J/MNRAS/521/2012 Fornax dwarfs galaxies properties from scaling (Watkins+, 2023)
A possible signature of the influence of tidal perturbations in dwarf galaxy
scaling relations.
Watkins A.E., Salo H., Kaviraj S., Collins C.A., Knapen J.H., Venhola A.,
Roman J.
<Mon. Not. R. Astron. Soc. 521, 2012-2029 (2023)>
=2023MNRAS.521.2012W 2023MNRAS.521.2012W (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Clusters, galaxy ; Galaxies, radius ; Positional data ;
Photometry ; Optical ; Stars, masses ; Combined data
Keywords: galaxies: clusters: individual: Fornax Cluster - galaxies: dwarf -
galaxies: evolution - galaxies: interactions - galaxies: structure
Abstract:
Dwarf galaxies are excellent cosmological probes, because their
shallow potential wells make them very sensitive to the key processes
that drive galaxy evolution, including baryonic feedback, tidal
interactions, and ram pressure stripping. However, some of the key
parameters of dwarf galaxies, which help trace the effects of these
processes, are still debated, including the relationship between their
sizes and masses. We re-examine the Fornax Cluster dwarf population
from the point of view of isomass-radius-stellar mass relations
(IRSMRs) using the Fornax Deep Survey Dwarf galaxy Catalogue, with the
centrally located (among dwarfs) 3.63M☉/pc2 isodensity radius
defining our fiducial relation. This relation is a powerful diagnostic
tool for identifying dwarfs with unusual structure, as dwarf galaxies'
remarkable monotonicity in light profile shapes, as a function of
stellar mass, reduces the relation's scatter tremendously. By
examining how different dwarf properties (colour, 10th nearest
neighbour distance, etc.) correlate with distance from our fiducial
relation, we find a significant population of structural outliers with
comparatively lower central mass surface density and larger
half-light-radii, residing in locally denser regions in the cluster,
albeit with similar red colours. We propose that these faint, extended
outliers likely formed through tidal disturbances, which make the
dwarfs more diffuse, but with little mass-loss. Comparing these
outliers with ultra-diffuse galaxies (UDGs), we find that the term UDG
lacks discriminatory power; UDGs in the Fornax Cluster lie both on and
off of IRSMRs defined at small radii, while IRSMR outliers with masses
below ∼107.5M☉ are excluded from the UDG classification due to
their small effective radii.
Description:
Dwarf galaxies are the most abundant kind of galaxy in the Universe
This, combined with their shallow potential wells, makes them
excellent laboratories for galaxy evolution physics. For example, the
efficiency with which mass is transported by galactic superwinds from
supernova, stellar and active galactic nucleus feedback, relative to
each process's energetic output, is much higher in dwarf galaxies than
in their massive counterpartsGalaxy clusters are the most massive
gravitationally bound systems and thus host some of the most vibrant
such assembly histories. The term 'dwarf' therefore refers not to a
single monolithic population, but to a diverse population of
gravitationally bound systems. Such systems follow power-law
correlations, also known as scaling relations, which connect many
fundamental physical properties of galaxies - including dwarfs -
giving insights into the galaxy formation and evolution processes.
Scaling relations can thus help illuminate the processes that shape
dwarf galaxy evolution across the varied and often violent
environments within a galaxy cluster, particularly when contrasted
with scaling relations followed by higher mass galaxies. We compile
and explore these various scaling relations for a sample of nearby
galaxies spanning a wide range of stellar masses and morphologies,
with a large sample of dwarfs taken from the Fornax Deep Survey Dwarf
galaxy Catalogue, as well as a large sample of nearby dwarf and
massive galaxies from the Spitzer Survey of Stellar Structure in
Galaxies.
For this study, we used both imaging data and derived data products
from the FDS, as well as the S4G catalog including both the original
survey and the ETG extension catalog. These survey moslty use 2.6 m
European Southern Observatory VST OmegaCAM to observe Fornax Cluster
and associated subgroup Fornax A in in the g', r', and i' photometric
bands. For our analysis, we used the photometric data products
produced by Su et al. (2021A&A...647A.100S 2021A&A...647A.100S, Cat. J/A+A/647/A100) for a
sample of nearly 600 dwarf and massive galaxies. Further, we derived
isophotal and isomass radii from the surface brightness profiles
produced this catalogue. We use also others catalogs to compare them.
With these two surveys combined, our sample contains surface
photometry and galfit decompositions of 3400 galaxies spanning nearly
six orders of magnitude in stellar mass across a wide range of
environments in the nearby Universe. Next, we follow the relations
described in section 3 and section 4 to conduct our analysis and
obtain four parameters: total stellar mass, isomass radius, Sersic
index, and central mass surface density. The table.dat presents
results from scaling relations for 594 dwarf galaxies.
Objects:
----------------------------------------------------------------------------
RA (2000) DE Designation(s)
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03 38 29.40 -35 27 07.9 ACO S 373 = NAME Fornax Cluster
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File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table.dat 373 594 The isomass radii, galaxy central coordinates
and stellar masses for FDS galaxies sample
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See also:
J/MNRAS/491/1901 : Dwarf galaxies in the MATLAS low-density fields
(Habas+, 2020)
J/MNRAS/416/1680 : ATLAS3D project. VII. (Cappellari+, 2011)
J/MNRAS/384/1544 : Surface photometry of local dwarf galaxies (Sharina+, 2008)
J/MNRAS/357/819 : Colours and HI line observations in Virgo (Sabatini+, 2005)
J/A+A/662/A43 : The Fornax Deep Survey (FDS) with VST. XII. (Venhola+, 2022)
J/A+A/660/A69 : S4G extension for nearby early-type galaxies (Watkins+,2022)
J/A+A/647/A100 : Fornax Deep Survey with VST. XI. (Su+, 2021)
J/A+A/623/A1 : Fornax Deep Survey with VST. V. Isophote fit (Iodice+, 2019)
J/A+A/620/A165 : Fornax Deep Survey with VST. IV. dwarf galaxies
(Venhola+, 2018)
J/A+A/608/A142 : Fornax Deep Survey with VST. III. LSB galaxies
(Venhola+, 2017)
J/A+A/587/A160 : 3.6um S4G Galactic bars characterization (Diaz-Garcia+,2016)
J/A+A/581/A10 : VEGAS: A VST Early-type GAlaxy Survey (Capaccioli+, 2015)
J/ApJ/660/1186 : VCC galaxies classification with SDSS (Lisker+, 2007)
J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)
J/AJ/138/1037 : Star formation in Centaurus A Group dwarfs (Cote+ 2009)
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Galaxies
(Sheth+, 2010)
Byte-by-byte Description of file: table.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Galaxy name in catalogue FDSDC (Name)
19- 36 F18.15 deg RAdeg Galaxy centre right ascension (J2000) (RA)
38- 56 F19.15 deg DEdeg Galaxy centre declination (J2000) (Dec)
58- 66 F9.4 [Msun] logM* ?=-999 The logarithm of stellar mass
(logMstar)
68- 76 F9.4 [Msun] e_logM* ?=-999 The uncertainty on logM* (dlogMstar)
78- 98 F21.16 arcsec R36.31 ?=-999 The axial-ratio-corrected 36.31
Msun/pc2 isomass radius (R36.31)
100- 121 F22.17 arcsec R14.45 ?=-999 The axial-ratio-corrected 14.45
Msun/pc2 isomass radius (R14.45)
123- 144 F22.17 arcsec R5.75 ?=-999 The axial-ratio-corrected 5.75
Msun/pc2 isomass radius (R5.75)
146- 166 F21.16 arcsec R3.63 ?=-999 The axial-ratio-corrected 3.63
Msun/pc2 isomass radius (R3.63)
168- 189 F22.17 arcsec R2.29 ?=-999 The axial-ratio-corrected 2.29
Msun/pc2 isomass radius (R2.29)
191- 211 F21.16 arcsec R1.45 ?=-999 The axial-ratio-corrected 1.45
Msun/pc2 isomass radius (R1.45)
213- 233 F21.16 arcsec R0.92 ?=-999 The axial-ratio-corrected 0.92
Msun/pc2 isomass radius (R0.92)
235- 255 F21.16 arcsec R0.36 ?=-999 The axial-ratio-corrected 0.36
Msun/pc2 isomass radius (R0.36)
257- 277 F21.16 arcsec R0.14 ?=-999 The axial-ratio-corrected 0.14
Msun/pc2 isomass radius (R0.14)
279- 301 F23.18 arcsec e_R3.63 ?=-999 The lower estimate for R3.63 from
sky-subtraction uncertainty (R3.63_l)
303- 325 F23.18 arcsec E_R3.63 ?=-999 The upper estimate for R3.63 from
sky-subtraction uncertainty (R3.63_u)
327- 349 F23.18 arcsec e2_R3.63 ?=-999 The lower estimate for R3.63 from 10%
calibration uncertainty (R3.63_l10)
351- 373 F23.18 arcsec E2_R3.63 ?=-999 The upper estimate for R3.63 from 10%
calibration uncertainty (R3.63_u10)
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History:
From electronic version of the journal
License: CC-BY-4.0
(End) Luc Trabelsi [CDS] 29-May-2026