J/MNRAS/441/1992 Galaxies with disc breaks in S4G and NIRS0S (Laine+, 2014)
Morphology and environment of galaxies with disc breaks in the S4G and NIRS0S.
Laine J., Laurikainen E., Salo H., Comeron S., Buta R.J., Zaritsky D.,
Athanassoula E., Bosma A., Munoz-Mateos J.-C., Gadotti D.A., Hinz J.L.,
Erroz-ferrer S., Gil De Paz A., Kim T., Menendez-Delmestre K., Mizusawa T.,
Regan M.W., Seibert M., Sheth K.
<Mon. Not. R. Astron. Soc., 441, 1992-2012 (2014)>
=2014MNRAS.441.1992L 2014MNRAS.441.1992L
ADC_Keywords: Galaxy catalogs; Morphology
Keywords: galaxies: evolution - galaxies: formation - galaxies: interactions -
galaxies: photometry - galaxies: structure
Abstract:
We study the surface brightness profiles of disc galaxies in the
3.6µm images from the Spitzer Survey of Stellar Structure in
Galaxies (S4G) and Ks-band images from the Near-Infrared S0-Sa galaxy
Survey (NIRS0S). We particularly connect properties of single
exponential (type I), downbending double exponential (type II), and
upbending double exponential (type III) disc profile types, to
structural components of galaxies by using detailed morphological
classifications, and size measurements of rings and lenses. We also
study how the local environment of the galaxies affects the profile
types by calculating parameters describing the environmental density
and the tidal interaction strength. We find that in majority of type
II profiles the break radius is connected with structural components
such as rings, lenses, and spirals. The exponential disc sections of
all three profile types, when considered separately, follow the disc
scaling relations. However, the outer discs of type II, and the inner
discs of type III, are similar in scalelength to the single
exponential discs. Although the different profile types have similar
mean environmental parameters, the scalelengths of the type III
profiles show a positive correlation with the tidal interaction
strength.
Description:
We use the S4G (Sheth et al. 2010PASP..122.1397S 2010PASP..122.1397S, Cat.
J/PASP/122/1397) which consists of more than 2300 galaxies observed at
3.6 and 4.5um wavelengths with the Infrared Array Camera (IRAC).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 86 328 General properties of the sample, and the
environmental parameters
tablea2.dat 123 335 Disc-profile parameters for the studied galaxies
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See also:
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Galaxies (Sheth+ 2010)
J/ApJS/199/26 : The 2MASS Redshift Survey (2MRS) (Huchra+, 2012)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Galaxy name
13- 18 A6 --- Survey The survey from which the galaxy is taken: S4G
(J/PASP/122/1397) or NIRS0S (J/MNRAS/418/1452)
22- 52 A31 --- MType Morphological types (1)
55- 58 F4.1 --- TT [-3/7] Numerical morphology code from the same
sources as for column MType
61- 66 F6.2 mag BMAG ?=- Absolute blue magnitude from HyperLeda
(Paturel et al. 2003A&A...412...45P 2003A&A...412...45P, VII/237)
68- 72 F5.2 Mpc Dist [3/83] Distance calculated from the 2MASS
Redshift Survey recession velocity
(Huchra et al. 2012, Cat. J/ApJS/199/26)
74- 78 F5.2 [-] Q [-7/0] Value of the Dahari parameter (2)
80- 84 F5.2 [Mpc-2] SigA3 [-2/4] Value of the surface density parameter,
ΣA3 = log(3/(πR32)) (3rd
nearest neigh vouring galxy)
86 I1 Mpc r Projected radius at the distance of the galaxy
used for the environmental analysis
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Note (1): from Laurikainen et al. (2011MNRAS.418.1452L 2011MNRAS.418.1452L) for NIRS0S data and
Buta et al. (in preparation) for S4G data.
Note (2): the Dahari parameter (Q; Dahari, 1984AJ.....89..966D 1984AJ.....89..966D) is used to
estimate the gravitational interaction strength [log(Ftital/Fbinding)]
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Galaxy name (1)
13- 16 A4 --- Prof Disc-profile type (3)
19- 23 F5.2 kpc Rb.pc [0.5/34]?=- Break radius in kiloparsecs
25- 28 F4.2 kpc e_Rb.pc ?=- rms uncertainty on Rbreakpc
30- 35 F6.2 arcsec Rbr [17/334]?=- Break radius in arcseconds
37- 41 F5.2 arcsec e_Rbr ?=- rms uncertainty on Rbreak
43- 48 F6.2 mag/arcsec2 SBbr ?=- Surface brightness at the break
(AB scale, 3.6um)
50- 53 F4.2 mag/arcsec2 e_SBbr ?=- rms uncertainty on SBbreak
55- 59 F5.2 mag/arcsec2 SBi Extrapolated central surface brightness of
the disc inside the break (AB, 3.6um) (2)
61- 64 F4.2 mag/arcsec2 e_SBi rms uncertainty on SBi
66- 70 F5.2 kpc hi.pc [0.2/30] Scalelength of the disc inside the
break in kiloparsecs (2)
72- 75 F4.2 kpc e_hi.pc rms uncertainty on hi.pc
77- 82 F6.2 arcsec hi [5/560] Scalelength of the disc inside the
break in arcseconds (2)
84- 88 F5.2 arcsec e_hi rms uncertainty on hi
90- 94 F5.2 mag/arcsec2 SBo ?=- Extrapolated central surface brightness
of the disc outside the break (AB, 3.6um)
96- 99 F4.2 mag/arcsec2 e_SBo ?=- rms uncertainty on SBo
101-105 F5.2 kpc ho.pc [0.1/21]?=- Scalelength of the disc outside
the break in kiloparsecs
107-110 F4.2 kpc e_ho.pc ?=- rms uncertainty on ho.pc
112-117 F6.2 arcsec ho [7/185]?=- scalelength of the disc outside
the break in arcseconds
119-123 F5.2 arcsec e_ho ?=- rms uncertainty on ho
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Note (1): If a galaxy has two lines in this file then the latter line
corresponds to another outer break.
Note (2): for type I discs this is the main disc.
Note (3): the classification of profile types is:
I = classical single exponential disc
II = downbending dual-exponential disc (outer disc has a lower
scalelength than the inner disc)
II.i = the break is at or inside the bar radius
III = upbneding dual-exponential disc (outer disc has a larger
scalelength than the inner disc)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Feb-2015