2017A&A...604A.105T


Query : 2017A&A...604A.105T

2017A&A...604A.105T - Astronomy and Astrophysics, volume 604A, 105-105 (2017/8-1)

Formation of S0 galaxies through mergers. Evolution in the Tully-Fisher relation since z ∼ 1.

TAPIA T., ELICHE-MORAL M.C., ACEVES H., RODRIGUEZ-PEREZ C., BORLAFF A. and QUEREJETA M.

Abstract (from CDS):

Context. Lenticular (S0) galaxies are known to derive from spiral galaxies. The fact that S0s nearly obey the Tully-Fisher relation (TFR) at z∼0 (as spirals have done in the last ∼9Gyr) is considered an argument against their major-merger origin because equal mergers of two disc galaxies produce remnants that are outliers of the TFR.
Aims. We explore whether a scenario that combines an origin by mergers at z∼1.8-1.5 with a subsequent passive evolution of the resulting S0 remnants since z∼0.8-1 is compatible with observational data of S0s in the TFR both at z∼0.8 and z∼0.
Methods. We studied a set of major and minor merger experiments from the GalMer database that generate massive S0 remnants that are dynamically relaxed and have realistic properties. We analysed the location of these remnants in the photometric and stellar TFRs assuming that they correspond to z∼0.8 galaxies. We then estimated their evolution in these planes over the last ∼7Gyr considering that they have evolved passively in isolation. The results were compared with data of real S0s and spirals at different redshifts. We also tested how the use of Vcirc or Vrot,max affects the results.
Results. Just after ∼1-2 Gyr of coalescence, major mergers generate S0 remnants that are outliers of the local photometric and stellar TFRs (as already stated in previous studies), in good agreement with observations at z ∼ 0.8. After ∼4-7 Gyr of passive evolution in isolation, the S0 remnants move towards the local TFR, although the initial scatter among them persists. This scatter is sensitive to the indicator used for the rotation velocity: Vcirc values yield a lower scatter than when Vrot,max values are considered instead. In the planes involving Vrot,max, a clear segregation of the S0 remnants in terms of the spin-orbit coupling of the model is observed, in which the remnants of retrograde encounters overlap with local S0s hosting counter-rotating discs. The location of the S0 remnants at z∼0 agrees well with the observed distribution of local S0 galaxies in the σ0-MK, Vcirc0, and Vrot,max0 planes.
Conclusions. Massive S0 galaxies may have been formed through major mergers that occurred at high redshift and have later evolved towards the local TFR through passive evolution in relative isolation, a mechanism that would also contribute to the scatter observed in this relation.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: formation - galaxies: evolution - galaxies: elliptical and lenticular, cD - galaxies: interactions - galaxies: structure - galaxies: kinematics and dynamics - galaxies: kinematics and dynamics

Simbad objects: 19

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Number of rows : 19
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 NGC 1023 IG 02 40 24.0133575864 +39 03 47.663392896 10.91 10.35 9.35 7.83   ~ 641 2
2 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1729 0
3 NGC 2551 GiG 08 24 50.2699218936 +73 24 43.353747900   13.10 12.11     ~ 76 1
4 NGC 2768 SyG 09 11 37.504 +60 02 13.95 11.30 10.84 9.87     ~ 488 2
5 NGC 3115 GiG 10 05 13.9270507008 -07 43 06.982712292   11   9.37   ~ 982 2
6 NGC 3384 GiG 10 48 16.8855574392 +12 37 45.371165844   10.0       ~ 579 1
7 NGC 3489 GiG 11 00 18.5483994744 +13 54 04.206202668 11.46 11.12 10.29     ~ 385 1
8 NGC 3593 GiG 11 14 36.9731893800 +12 49 05.497790664   11.8       ~ 343 2
9 IC 719 G 11 40 18.4960446000 +09 00 35.742181788   13.6       ~ 117 0
10 NGC 3941 Sy2 11 52 55.3609498656 +36 59 10.716212904   11.45 11.62 9.97   ~ 237 0
11 NGC 4138 Sy1 12 09 29.8011417048 +43 41 06.864140004 12.46 12.29 11.32 10.82   ~ 390 1
12 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6383 0
13 NGC 4546 GiG 12 35 29.4931619736 -03 47 35.383858656 11.89 11.30 10.32     ~ 214 1
14 NGC 4550 GiP 12 35 30.5913588048 +12 13 14.921166792 12.97 12.56 11.68     ~ 527 1
15 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4604 2
16 NGC 5631 Sy2 14 26 33.2913328320 +56 34 57.424681848   13.51 12.55     ~ 172 0
17 NGC 6340 GiP 17 10 24.8346254376 +72 18 15.919996608   11.87 11.01     ~ 182 1
18 NGC 7332 GiP 22 37 24.5373044952 +23 47 53.830708800   12.0       ~ 365 0
19 NGC 7457 G 23 00 59.9263288440 +30 08 41.764398792   11.04 11.87     ~ 425 0

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2023.02.04-00:43:48

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