The SAMI Galaxy Survey: Exploring the gas-phase Mass-Metallicity Relation. (arXiv:1812.11263v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_S/0/1/0/all/0/1">S.F. Sanchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barrera_Ballesteros_J/0/1/0/all/0/1">J.K. Barrera-Ballesteros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Coba_C/0/1/0/all/0/1">C. Lopez-Coba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brough_S/0/1/0/all/0/1">S. Brough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bryant_J/0/1/0/all/0/1">J. J. Bryant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bland_Hawthorn_J/0/1/0/all/0/1">J. Bland-Hawthorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Croom_S/0/1/0/all/0/1">S. M. Croom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sande_J/0/1/0/all/0/1">J. van de Sande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortese_L/0/1/0/all/0/1">L. Cortese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goodwin_M/0/1/0/all/0/1">M. Goodwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lawrence_J/0/1/0/all/0/1">J.S. Lawrence</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Sanchez_A/0/1/0/all/0/1">A. R. Lopez-Sanchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sweet_S/0/1/0/all/0/1">S. M. Sweet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Owers_M/0/1/0/all/0/1">M. S. Owers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richards_S/0/1/0/all/0/1">S. N. Richards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walcher_C/0/1/0/all/0/1">C. J. Walcher</a>

We present a detailed exploration of the stellar mass vs. 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) nor the specific SFR (SFR/Mass) 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 ($r_csim -$0.3), it is confined to the low mass regime
(M*<10$^9$Msun) or high SFR regimes, and it does not produce any significant improvement in the {description of the average population of galaxies. The aparent disagreement with published results based on single fiber 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

We present a detailed exploration of the stellar mass vs. 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) nor the specific SFR (SFR/Mass) 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 ($r_csim -$0.3), it is confined to the low mass regime
(M*<10$^9$Msun) or high SFR regimes, and it does not produce any significant
improvement in the {description of the average population of galaxies. The
aparent disagreement with published results based on single fiber 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

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