J/A+A/672/A27 Galaxies outside clusters (Bilek+, 2023)
Origin of the differences in rotational support among early-type galaxies:
The case of galaxies outside clusters.
Bilek M., Duc P.-A., Sola E.
<Astron. Astrophys. 672, A27 (2023)>
=2023A&A...672A..27B 2023A&A...672A..27B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs; Abundances ; Morphology
Keywords: galaxies: elliptical and lenticular, cD -
galaxies: kinematics and dynamics - galaxies: interactions -
galaxies: evolution - methods: statistical - methods: observational
Abstract:
Early-type galaxies (ETGs) are divided into slow and fast rotators
(FRs and SRs) according to the degree of ordered rotation of their
stellar populations. Cosmological hydrodynamical simulations indicate
that galaxies form as FRs before their rotational support decreases,
usually because of mergers.
We aimed to investigate this process observationally for galaxies
outside of clusters.
We made use of the fact that different merger types leave different
traces that have different lifetimes. We statistic ally analyzed
multiple characteristics of galaxies that are expected to be
influenced by mergers, such as tidal features, kinematically distinct
cores, and stellar ages. They were taken from the MATLAS and ATLAS3D
databases. Through multilinear regression we identified the quantities
that, at a fixed mass and environmental density of the galaxy,
significantly correlate with a measure of the ordered rotation of the
galaxy, lambdaNRe.
We found a negative correlation of the rotational support with the
occurrence of tidal disturbances and kinematic substructures, and a
positive correlation with metallicity and metallicity gradients. For
massive galaxies, the rotational support correlates negatively with
the abundance of alpha elements, and for the galaxies in low-density
environments, it correlates negatively with the central photometric
cuspiness. These and additional literature observational constraints
are explained the easiest if the mergers that decreased the rotational
support of ETGs were typically minor, wet, and happening at z∼2. They
did not form the currently observed tid al features. The observed
frequency of tidal features implies a merging rate of 0.07-0.2 per
Gyr. This is insufficient to explain the observed growth of the radii
of ETGs with redshift by mergers.
Description:
The complete dataset analyzed in the paper.
Note: compared to the whole MATLAS sample, galaxies PGC058114 and
PGC071531 were excluded.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table.dat 725 175 Complete dataset analyzed in the paper
--------------------------------------------------------------------------------
See also:
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/416/1680 : ATLAS3D project. VII. (Cappellari+, 2011)
J/MNRAS/448/3484 : ATLAS3D project. XXX (McDermid+, 2015)
J/A+A/635/A129 : ATLAS3D sample metallicity and age gradients
(Krajnovic+, 2020)
Byte-by-byte Description of file: table.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Galaxy name (1)
11- 28 F18.15 [Msun] logMJAM log10 of JAM mass (derived from data in
Cappellari et al., 2013MNRAS.432.1709C 2013MNRAS.432.1709C)
30- 34 F5.2 [Mpc-3] logrho10 log10 of rho10 environmental density
(source Cappellari et al.,
2011MNRAS.416.1680C 2011MNRAS.416.1680C)
36- 40 F5.3 --- lam Specific angular momentum parameter
lambdaRe (source
Emsellem et al., 2011MNRAS.416.1680C 2011MNRAS.416.1680C)
42- 46 F5.3 --- eps epsilone ellipticity (source
Emsellem et al., 2011MNRAS.416.1680C 2011MNRAS.416.1680C)
48- 50 F3.1 --- sh [0/2] Shell presence rating (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B) (2)
52- 54 F3.1 --- st [0/2] Stream presence rating (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B) (2)
56- 58 F3.1 --- tail [0/2] Tail presence rating (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B) (2)
60- 62 F3.1 --- DI [0/2]?=- Rating of presence of disturbed
isophotes (source Bilek et al.,
2020MNRAS.498.2138B 2020MNRAS.498.2138B) (2)
64- 66 F3.1 --- anyTF [0/2] Rating of presence of any tidal
features (2)
68- 70 F3.1 --- anyTForDI [0/2]?=- Rating of presence of any tidal
features or disturbed isophotes (2)
72- 90 F19.17 --- shfr Frequency of shells (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B)
92-109 F18.16 --- stfr Frequency of streams (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B)
111-129 F19.17 --- tailfr Frequency of tails (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B)
131-133 F3.1 --- dust [0/2] Dust presence rating (source
Bilek et al., 2020MNRAS.498.2138B 2020MNRAS.498.2138B) (2)
135-137 F3.1 --- KDC [0/1] Presence of a kinematically
distinct core (source Krajnovic et al.,
2011MNRAS.414.2923K 2011MNRAS.414.2923K)
139-141 F3.1 --- CRC [0/1] Presence of a counter-rotating core
(source Krajnovic et al.,
2011MNRAS.414.2923K 2011MNRAS.414.2923K)
143-145 F3.1 --- KT [0/1] presence of a kinematic twist
(source Krajnovic et al.,
2011MNRAS.414.2923K 2011MNRAS.414.2923K)
147-149 F3.1 --- 2sig [0/1] presence of a two-sigma feature
(source Krajnovic et al.,
2011MNRAS.414.2923K 2011MNRAS.414.2923K)
151-153 F3.1 --- noKinf [0/1] no kinematic substructure is
present
155-175 F21.18 [kpc] logRemaj log10 of Remaj radius (derived from
data in Cappellari et al.,
2013MNRAS.432.1709C 2013MNRAS.432.1709C and distances in
Cappellari et al., 2011MNRAS.413..813C 2011MNRAS.413..813C)
177-181 F5.2 --- gam ?=- gamma' slope of the central
photometric profile (source
Krajnovic et al., 2020A&A...635A.129K 2020A&A...635A.129K)
183-187 F5.2 Gyr age ?=- SSP stellar age (source
McDermid et al., 2015MNRAS.448.3484M 2015MNRAS.448.3484M)
189-194 F6.3 --- agegr gradient of SSP stellar age (source
Krajnovic et al., 2020A&A...635A.129K 2020A&A...635A.129K)
196-200 F5.2 --- Z ?=- SSP stellar metallicity (source
McDermid et al., 2015MNRAS.448.3484M 2015MNRAS.448.3484M)
202-207 F6.3 --- Zgr Gradient of SSP stellar metallicity
(source Krajnovic et al.,
2020A&A...635A.129K 2020A&A...635A.129K)
209-213 F5.2 --- alpha ?=- SSP stellar alpha element abundance
(source McDermid et al.,
2015MNRAS.448.3484M 2015MNRAS.448.3484M)
215-220 F6.3 --- alphagr Gradient of SSP stellar alpha element
abundance (source Krajnovic et al.,
2020A&A...635A.129K 2020A&A...635A.129K)
222-241 F20.17 --- c-sh [-1/2] Cleaned sh
243-262 F20.17 --- c-st [-1/2] Cleaned st
264-283 F20.17 --- c-tail [-1/2] Cleaned tail
285-305 F21.18 --- c-DI [-2/2]?=- Cleaned DI
307-326 F20.17 --- c-anyTF [-1/2] Cleaned anyTF
328-347 F20.17 --- c-anyTForDI [-1/2]?=- Cleaned anyTForDI
349-368 F20.17 --- c-shfr Cleaned shfr
370-390 F21.18 --- c-stfr Cleaned stfr
392-412 F21.18 --- c-tailfr Cleaned tailfr
414-433 F20.17 --- c-dust [-1/2] Cleaned dust
435-454 F20.17 --- c-KDC [-1/1] Cleaned KDC
456-475 F20.17 --- c-CRC [-1/1] Cleaned CRC
477-498 F22.19 --- c-KT [-1/1] Cleaned KT
500-520 F21.18 --- c-2sig [-1/1] Cleaned 2sig
522-541 F20.17 --- c-noKinf [-1/1] Cleaned noKinf
543-564 F22.19 --- c-logRemaj Cleaned logRe_maj
566-587 F22.18 --- c-gam ?=- Cleaned gam
589-609 F21.18 --- c-age ?=- Cleaned age
611-632 F22.19 --- c-agegr Cleaned agegr
634-655 F22.19 --- c-Z ?=- Cleaned Z
657-678 F22.19 --- c-Zgr Cleaned Zgr
680-701 F22.19 --- c-alpha ?=- Cleaned alpha
703-725 F23.20 --- c-alphagr Cleaned alphagr
--------------------------------------------------------------------------------
Note (1): following Cappellari et al., 2011MNRAS.413..813C 2011MNRAS.413..813C, Cat. J/MNRAS/413/813
(note: MATLAS galaxies PGC058114 and PGC071531 were excluded).
Note (2): Presence of the features as follows:
0.0 = no
0.5 = between not present and likely
1.0 = likely
1.5 = between likely and present
2.0 = yes
--------------------------------------------------------------------------------
Acknowledgements:
Michal Bilek, michal.bilek(at)obspm.fr
(End) Patricia Vannier [CDS] 20-Jan-2023