J/A+A/585/A47 CALIFA color/metallicity gradients connections (Marino+, 2016)
Outer-disk reddening and gas-phase metallicities: The CALIFA connection.
Marino R.A., Gil de Paz A., Sanchez S.F., Sanchez-Blazquez P., Cardiel N.,
Castillo-Morales A., Pascual S., Vilchez J., Kehrig C., Molla M.,
Mendez-Abreu J., Catalan-Torrecilla C., Florido E., Perez I., Ruiz-Lara T.,
Ellis S., Lopez-Sanchez A.R., Gonzalez Delgado R.M., De Lorenzo-Caceres A.,
Garcia-Benito R., Galbany L., Zibetti S., Cortijo C., Kalinova V., Mast D.,
Iglesias-Paramo J., Papaderos P., Walcher C.J., Bland-Hawthorn J.,
(the Califa Team)
<Astron. Astrophys., 585, A47-47 (2016)>
=2016A&A...585A..47M 2016A&A...585A..47M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, SDSS
Keywords: galaxies: abundances - galaxies: evolution - galaxies: photometry -
galaxies: ISM - ISM: abundances - HII regions
Abstract:
We study, for the first time in a statistically significant and
well-defined sample, the relation between the outer-disk ionized-gas
metallicity gradients and the presence of breaks in the surface
brightness profiles of disk galaxies. Sloan Digital Sky Survey (SDSS)
g'- and r'-band surface brightness, (g'-r') color, and ionized-gas
oxygen abundance profiles for 324 galaxies within the Calar Alto
Legacy Integral Field Area (CALIFA) survey are used for this purpose.
We perform a detailed light-profile classification, finding that 84%
of our disks show down- or up-bending profiles (Type II and Type III,
respectively), while the remaining 16% are well fitted by one single
exponential (Type I). The analysis of the color gradients at both
sides of this break shows a U-shaped profile for most Type II galaxies
with an average minimum (g'-r') color of ∼0.5mag and an ionized-gas
metallicity flattening associated with it only in the case of low-mass
galaxies. Comparatively, more massive systems show a rather uniform
negative metallicity gradient. The correlation between metallicity
flattening and stellar mass for these systems results in p-values as
low as 0.01. Independent of the mechanism having shaped the outer
light profiles of these galaxies, stellar migration or a previous
episode of star formation in a shrinking star-forming disk, it is
clear that the imprint in their ionized-gas metallicity was different
for low- and high-mass Type II galaxies. In the case of Type III
disks, a positive correlation between the change in color and
abundance gradient is found (the null hypothesis is ruled out with a
p-value of 0.02), with the outer disks of Type III galaxies with
masses ≤1010M☉ showing a weak color reddening or even a
bluing. This is interpreted as primarily due to a mass downsizing
effect on the population of Type III galaxies that recently
experienced an enhanced inside-out growth.
Description:
We have selected the 350 galaxies observed by the CALIFA survey
(Sanchez et al., 2012A&A...538A...8S 2012A&A...538A...8S) at the CAHA 3.5m telescope with
Potsdam Multi Aperture Spectrograph (PMAS) in the PPak mode and
processed by the CALIFA v1.5 pipeline up to September 2014.
The SDSS g' and r' SB and (g'-r') color profiles were derived using the
DR10 data products, in particular, we used the swarp mosaicking code
(Ahn et al., 2014ApJS..211...17A 2014ApJS..211...17A).
We obtain spectroscopic information for ∼15130 HII regions (or
complexes) from our 324 CALIFA data cubes using HII explorer.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 86 326 Disk classification and physical properties of
the CALIFA galaxies
tableb2.dat 74 131 Derived physical properties at break radius for
the CALIFA galaxies
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See also:
J/A+A/559/A114 : Updated O3N2 and N2 abundance indicators (Marino+, 2013)
J/A+A/573/A59 : Gas kinematics in CALIFA survey (Garcia-Lorenzo+, 2015)
J/A+A/576/A135 : CALIFA DR2 (Garcia-Benito+, 2015)
J/A+A/581/A103 : CALIFA survey across the Hubble sequence (Gonzalez+, 2015)
J/A+A/582/A21 : Merging galaxies (mis)alignments (Barrera-Ballesteros+, 2015)
J/A+A/584/A87 : CALIFA sample SFR calibration (Catalan-Torrecilla+, 2015)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name (G1)
17- 22 F6.4 --- z Heliocentric redshift z distance obtained
from the NED database
25- 32 A8 --- PType Photometrical type obtained from our analysis
of the SDSS r'-band profile
36- 40 A5 --- MType Morphological type
44- 48 F5.2 [Msun] log(M*) ?=- Stellar mass
52- 57 F6.2 mag RMAG ?=- Absolute R-band magnitude
60- 64 F5.2 kpc Reff Effective radius
68- 71 F4.2 --- Rg'b ?=- Break radii obtained as the minimum of the
double bootstrapping fit to the
SDSS g'-band in Reff unit
73- 76 F4.2 --- e_Rg'b ? rms uncertainty on Rgb
78- 81 F4.2 --- Rr'b ?=- Break radii obtained as the minimum of the
double bootstrapping fit to the
SDSS i'-band in Reff unit
83- 86 F4.2 --- e_Rr'b ? rms uncertainty on Rr'b
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Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Galaxy name (G1)
17- 24 A8 --- PhotT Photometrical type obtained from our
analysis of the SDSS r'-band profiles
26- 29 F4.2 --- Rr'b Break radius obtained as the minimum
of the double bootstrapping fit to
the SDSS r'-band data in units of
their Reff
31- 34 F4.2 --- e_Rr'b rms uncertainty on Rr'b
36- 40 F5.3 --- Da(O/H) Difference between the outer-to-the-
inner slopes as measured in the
oxygen profiles
42- 46 F5.3 --- e_Da(O/H) rms uncertainty on Da(O/H)
48- 52 F5.3 --- Dacolor Difference between the outer-to-the-
inner slopes as measured in the
(g'-r') color profiles
54- 58 F5.3 --- e_Dacolor rms uncertainty on Dacolor
60- 64 F5.2 mag/arcsec+2 mur'brk r'-band surface brightness computed at
the r' break radius
66- 69 F4.2 mag (g'-r')r'b color value computed at the r' break
radius
71- 74 F4.2 [-] (O/H)r'b Oxygen abundance value computed at
the r' break radius
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Global notes:
Note (G1): SDSS J100141 = SDSS J100141.02+371447.4,
2MASXJ01331766 = 2MASX J01331766+1319567
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Mar-2016