J/A+A/562/A121 ARRAKIS: Atlas of Resonance Rings as Known In S4G (Comeron+ 2014)
ARRAKIS: Atlas of Resonance (pseudo)Rings as Known In the S4G.
Comeron S., Salo H., Laurikainen E., Knapen J.H., Buta R.J.,
Herrera-Endoqui M., Laine J., Holwerda B.W., Sheth K., Regan M.W.,
Hinz J.L., Munoz-Mateo J.C., Gil de Paz A., Menedez-Delmestre K.,
Seibert M., Mizusawa T., Kim T., Erroz-Ferrer S., Gadotti D.A.,
Athanassoula E., Bosma A., Ho L.C.
<Astron. Astrophys. 562, A121 (2014)>
=2014A&A...562A.121C 2014A&A...562A.121C
ADC_Keywords: Atlases ; Galaxy catalogs ; Galaxies, nearby ; Galaxies, ring ;
Galaxies, IR
Keywords: atlases - catalogues - galaxies: statistics - galaxies: structure
Abstract:
Resonance rings and pseudorings (here collectively called "rings")
are thought to be related to the gathering of material near dynamical
resonances caused by non-axisymmetries in galaxy discs. Therefore,
they are the consequence of secular evolution processes that
redistribute material and angular momentum in discs. Their study may
give clues on the formation and growth of bars and other disc
non-axisymmetries.
Our aims are to produce a Catalogue and an Atlas of the rings detected
in the Spitzer Survey of Stellar Structure in Galaxies (S4G) and to
conduct a statistical study of the data in the Catalogue.
We traced the contours of rings previously identified by Buta et al.
(in preparation) and fitted them with ellipses. We found the
orientation of bars by studying the galaxy ellipse fits from S4G's
Pipeline4. We used the galaxy orientation data obtained by S4G's
Pipeline 4 to obtain intrinsic ellipticities and orientations of rings
and the bars.
ARRAKIS contains data on 724 ringed galaxies in the S4G. The frequency
of resonance rings in the S4G is of 16±1% and 35±1% for outer and
inner features, respectively. Outer rings are mostly found in Hubble
stages -1≤T≤4. Inner rings are found in a broad distribution that
covers the range -1≤T≤7. We confirm that outer rings have two
preferred orientations, namely parallel and perpendicular to the bar.
We confirm a tendency for inner rings to be oriented parallel to the
bar, but we report the existence of a significant fraction (maybe as
large as 50%) of inner features that have random orientations with
respect to the bar. These misaligned inner rings are mostly found in
late-type galaxies (T≥4). We find that the fraction of barred
galaxies hosting outer (inner) rings is ∼1.7 times (∼1.3 times) that
in unbarred galaxies.
We confirm several results from previous surveys, as well as
predictions from simulations of resonant rings and/or from manifold
flux tube theory. We report that a significant fraction of inner rings
in late-type galaxies have a random orientation with respect to the
bar. This may be due to spiral modes decoupled from the bar dominating
the Fourier amplitude spectrum at the radius of the inner ring. The
fact that rings are only mildly favoured by bars suggests that those
in unbarred galaxies either formed due to weak departures from the
axisymmetry of the galactic potential or that they are born because of
bars that have been destroyed after the ring formation.
Description:
Appendix B. Catalogue of the rings in ARRAKIS.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 58 1324 Catalogue with the properties of rings and bars
in S4G ringed galaxies
tablea2.dat 58 19 Catalogue with the properties of rings and bars
in ringed galaxies appearing in S4G frames but
not included in the original S4G sample
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See also:
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Galaxies (Sheth+ 2010)
J/ApJS/190/147 : Mid-IR galaxy morphology from S4G (Buta+, 2010)
Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Galaxy name
11- 15 F5.1 Mpc Dist ?=- Distance to the galaxy
17- 20 A4 --- Kind Kind of feature (1)
22- 26 F5.2 arcmin Dmaj Feature major diameter
29- 32 F4.2 arcmin Dmin Feature minor diameter
35- 39 F5.1 deg PA [0/180] Major axis PA of the feature
41- 45 F5.2 arcmin Dmaj0 ?=- Feature deprojected major diameter
47- 51 F5.2 arcmin Dmin0 ?=- Feature deprojected minor diameter
54- 58 F5.1 deg nodes [0/180]?=- Deprojected major axis angle
difference θr with respect to the
line of nodes of the deprojection
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Note (1): Kind of features (see section 3.1 for details):
nr = nuclear ring
nr' = nuclear pseudoring
nr'l = nuclear pseudoring/lens
nrl = nuclear ring/lens
r = inner ring
rs = inner pseudoring
rs_ = inner pseudoring, closest to pure spiral
_rs = inner pseudoring, closest to inner ring
R = outer ring
R' = outer pseudoring
R1 = Type 1 Outer Lindblad Resnonace (OLR) subclass outer ring
R1' = Type 1 OLR subclass outer pseudoring
R2' = Type 2 OLR subclass outer pseudoring
nl = nuclear lens
l = inner lens
rl = inner ring/lens
rl_ = inner ring/lens, closest to lens
_rl = inner ring/lens, closest to inner ring
r'l = inner pseudoring/lens
L = outer lens
RL = outer ring/lens
PRG = polar ring galaxy
R'L = outer pseudoring/outer lens
R2'L = Type 2 OLR subclass outer pseudoring/outer lens
RG = ring galaxy (collisional ring)
RL = outer ring/outer lens
RL_ = outer ring/outer lens, closest to outer lens
bar = bar
x1r = x1-ring (ring formed at the largest non-looping orbit whose major
axis is parallel to the bar major axis)
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Acknowledgements:
Sebastien Comeron, seb.comeron(at)gmail.com
History:
* 03-Dec-2013: Original version from Sebastien Comeron
(but table A2 had wrong identifiers)
* 21-Jul-2014: New version of both tables (fixed and standardized names
in both tables, no zero between the acronym and number)
(End) S. Comeron [Univ. of Oulu, Finland], P. Vannier [CDS] 03-Dec-2013