J/MNRAS/467/2127 4 samples of disc galaxies (Pranger+, 2017)
The effect of environment on the structure of disc galaxies.
Pranger F., Trujillo I., Kelvin L.S., Cebrian M.
<Mon. Not. R. Astron. Soc., 467, 2127-2144 (2017)>
=2017MNRAS.467.2127P 2017MNRAS.467.2127P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, SDSS ; Morphology
Keywords: galaxies: evolution - galaxies: photometry - galaxies: structure
Abstract:
We study the influence of environment on the structure of disc
galaxies, using IMFIT to measure the g- and r-band structural
parameters of the surface-brightness profiles for ∼700
low-redshift (z<0.063) cluster and field disc galaxies with
intermediate stellar mass (0.8x1010M☉<M*<4x1010M☉)
from the Sloan Digital Sky Survey, DR7. Based on this measurement, we
assign each galaxy to a surface-brightness profile type
(Type I = single-exponential, Type II = truncated,
Type III = antitruncated). In addition, we measure (g-r) rest frame
colour for disc regions separated by the break radius. Cluster disc
galaxies (at the same stellar mass) have redder (g-r) colour by ∼0.2
mag than field galaxies. This reddening is slightly more pronounced
outside the break radius. Cluster disc galaxies also show larger
global Sersic-indices and are more compact than field discs, both by
∼15 per cent. This change is connected to a flattening of the (outer)
surface-brightness profile of Type I and - more significantly - of
Type III galaxies by ∼8 per cent and ∼16 per cent, respectively, in
the cluster environment compared to the field. We find fractions of
Type I, Type II and Type III of (6±2) per cent, (66±4) per cent
and (29±4) per cent in the field and (15-4+7) per cent, (56±7)
per cent and (29±7) per cent in the cluster environment,
respectively. We suggest that the larger abundance of Type I galaxies
in clusters (matched by a corresponding decrease in the Type II
fraction) could be the signature of a transition between Type II and
Type I galaxies produced/enhanced by environment-driven mechanisms.
Description:
We have selected four samples of disc galaxies within the same narrow
stellar mass range (0.8<M*<4)x1010M☉. While one of these
samples consists of galaxies residing in galaxy clusters, the other
three consist of galaxies outside of galaxy clusters, i.e. from the
field. Each of the four samples holds around 175 galaxies that have
been classified according to their disc structure
(Type I = single-exponential, Type II = truncated,
Type III = antitruncated).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 82 175 Total cluster sample
tablec2.dat 82 172 Field sample 1
tablec3.dat 82 172 Field sample 2
tablec4.dat 82 177 Field sample 3
tablec5.dat 50 175 Total cluster sample, scalelengths and break radii
tablec6.dat 50 172 Field sample 1, scalelengths and break radii
tablec7.dat 50 172 Field sample 2, scalelengths and break radii
tablec8.dat 50 177 Field sample 3, scalelengths and break radii
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Byte-by-byte Description of file: tablec[1234].dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Index Index
5- 11 F7.3 deg RAdeg Right ascension (J2000)
13- 19 F7.4 deg DEdeg Declination (J2000)
21- 23 A3 --- Type Type (1)
25- 30 F6.4 --- z Redshift
32- 36 F5.3 kpc Re Errective radius
38- 42 F5.3 --- n Sersic index
44- 50 F7.4 mag (g-r)in Inner median g-r colour index
52- 58 F7.4 mag (g-r)in1 Inner median g-r colour index determined
between <Rb> and Rc1 (2)
60- 66 F7.4 mag (g-r)in2 Inner median g-r colour index determined
between <Rb> and Rc2 (2)
68- 74 F7.4 mag (g-r)out ?=- Outer median g-r colour index
76- 82 I7 --- ID Identification number
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Note (1): Types as follows:
Type I = single-exponential
Type II = truncated
Type III = antitruncated
Note (2): where <Rb> is the mean break radius (<Rb≥(Bbg+Rbs)/2,
RC1 the inner radius, RC1=0.5Re, and RC2 the outer radius, RC2=0.75Re.
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Byte-by-byte Description of file: tablec[5678].dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Index Index
5- 10 F6.4 kpc h1g Inner scalelength of disc galaxy from g band
12- 18 F7.4 kpc h2g ?=- Outer scalelength of disc galaxy from g band
20- 26 F7.4 kpc Rbg ?=- Break radius from g band
28- 34 F7.4 kpc h1r Inner scalelength of disc galaxy from h band
36- 42 F7.4 kpc h2r ?=- Outer scalelength of disc galaxy from h band
44- 50 F7.4 kpc Rbr ?=- Break radius from h band
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Nov-2019