J/A+A/647/A100 Fornax Deep Survey with VST. XI. (Su+, 2021)
The Fornax Deep Survey (FDS) with the VST. XI. The search for signs of
preprocessing between the Fornax main cluster and Fornax A group.
Su A.H., Salo H., Janz J., Laurikainen E., Venhola A., Peletier R.F.,
Iodice E., Hilker M., Cantiello M., Napolitano N., Spavone M., Raj M.A.,
van de Ven G., Mieske S., Paolillo M., Capaccioli M., Valentijn E.A.,
Watkins A.E.
<Astron. Astrophys. 647, A100 (2021)>
=2021A&A...647A.100S 2021A&A...647A.100S (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Photometry ; Morphology
Keywords: galaxies: clusters: individual: Fornax -
galaxies: groups: individual: Fornax A -
galaxies: interactions - Galaxy: evolution - galaxies: structure -
galaxies: photometry
Abstract:
Galaxies either live in a cluster, a group, or in a field environment.
In the hierarchical framework, the group environment bridges the field
to the cluster environment, as field galaxies form groups before
aggregating into clusters. In principle, environmental mechanisms,
such as galaxy-galaxy interactions, can be more efficient in groups
than in clusters due to lower velocity dispersion, which lead to
changes in the properties of galaxies. This change in properties for
group galaxies before entering the cluster environment is known as
preprocessing. Whilst cluster and field galaxies are well studied, the
extent to which galaxies become preprocessed in the group environment
is unclear. We investigate the structural properties of cluster and
group galaxies by studying the Fornax main cluster and the infalling
Fornax A group, exploring the effects of galaxy preprocessing in this
showcase example. Additionally, we compare the structural complexity
of Fornax galaxies to those in the Virgo cluster and in the field. Our
sample consists of 582 galaxies from the Fornax main cluster and
Fornax A group. We quantified the light distributions of each galaxy
based on a combination of aperture photometry, Sersic+PSF (point
spread function) and multi-component decompositions, and
non-parametric measures of morphology. From these analyses, we derived
the galaxy colours, structural parameters, non-parametric
morphological indices (Concentration C; Asymmetry A, Clumpiness S;
Gini G; second order moment of light M20), and structural complexity
based on multi-component decompositions. These quantities were then
compared between the Fornax main cluster and Fornax A group. The
structural complexity of Fornax galaxies were also compared to those
in Virgo and in the field. We find significant (Kolmogorov-Smirnov
test p-value <alpha=0.05) differences in the distributions of
quantities derived from Sersic profiles (g'-r', r'-i', Re, and
{bar}µe,r'), and non-parametric indices (A and S) between the
Fornax main cluster and Fornax A group. Fornax A group galaxies are
typically bluer, smaller, brighter, and more asymmetric and clumpy.
Moreover, we find significant cluster-centric trends with r'-i', Re,
and {bar}µe,r', as well as A, S, G, and M20 for galaxies in the
Fornax main cluster. This implies that galaxies falling towards the
centre of the Fornax main cluster become fainter, more extended, and
generally smoother in their light distribution. Conversely, we do not
find significant group-centric trends for Fornax A group galaxies. We
find the structural complexity of galaxies (in terms of the number of
components required to fit a galaxy) to increase as a function of the
absolute r'-band magnitude (and stellar mass), with the largest change
occurring between -14mag≲Mr'≲-19,mag
(7.5≲log10(M*/M☉)~=9.7). This same trend was found in galaxy
samples from the Virgo cluster and in the field, which suggests that
the formation or maintenance of morphological structures (e.g. bulges,
bar) are largely due to the stellar mass of the galaxies, rather than
the environment they reside in.
Description:
Structural quantities based on photometry of galaxies in the Fornax
main cluster and Fornax A group. This includes Sersic-derived
quantities based on Sersic+PSF decompositions, non-parametric
morphological indices (C, A, S, G, M20, Delta(g-r)), and
multi-component decomposition models.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablei1.dat 88 582 Summary table of FDS sample properties
table2.dat 80 582 Table of parameters from Sersic+PSF decompositions
table3.dat 57 582 Table of non-parametric indices
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See also:
J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)
J/A+A/608/A142 : Fornax Deep Survey with VST. III. (Venhola+, 2017)
J/A+A/620/A165 : Fornax Deep Survey with VST. IV. (Venhola+, 2018)
J/A+A/623/A1 : Fornax Deep Survey with VST. V. (Iodice+, 2019)
J/A+A/639/A136 : Fornax Deep Survey with VST. IX. (Cantiello+, 2020)
https://www.oulu.fi/astronomy/FDS_DECOMP/main/index.html :
external link to decompositions showcase
Byte-by-byte Description of file: tablei1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- FDS FDS identification number, FDSNN_NNNNa
19- 24 A6 --- FCC FCC identification number, FCCNNN,
if available
26- 35 A10 --- OName Other known catalog name from HyperLeda
37- 43 F7.4 deg RAdeg Right ascension (J2000)
45- 52 F8.4 deg DEdeg Declination (J2000)
54- 57 F4.1 [Msun] logMstar log10 of stellar mass in solar mass units
59- 66 A8 --- MCmodel Model components from multi-component
decompositions (1)
68- 72 F5.2 --- B/T ? Bulge-to-total ratio
74- 78 F5.2 --- Bar/T ? Bar-to-total ratio
80- 84 F5.1 arcsec Reff Effective radius from the outermost
multi-component disk component
86- 88 A3 --- S4Goverlap [Yes No] If galaxy is also in S4G
(Salo et al., 2015, Cat. J/ApJS/219/4)
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Note (1): Components from multi-comp models include: nucleus (N), bulge (B),
disk (D), bar (bar), and barlens (bl).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- FDS FDS identification number, FDSNN_NNNNb
19- 24 F6.2 mag rmagS Sersic r-band total magnitude
26- 29 F4.2 mag g-rS Sersic g-r colour
31- 35 F5.2 mag r-iS Sersic r-i colour
37- 41 F5.1 arcsec reff Sersic effective radius
43- 47 F5.3 --- n Sersic index
49- 53 F5.3 --- b/a Sersic axial ratio (=b/a)
55- 59 F5.1 deg PA [] Sersic position angle
61- 66 F6.2 mag rmagP PSF r-band total magnitude
68- 73 F6.2 mag g-rP PSF g-r colour index
75- 80 F6.2 mag r-iP PSF r-i colour index
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- FDS FDS identification number, FDSNN_NNNNa
19- 23 F5.3 --- C Concentration
25- 30 F6.3 --- A Asymmetry
32- 37 F6.3 --- S Clumpiness
39- 43 F5.3 --- G Gini coefficient
45- 50 F6.3 --- M20 Brightest second order moment of light
52- 57 F6.3 mag Dg-r Outer minus inner g-r colour difference
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Acknowledgements:
Alan Su, hung-shuo.su(at)oulu.fi
References:
Salo et al., 2015ApJS..219....4S 2015ApJS..219....4S, Cat. J/ApJS/219/4
Iodice et al., Paper I 2016ApJ...820...42I 2016ApJ...820...42I
Iodice et al., Paper II 2017ApJ...839...21I 2017ApJ...839...21I
Venhola et al., Paper III 2017A&A...608A.142V 2017A&A...608A.142V, Cat. J/A+A/608/A142
Venhola et al., Paper IV 2018A&A...620A.165V 2018A&A...620A.165V, Cat. J/A+A/620/A165
Iodice et al., Paper V 2019A&A...623A...1I 2019A&A...623A...1I, Cat. J/A+A/623/A1
Venhola et al., Paper VI 2019A&A...625A.143V 2019A&A...625A.143V
Raj et al., Paper VII 2019A&A...628A...4R 2019A&A...628A...4R
Spavone et al., Paper VIII 2019A&A...639A..14S 2019A&A...639A..14S
Cantiello et al., Paper IX 2020A&A...639A.136C 2020A&A...639A.136C, Cat. J/A+A/639/A136
Raj et al., Paper X 2020A&A...640A.137R 2020A&A...640A.137R
(End) Patricia Vannier [CDS] 19-Jan-2021