J/ApJ/771/59 Surface brightness of S4G face-on galaxies (Munoz-Mateos+, 2013)
The impact of bars on disk breaks as probed by S4G imaging.
Munoz-Mateos J.C., Sheth K., Gil de Paz A., Meidt S., Athanassoula E.,
Bosma A., Comeron S., Elmegreen D.M., Elmegreen B.G., Erroz-Ferrer S.,
Gadotti D.A., Hinz J.L., Ho L.C., Holwerda B., Jarrett T.H., Kim T.,
Knapen J.H., Laine J., Laurikainen E., Madore B.F., Menendez-Delmestre K.,
Mizusawa T., Regan M., Salo H., Schinnerer E., Seibert M., Skibba R.,
Zaritsky D.
<Astrophys. J., 771, 59 (2013)>
=2013ApJ...771...59M 2013ApJ...771...59M
ADC_Keywords: Galaxies, nearby ; Morphology ; Photometry, infrared
Keywords: galaxies: evolution; galaxies: photometry; galaxies: spiral;
galaxies: stellar content; galaxies: structure
Abstract:
We have analyzed the radial distribution of old stars in a sample of
218 nearby face-on disks, using deep 3.6µm images from the Spitzer
Survey of Stellar Structure in Galaxies. In particular, we have
studied the structural properties of those disks with a broken or
down-bending profile. We find that, on average, disks with a genuine
single-exponential profile have a scale length and a central surface
brightness which are intermediate to those of the inner and outer
components of a down-bending disk with the same total stellar mass. In
the particular case of barred galaxies, the ratio between the break
and the bar radii (Rbr/Rbar) depends strongly on the total stellar
mass of the galaxy. For galaxies more massive than 1010M☉, the
distribution is bimodal, peaking at Rbr/Rbar∼2 and ∼3.5. The first
peak, which is the most populated one, is linked to the outer Lindblad
resonance of the bar, whereas the second one is consistent with a
dynamical coupling between the bar and the spiral pattern. For
galaxies below 1010M☉, breaks are found up to ∼10Rbar, but
we show that they could still be caused by resonances given the rising
nature of rotation curves in these low-mass disks. While not ruling
out star formation thresholds, our results imply that radial stellar
migration induced by non-axisymmetric features can be responsible not
only for those breaks at ∼2Rbar, but also for many of those found at
larger radii.
Description:
The full Spitzer Survey of Stellar Structure in Galaxies (S4G; Sheth
et al. 2010, Cat. J/PASP/122/1397) sample comprises a total of more
than 2300 nearby galaxies. They were selected from the HyperLEDA
database (Paturel et al. 2003, Cat. VII/237) according to the
following selection criteria: radio-derived radial velocity
vradio<3000km/s (which corresponds to d≲40Mpc for H0=71km/s/Mpc),
Galactic latitude |b|>30°, total corrected blue magnitude
mBcorr<15.5 and blue light isophotal diameter D25>1.0'.
We selected only disk-like galaxies ranging from S0's to Sd's (that
is, having numerical types -3≤T≤7), using the optical morphological
types compiled in HyperLEDA. We retained only galaxies with
M3.6um(AB)←18mag. Finally, we required our galaxies to be at least
moderately face-on, having an axial ratio b/a>0.5 (i<60°) at
µ3.6um=25.5(AB)mag/arcsec2, which we take as our fiducial
surface brightness level for the outer parts of disks. Our final
sample contains 218 galaxies, including both barred and unbarred ones,
whose main properties are quoted in Table 1.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 74 218 Sample
table2.dat 158 227 Profile measurements for the 218 galaxies
table3.dat 103 146 Bar properties
--------------------------------------------------------------------------------
See also:
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
J/ApJ/733/74 : GALEX - SDSS properties of local galaxies (Lemonias+, 2011)
J/ApJ/722/L120 : Central surface brightness of SDSS galaxies (Fathi, 2010)
J/PASP/122/1397 : Spitzer Survey of gal. Stellar Struct.: S4G (Sheth+, 2010)
J/MNRAS/393/1531 : BUDDA structural properties of galaxies (Gadotti+, 2009)
J/ApJ/703/1569 : SINGS galaxies radial distribution. I. (Munoz-Mateos+, 2009)
J/ApJ/684/1026 : Photometric profiles from GOODS data (Azzollini+, 2008)
J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)
J/AJ/136/2563 : HI Nearby Galaxy Survey, THINGS (Walter+, 2008)
J/AJ/133/2846 : Photometric decomposition of barred galaxies (Reese+, 2007)
J/ApJ/659/1176 : Study of bars in 180 spiral galaxies (Marinova+, 2007)
J/ApJS/173/572 : GALEX/Spitzer photometry in NGC 7331 (Thilker+, 2007)
J/ApJS/162/49 : UBV imaging of irregular galaxies (Hunter+, 2006)
J/ApJS/156/345 : Surface photometry of BCD galaxies (Gil De Paz+, 2005)
J/MNRAS/355/1251 : Bar-induced strengths in galaxies (Laurikainen+, 2004)
J/MNRAS/332/422 : Galaxies morphology and IR photometry. VIII (Pierini+, 2002)
J/A+AS/121/507 : Near-IR surface photometry of Virgo galaxies (Boselli+ 1997)
http://leda.univ-lyon1.fr/ : HyperLeda online database
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name
12- 13 I2 h RAh Hour of Right Ascension (J2000)
15- 16 I2 min RAm Minute of Right Ascension (J2000)
18- 21 F4.1 s RAs Second of Right Ascension (J2000)
23 A1 --- DE- Sign of the Declination (J2000)
24- 25 I2 deg DEd Degree of Declination (J2000)
27- 28 I2 arcmin DEm Arcminute of Declination (J2000)
30- 33 F4.1 arcsec DEs Arcsecond of Declination (J2000)
35- 38 A4 --- Morph Morphology classification
40- 43 F4.1 --- TT [-3/7] T type classification
45- 48 F4.1 Mpc Dist [2/49] Distance
50- 54 F5.1 arcsec R [35/671] Radius at 25.5 mag/"2 isophote
56- 60 F5.3 --- ell [0/1] Ellipticity (1-b/a) of 25.5 mag/"2
isophote
62- 67 F6.1 deg pa [-180/90] Position angle of 25.5mag/"2
isophote
69- 74 F6.2 mag 3.6Mag [-23.3/-18] Spitzer/IRAC 3.6um band absolute
AB magnitude
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name
12- 21 A10 --- Prof Profile type (1)
23- 28 F6.2 arcsec r1i First radial limit on inner exponential
30- 35 F6.2 arcsec r2i Second radial limit on inner exponential
37- 42 F6.2 arcsec r1o ? First radial limit on outer exponential
44- 49 F6.2 arcsec r2o ? Second radial limit on outer exponential
51- 55 F5.2 mag/arcsec2 mu0i [16.5/22.7] Extrapolated central surface
brightness of inner exponential
57- 60 F4.2 mag/arcsec2 E_mu0i Upper 1σ uncertainty in mu0i
62- 65 F4.2 mag/arcsec2 e_mu0i Lower 1σ uncertainty in mu0i
67- 71 F5.2 mag/arcsec2 mu0o [13.6/22.7]? Extrapolated central surface
brightness of outer exponential
73- 76 F4.2 mag/arcsec2 E_mu0o ? Upper 1σ uncertainty in mu0o
78- 82 F5.2 mag/arcsec2 e_mu0o ? Lower 1σ uncertainty in mu0o
84- 89 F6.2 arcsec hi [4.7/207] Inner disk scale-length hi (2)
91- 96 F6.2 arcsec E_hi ? Upper 1σ uncertainty in hi
98-103 F6.2 arcsec e_hi Lower 1σ uncertainty in hi
105-110 F6.2 arcsec ho [4.3/112]? Outer disk scale-length ho (2)
112-116 F5.2 arcsec E_ho ? Upper 1σ uncertainty in ho
118-122 F5.2 arcsec e_ho ? Lower 1σ uncertainty in ho
124-129 F6.2 arcsec Rbr [12.9/289]? Break radius Rbr (2)
131-135 F5.2 arcsec E_Rbr ? Upper 1σ uncertainty in Rbr
137-141 F5.2 arcsec e_Rbr ? Lower 1σ uncertainty in Rbr
143-147 F5.2 arcsec-1 alpha [0.06/31]? Break sharpness (2)
149-153 F5.2 arcsec-1 E_alpha ? Upper 1σ uncertainty in alpha
155-158 F4.2 arcsec-1 e_alpha ? Lower 1σ uncertainty in alpha
--------------------------------------------------------------------------------
Note (1): The profiles are are divded into three main borad categories (see
section 3.2; terms between brackets denote an uncertain classification):
1 = single exponential, i.e. I(r)=I0exp(-r/h)
2 = down-bending; in type 2 barred galaxies, the break can be
inside the bar radius (2i) or outside (2o).
in the outer part, while in type 3d (disk) the allipticity remains
roughly constant beyond the break radius.
Note (2): Low α values correspond to a smooth transition between
the inner and outer disk and high values yielded a sharper break.
The profile is defined by:
I(r) = S I0 exp(-r/hi) [1+exp(α(r-Rbr))]γ
γ = 1/α(1/hi-1/ho)
S = [1+exp(αRbr]-γ
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name
12- 12 A1 --- Bar Bar flag (B: barred; C: candidate bar)
14- 16 I3 arcsec a1 [2/128] Radius at maximum ellipticity
18- 22 F5.3 --- e1 [0/1] Ellipticity at maximum ellipticity
24- 28 F5.1 deg pa1 Position angle at maximum ellipticity
30- 32 I3 arcsec a0 [4/166] Radius at minimum ellipticity
34- 38 F5.3 --- e0 [0/1] Ellipticity at minimum ellipticity
40- 44 F5.1 deg pa0 Position angle at minimum ellipticity
46- 50 F5.1 arcsec a10 ? Radius where PA departs by 10 degrees from
maximum ellipticity
52- 56 F5.3 --- e10 [0/1]? Ellipticity where PA departs by 10
degrees from maximum ellipticity (pa1)
58- 62 F5.1 deg pa10 [0/180]? Position angle where PA departs by 10
degrees from maximum ellipticity (pa1)
64- 68 F5.1 arcsec a0.1 ? Radius where ellipticity drops by 0.1 with
respect of maximum ellipticity (e1)
70- 74 F5.3 --- e0.1 [0/1]? Ellipticity where ellipticity drops
by 0.1 with respect of maximum ellipticity e1
76- 80 F5.1 deg pa0.1 [0/180]? Position angle where ellipticity drops
by 0.1 with respect of maximum ellipticity e1
82- 86 F5.1 arcsec a [2.5/145] Final adopted radius (1)
88- 91 F4.1 arcsec e_a [0.1/32] Uncertainty in a (1)
93- 97 F5.3 --- e [0/1] Final adopted ellipticity (1)
99-103 F5.1 deg PA [0/180] Final adopted position angle (1)
--------------------------------------------------------------------------------
Note (1): Corrected for inclination.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 19-Jan-2015