J/ApJ/862/100 Carnegie-Irvine Galaxy Survey VII. S0 galaxies (Gao+, 2018)
The Carnegie-Irvine Galaxy Survey.
VII. Constraints on the origin of S0 galaxies from their photometric structure.
Gao H., Ho L.C., Barth A.J., Li Z.-Y.
<Astrophys. J., 862, 100 (2018)>
=2018ApJ...862..100G 2018ApJ...862..100G
ADC_Keywords: Galaxies, photometry; Morphology; Surveys; Velocity dispersion
Keywords: galaxies: bulges ; galaxies: elliptical and lenticular, cD ;
galaxies: evolution ; galaxies: photometry ; galaxies: structure
Abstract:
Using high-quality optical images from the Carnegie-Irvine Galaxy
Survey, we perform multicomponent decompositions of S0 galaxies (S0s)
to derive accurate structural parameters to constrain their physical
origin. Many S0s do not host prominent bulges. S0s have a broad
distribution of bulge-to-total ratios (B/T) and Sersic indices (n),
with average values of B/T=0.34±0.15 and n=2.62±1.02,
qualitatively consistent with the notion that S0s define a parallel
sequence with and may have evolved from spiral galaxies. This is
further reinforced by the incidence of bars and lenses in S0s, which,
when compared with the statistics in spirals, supports the idea that
lenses are demised bars. However, despite their wide range of
prominence, the bulges of S0s form a surprisingly uniform sequence on
both the Kormendy and fundamental plane relations. There is no
evidence for population dichotomy or other indications of
differentiation into classical and pseudo bulges. Most of the S0s
reside in the field and in groups; cluster environment is not a
necessary condition for S0 production. The properties of S0 bulges
show little correlation with environmental indicators, after the
dependence of galaxy stellar mass on environment is taken into
account. As the bulges of late-type spirals and S0s are intrinsically
different, and environmental effects that may account for such
evolution appear to be minimal, we conclude that late- type spirals
are not plausible progenitors of S0s. The bulges of S0s likely formed
at an early epoch, after which secular processes contributed little to
their subsequent evolution.
Description:
The Carnegie-Irvine Galaxy Survey (CGS; Ho+ 2011, J/ApJS/197/21)
sample is defined by BT≤12.9mag and δ<0°, without any
reference to morphology, size, or environment.
All the images for CGS were taken with the du Pont 2.5m telescope,
during the period 2003 February to 2006 June.
Here we focus only on the R-band data.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 99 62 Bulge parameters and bar/lens identifications of
the Carnegie-Irvine Galaxy Survey (CGS) S0 galaxies
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See also:
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
J/ApJ/542/673 : Morphological types of galaxies in clusters (Fasano+, 2000)
J/AJ/136/773 : Structure of classical bulges & pseudobulges (Fisher+, 2008)
J/MNRAS/393/1531 : BUDDA structural properties of galaxies (Gadotti+, 2009)
J/ApJ/716/942 : Bulges of nearby galaxies with Spitzer (Fisher+, 2010)
J/MNRAS/405/1089 : Photometric scaling for L/S0 galaxies (Laurikainen+ 2010)
J/MNRAS/416/1680 : ATLAS3D project. VII. (Cappellari+, 2011)
J/ApJS/197/21 : The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)
J/ApJS/197/22 : The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)
J/MNRAS/432/3141 : Morphological classification of PM2GC gal. (Calvi+, 2013)
J/ApJ/845/87 : CGS. V. Statistical study of bars & buckled bars (Li+, 2017)
J/ApJ/862/13 : The Carnegie-Irvine Galaxy Survey. VI. Spirals (Yu+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Galaxy name
14- 18 F5.2 mag Rmag [9.8/13.7] Total R-band magnitude
20- 23 F4.2 mag e_Rmag [0.05/0.5] Uncertainty in Rmag
25- 29 F5.3 --- B/T [0.06/0.8] Bulge-to-total ratio
31- 35 F5.3 --- e_B/T [0.002/0.2] Uncertainty in B/T
37- 41 F5.2 mag/arcsec2 mu-Reff [14.6/21.4] Surface brightness
at the effective radius
43- 46 F4.2 mag/arcsec2 e_mu-Reff [0.03/0.9] Uncertainty in mu-Reff
48- 51 F4.2 --- n [0.3/5] Sersic index
53- 56 F4.2 --- e_n [0.03/1.5] Uncertainty in n
58- 62 F5.2 arcsec Reff [0.5/30.1] Effective radius
64- 68 F5.2 arcsec e_Reff [0.04/16] Uncertainty in Reff
70- 74 F5.3 --- ell [0.01/0.6] Ellipticity
76- 80 F5.3 --- e_ell [0.001/0.05] Uncertainty in ell
82- 86 F5.2 kpc/arcmin Scale [2.4/21.9] Scale to convert
from arcmin to kpc
88- 92 F5.1 km/s sigma0 [74.5/308]? Central stellar
velocity dispersion
94- 97 F4.1 km/s e_sigma0 [1.9/19.4]? Uncertainty in sigma0
99 A1 --- Flag Bar/Lens Flag (1)
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Note (1): Flag for the presence or absence of a bar/lens as follows:
B = definitely barred;
W = weakly barred;
N = no bar or lens;
L = no bar but lens present;
? = uncertain.
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History:
From electronic version of the journal
References:
Ho et al. Paper I. 2011ApJS..197...21H 2011ApJS..197...21H Cat. J/ApJS/197/21
Li et al. Paper II. 2011ApJS..197...22L 2011ApJS..197...22L Cat. J/ApJS/197/22
Huang et al. Paper III. 2013ApJ...766...47H 2013ApJ...766...47H
Huang et al. Paper IV. 2016ApJ...821..114H 2016ApJ...821..114H Cat. J/ApJ/821/114
Li et al. Paper V. 2017ApJ...845...87L 2017ApJ...845...87L Cat. J/ApJ/845/87
Yu et al. Paper VI. 2018ApJ...862...13Y 2018ApJ...862...13Y Cat. J/ApJ/862/13
Gao et al. Paper VII. 2018ApJ...862..100G 2018ApJ...862..100G This catalog.
Gao et al. Paper VIII. 2019ApJS..244...34G 2019ApJS..244...34G Cat. J/ApJS/244/34
Gao et al. Paper IX. 2020ApJS..247...20G 2020ApJS..247...20G Cat. J/ApJS/247/20
Gao et al. Paper X. 2022ApJS..262...54G 2022ApJS..262...54G Cat. J/ApJS/262/54
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 30-Jul-2019