J/A+A/587/A70 CALIFA face-on spiral galaxies oxygen (Sanchez-Menguiano+, 2016)
Shape of the oxygen abundance profiles in CALIFA face-on spiral galaxies.
Sanchez-Menguiano L., Sanchez S.F., Perez I., Garcia-Benito R.,
Husemann B., Mast D., Mendoza A., Ruiz-Lara T., Ascasibar Y.,
Bland-Hawthorn J., Cavichia O., Diaz A.I., Florido E., Galbany L.,
Gonzalez Delgado R.M., Kehrig C., Marino R.A., Marquez I., Masegosa J.,
Mendez-Abreu J., Molla M., Del Olmo A., Perez E., Sanchez-Blazquez P.,
Stanishev V., Walcher C.J., Lopez-Sanchez A.R., (the Califa collaboration)
<Astron. Astrophys., 587, A70-70 (2016)>
=2016A&A...587A..70S 2016A&A...587A..70S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Abundances
Keywords: galaxies: abundances - galaxies: evolution - galaxies: ISM -
galaxies: spiral - techniques: imaging spectroscopy -
techniques: spectroscopic
Abstract:
We measured the gas abundance profiles in a sample of 122 face-on
spiral galaxies observed by the CALIFA survey and included all spaxels
whose line emission was consistent with star formation. This type of
analysis allowed us to improve the statistics with respect to previous
studies, and to properly estimate the oxygen distribution across the
entire disc to a distance of up to 3-4 disc effective radii (re). We
confirm the results obtained from classical HII region analysis. In
addition to the general negative gradient, an outer flattening can be
observed in the oxygen abundance radial profile. An inner drop is also
found in some cases. There is a common abundance gradient between 0.5
and 2.0re of αO/H=-0.075dex/re with a scatter of
σ=0.016dex/re when normalising the distances to the disc
effective radius. By performing a set of Kolmogorov-Smirnov tests, we
determined that this slope is independent of other galaxy properties,
such as morphology, absolute magnitude, and the presence or absence of
bars. In particular, barred galaxies do not seem to display shallower
gradients, as predicted by numerical simulations. Interestingly, we
find that most of the galaxies in the sample with reliable oxygen
abundance values beyond ∼2 effective radii (57 galaxies) present a
flattening of the abundance gradient in these outer regions. This
flattening is not associated with any morphological feature, which
suggests that it is a common property of disc galaxies. Finally, we
detect a drop or truncation of the abundance in the inner regions of
27 galaxies in the sample; this is only visible for the most massive
galaxies.
Description:
The analysed data were selected from the 939 galaxies that comprise
the CALIFA mother sample. These galaxies were observed using the
Potsdam Multi Aperture Spectrograph (PMAS) at the 3.5m telescope of
the Calar Alto observatory with a configuration called PPAK.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 68 122 Fundamental properties and oxygen abundance
information
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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)
J/A+A/585/A47 : CALIFA color/metallicity gradients connections (Marino+, 2016)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Galaxy name
15- 19 A5 --- MType Morphological type
22- 27 F6.2 mag gMAG g-band absolute magnitude
29- 33 F5.2 [Msun] logMass log10 of the integrated stellar mass
35- 39 F5.2 kpc re Disc effective radius
41- 44 F4.2 [-] [O/H]re Oxygen abundance value at one effective radius
46- 49 F4.2 [-] e_[O/H]re rms uncertainty on [O/H]re
51- 56 F6.3 --- alpha[O/H] Slope of the oxygen abundance gradient
measured between 0.5 and 2.0 re (in dex/re)
58- 62 F5.3 --- e_alpha[O/H] rms uncertainty on slope
64- 68 F5.3 --- CC Correlation coefficient of the linear fit
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-May-2016