 NGC 5173 GiP 13 28 25.2798599736 +46 35 29.890508928   13.10       ~ 139 1
31 NGC 5422 GiG 14 00 42.0190513968 +55 09 51.863031684   13.1       ~ 148 0
32 NGC 5582 GiP 14 20 43.1108121696 +39 41 36.927369816   13.0       ~ 111 0
33 NGC 5631 Sy2 14 26 33.2913328320 +56 34 57.424681848   13.51 12.55     ~ 171 0
34 UGC 9519 G 14 46 21.127 +34 22 14.34   14.4       ~ 90 0
35 M 102 SyG 15 06 29.561 +55 45 47.91 11.12 10.74 9.89     ~ 533 3
36 NGC 6798 G 19 24 03.1663172664 +53 37 29.387614044   14.5       ~ 60 0

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2023.01.30-05:45:24

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