J/MNRAS/484/3042 The gas-phase mass-metallicity relation (Sanchez+, 2019)
The SAMI galaxy survey: exploring the gas-phase mass-metallicity relation.
Sanchez S.F., Barrera-Ballesteros J.K., Lopez-Coba C., Brough S.,
Bryant J.J., Bland-Hawthorn J., Croom S.M., van de Sande J., Cortese L.,
Goodwin M., Lawrence J.S., Lopez-Sanchez A.R., Sweet S.M., Owers M.S.,
Richards S.N., Walcher C.J., (the Sami Team)
<Mon. Not. R. Astron. Soc., 484, 3042-3070 (2019)>
=2019MNRAS.484.3042S 2019MNRAS.484.3042S (SIMBAD/NED BibCode)
ADC_Keywords: Spectroscopy ; Abundances ; Galaxies, spectra ;
Interstellar medium ; Optical
Keywords: techniques: spectroscopic - galaxies: abundances -
galaxies: evolution - galaxies: ISM
Abstract:
We present a detailed exploration of the stellar mass versus gas-phase
metallicity relation (MZR) using integral field spectroscopy data
obtained from ∼1000 galaxies observed by the SAMI galaxy survey. These
spatially resolved spectroscopic data allow us to determine the
metallicity within the same physical scale (Reff) for different
calibrators. The shape of the MZ relations is very similar between the
different calibrators, while there are large offsets in the absolute
values of the abundances. We confirm our previous results derived
using the spatially resolved data provided by the CALIFA and MaNGA
surveys: (1) we do not find any significant secondary relation of the
MZR with either the star formation rate (SFR) or the specific SFR
(SFR/M*) for any of the calibrators used in this study, based on the
analysis of the individual residuals; (2) if there is a dependence
with the SFR, it is weaker than the reported one (rc~-0.3), it is
confined to the low-mass regime (M*<109M☉) or high-SFR
regimes, and it does not produce any significant improvement in the
description of the average population of galaxies. The apparent
disagreement with published results based on single-fibre
spectroscopic data could be due to (i) the interpretation of the
secondary relation itself; (ii) the lower number of objects sampled at
the low-mass regime by the current study; or (iii) the presence of
extreme star-forming galaxies that drive the secondary relation in
previous results.
Description:
The selection of the SAMI galaxy survey sample is described in detail
in Bryant et al. (2015MNRAS.447.2857B 2015MNRAS.447.2857B), with further details in Owers
et al. (2017MNRAS.468.1824O 2017MNRAS.468.1824O). A comparison with the sample selection
of other integral field spectroscopic surveys was presented in Sanchez
et al. (2017MNRAS.469.2121S 2017MNRAS.469.2121S, Cat. J/MNRAS/469/2121).
The sample analysed here consists of a random sub-set of the foreseen
final sample of SAMI targets (just over 3000 objects once the survey
is completed). It comprises the 2307 galaxies observed by August 2017,
included in the internal SAMI v0.10 distribution. These galaxies cover
the redshift range between 0.005<z<0.1, with stellar masses between
∼107-1011.5M☉, and with an extensive coverage of the
colour-magnitude diagram.
The SAMI observational setup uses the two arms of the spectrograph,
one in the blue, covering the wavelength range between ∼3700Å and
∼5700Å with a resolution of ∼173km/s (FWHM), and one in the red,
covering the wavelength range between ∼6250Å and ∼7350Å, with a
resolution of ∼67km/s (FWHM). Therefore, the standard data-reduction
produces two different data cubes, with two different wavelength
ranges, spectral resolutions and spectral sampling. In this analysis,
we combined those two data cubes into a single cube, following a
similar procedure as that adopted for the CALIFA data cubes (e.g.
Sanchez et al. 2016A&A...594A..36S 2016A&A...594A..36S, Cat. J/A+A/594/A36), by (i)
degrading the resolution of the red-arm (R∼4300) data cubes to that of
the blue-arm (R∼1800), (ii) re-sampling the full spectra to a common
sampling of 1Å, and (iii) correcting them for Galactic extinction,
using the attenuation curves provided by the SAMI data-reduction. The
stellar masses, star-formation rates, and oxygen abundances for 1044
galaxies extracted from the SAMI galaxy survey are listed in Table E1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablee1.dat 240 2255 Stellar Masses, star-formation rates, and
characteristics abundances for the all the
considered calibrators
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See also:
http://sami-survey.org : SAMI Galaxy Survey Home Page
Byte-by-byte Description of file: tablee1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Galaxy name (SAMINNNNNNNNN)
16- 23 F8.5 [Msun] logMass Stellar mass
25- 32 F8.6 [Msun] e_logMass Error on logMass
34- 43 F10.6 [Msun/yr] logSFR Star formation rate
45- 53 F9.7 [Msun/yr] e_logSFR Error on logSFR
55- 61 F7.5 [-] OHo3n2-m13 ? Oxygen abundance based on the O3N2
calibrator from Marino et al.
(2013A&A...559A.114M 2013A&A...559A.114M,
Cat. J/A+A/559/A114) (1)
63- 70 F8.6 [-] e_OHo3n2-m13 ? Error on OHo3n2-m13
72- 78 F7.5 [-] OHn2-m13 ? Oxygen abundance based on the N2
calibrator from Marino et al.
(2013A&A...559A.114M 2013A&A...559A.114M,
Cat. J/A+A/559/A114) (1)
80- 87 F8.6 [-] e_OHn2-m13 ? Error on OHn2-m13
89- 95 F7.5 [-] OHons ? Oxygen abundance based on the ONS
calibrator from
Pilyugin, Vilchez & Thuan
(2010ApJ...720.1738P 2010ApJ...720.1738P) (1)
97-104 F8.6 [-] e_OHons ? Error on OHons
106-112 F7.5 [-] OHr23 ? Oxygen abundance based on the R23
calibrator from Kobulnicky & Kewley
(2004ApJ...617..240K 2004ApJ...617..240K,
Cat. J/ApJ/617/240) (1)
114-121 F8.6 [-] e_OHr23 ? Error on OHr23
123-129 F7.5 [-] OHo3n2-pp04 ? Oxygen abundance based on the O3N2
indicator by Pettini & Pagel
(2004MNRAS.348L..59P 2004MNRAS.348L..59P) (3)
131-138 F8.6 [-] e_OHo3n2-pp04 ? Error on OHo3n2-pp04
140-146 F7.5 [-] OHpyqz ? Oxygen abundance provided by the pyqz
code (Vogt et al. 2015MNRAS.450.2593V 2015MNRAS.450.2593V)
as described by Dopita et al.
(2013ApJS..208...10D 2013ApJS..208...10D
Cat. J/ApJS/208/10) (4)
148-155 F8.6 [-] e_OHpyqz ? Error on OHpyqz
157-163 F7.5 [-] OHt2 ? t2 correction proposed by
Pena-Guerrero, Peimbert & Peimbert
(2012ApJ...756L..14P 2012ApJ...756L..14P), for the average
oxygen abundance estimated from the
four calibrators included in the first
family (2)
165-172 F8.6 [-] e_OHt2 ? Error on OHt2
174-180 F7.5 [-] OHm08 ? Oxygen abundance based on a
combination or R23 and the previous
one proposed by Maiolino et al.
(2008A&A...488..463M 2008A&A...488..463M) (3)
182-189 F8.6 [-] e_OHm08 ? Error on OHm08
191-197 F7.5 [-] OHt04 ? Oxygen abundance based on the R23
calibrator described by Tremonti et al.
(2004ApJ...613..898T 2004ApJ...613..898T) (4)
199-206 F8.6 [-] e_OHt04 ? Error on OHt04
208-214 F7.5 [-] OHdop ? Oxygen abundance described by
Dopita et al. (2016Ap&SS.361...61D 2016Ap&SS.361...61D),
based on the N2/S2 and N2 line
ratios (4)
216-223 F8.6 [-] e_OHdop ? Error on OHdop
225-231 F7.5 [-] OHepm ? Oxygen abundance based on a version
of the O3N2 calibrator that corrects
for relative abundance from nitrogen
to oxygen from Perez-Montero & Contini
(2009MNRAS.398..949P 2009MNRAS.398..949P) (1)
233-240 F8.6 [-] e_OHepm ? Error on OHepm
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Note (1): First family of calibrators based or anchored to estimations done
using the Direct Method (DM; Perez-Montero 2017PASP..129d3001P 2017PASP..129d3001P)
Note (2): Second family of calibrators that consider the inhomogeneities in the
electron temperature in ionized nebulae, known as the t2 correction
(Peimbert 1967ApJ...150..825P 1967ApJ...150..825P)
Note (3): Third family of calibrators that use the values anchored to the DM
only for the low-abundance regime, using values derived from
photoionization models for the high-abundance regime (i.e. mixed
calibrators)
Note (4): Fourth family of calibrators anchored to the predictions by
photoionization models
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 18-Aug-2022