J/ApJ/845/87 CGS. V. Statistical study of bars and buckled bars (Li+, 2017)
The Carnegie-Irvine Galaxy Survey.
V. Statistical study of bars and buckled bars.
Li Z.-Y., Ho L.C., Barth A.J.
<Astrophys. J., 845, 87 (2017)>
=2017ApJ...845...87L 2017ApJ...845...87L
ADC_Keywords: Galaxies, optical ; Morphology ; Colors
Keywords: galaxies: bulges; galaxies: spiral; galaxies: structure
Abstract:
Simulations have shown that bars are subject to a vertical buckling
instability that transforms thin bars into boxy or peanut-shaped
structures, but the physical conditions necessary for buckling to
occur are not fully understood. We use the large sample of local disk
galaxies in the Carnegie-Irvine Galaxy Survey to examine the incidence
of bars and buckled bars across the Hubble sequence. Depending on the
disk inclination angle (i), a buckled bar reveals itself as either a
boxy/peanut-shaped bulge (at high i) or as a barlens structure (at
low i). We visually identify bars, boxy/peanut-shaped bulges, and
barlenses, and examine the dependence of bar and buckled bar fractions
on host galaxy properties, including Hubble type, stellar mass, color,
and gas mass fraction. We find that the barred and unbarred disks show
similar distributions in these physical parameters. The bar fraction
is higher (70%-80%) in late-type disks with low stellar mass
(M*<1010.5M☉) and high gas mass ratio. In contrast, the
buckled bar fraction increases to 80% toward massive and early-type
disks (M*>1010.5M☉), and decreases with higher gas mass ratio.
These results suggest that bars are more difficult to grow in massive
disks that are dynamically hotter than low-mass disks. However, once a
bar forms, it can easily buckle in the massive disks, where a deeper
potential can sustain the vertical resonant orbits. We also find a
probable buckling bar candidate (ESO506-G004) that could provide
further clues to understand the timescale of the buckling process.
Description:
Images in B-, V-, R-, and I-band filters were taken with the du Pont
2.5m telescope at Las Campanas Observatory, with a field of view (FOV)
of 8.9'x8.9'. The typical depths of the B-, V-, R-, and I-band images
are 27.5, 26.9, 26.4, and 25.3mag/arcsec2, respectively.
More information about the Carnegie-Irvine Galaxy Survey (CGS) design,
data reduction, and photometric measurements can be found in Papers I
(Ho+, 2011, J/ApJS/197/21) and II (Li+, 2011, J/ApJS/197/22).
In this work, we use the CGS I-band images to minimize the effect of
dust extinction. The selected sample contains 376 disk galaxies with
264 disks hosting bars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 49 376 Carnegie-Irvine Galaxy Survey (CGS) disk galaxy
properties and bar classification
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See also:
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/ApJ/424/599 : Abundances in barred spiral galaxies (Martin+ 1994)
J/ApJS/143/73 : Morphology of spiral galaxies (Eskridge+, 2002)
J/ApJ/659/1176 : Study of bars in 180 spiral galaxies (Marinova+, 2007)
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Gal. (Sheth+, 2010)
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/ApJ/771/59 : S4G face-on galaxy surface brightness (Munoz-Mateos+, 2013)
J/ApJ/821/114 : The CGS. IV. Elliptical galaxies colors (Huang+, 2016)
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 Identifier
14- 17 A4 --- Morph Morphological type
19- 23 F5.2 deg inc [0/70] Inclination measured in I band
25- 29 F5.2 [Msun] logM* [8/12]? Log stellar mass
31- 34 F4.2 mag V-I [0/10] The (V-I) color index (1)
36- 39 F4.2 --- Ratio [0/1.1]? The H I mass to stellar mass ratio
41- 49 A9 --- Bar Bar type (2)
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Note (1): Extinction corrected color of the whole galaxy.
Note (2): Bar type as follows:
B/PS = boxy/peanut-shaped (B/PS) bulge (37 occurrences)
barlens = lens-like morphology embedded in the bar (64 occurrences)
unbuckled = Unbuckled bar (163 occurrences)
unbarred = Unbarred disk (112 occurrences)
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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 This catalog
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 Cat. J/ApJ/862/100
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] 03-Apr-2018