J/A+A/666/A186 MZ-SFR in SDSS star-forming galaxies (Duarte Puertas+, 2022)
Mass-metallicity and star formation rate in galaxies:
A complex relation tuned to stellar age.
Duarte Puertas S., Vilchez J.M., Iglesias-Paramo J., Molla M.,
Perez-Montero E., Kehrig C., Pilyugin L.S., Zinchenko I.A.
<Astron. Astrophys. 666, A186 (2022)>
=2022A&A...666A.186D 2022A&A...666A.186D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Redshifts ; Abundances ; Stars, masses ; Optical
Keywords: galaxies: general - galaxies: star forming - galaxies: abundances -
galaxies: evolution
Abstract:
In this work we study the stellar mass -- metallicity relation (MZR)
of an extended sample of star-forming galaxies in the local Universe
and its possible dependence with the star formation rate (SFR).
A sample of ∼195000 Sloan Digital Sky Survey (SDSS) star-forming
galaxies has been selected up to z=0.22 with the aim of analysing the
behaviour of the relation of MZR with respect to SFR and taking into
account the age of their stellar populations.
For this sample we have obtained, for the first time, aperture
corrected oxygen and nitrogen-to-oxygen abundances (O/H and N/O,
respectively) and SFR using the empirical prescriptions from the Calar
Alto Legacy Integral Field Area (CALIFA) survey. To perform this study
we make use also of the stellar mass of the galaxies and the parameter
Dn(4000) as a proxy of the age of the stellar population.
We derive a robust MZR locus, which is found to be fully consistent
with the "anchoring" points of a selected set of well studied nearby
galaxies with a direct derivation of the chemical abundance. A complex
relation between MZR and SFR across the whole range of galaxy mass and
metallicity has been observed, where the slope changes seen in the O/H
-- SFR plane present a pattern which seems to be tuned to the
galaxies' stellar age, and therefore, stellar age has to be taken into
account in the stellar mass -- metallicity -- SFR relation.
In order to provide an answer to the question of whether or not the
MZR depends on the SFR it is essential to take into account the age of
the stellar populations of galaxies. A strong dependence between the
MZR and SFR is observed mainly for star-forming galaxies with strong
SFR values and low Dn(4000). The youngest galaxies of our SDSS sample
show the highest SFR measured for their stellar mass.
Description:
Our study is based on the MPA-JHU public catalogue (Kauffmann et al..
2003MNRAS.341...33K 2003MNRAS.341...33K; Brinchmann et al., 2004MNRAS.351.1151B 2004MNRAS.351.1151B; Tremonti
et al., 2004ApJ...613..898T 2004ApJ...613..898T; Salim et al., 2007ApJS..173..267S 2007ApJS..173..267S), which
gives spectroscopic data of the galaxies in the Sloan Digital Sky
Survey Data Release 7 (SDSS-DR7) (Abazajian et al.,
2009ApJS..182..543A 2009ApJS..182..543A). The SDSS spectroscopic primary sample of
galaxies is complete in Petrosian r magnitude in the range
14.5≤r≤17.7 (Strauss et al., 2002AJ....124.1810S 2002AJ....124.1810S; Brinchmann et
al. ArXiv e-prints [arXiv:astro-ph/0406220]). We added the photometric
data from the SDSS-DR12 (York et al., 2000AJ....120.1579Y 2000AJ....120.1579Y; Alam et
al., 2015ApJS..219...12A 2015ApJS..219...12A, Cat. V/147) to the MPA-JHU catalogue.
We selected a subset of 194353 star-forming galaxies. For these
star-forming galaxies we derived aperture-corrected oxygen and
nitrogen-to-oxygen abundances using the empirical aperture corrections
of Iglesias-Paramo et al. (2016ApJ...826...71I 2016ApJ...826...71I, Cat. J/ApJ/826/71) and
the calibrators of Pilyugin & Grebel (2016MNRAS.457.3678P 2016MNRAS.457.3678P).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 126 194353 Catalogue of 194353 SDSS star-forming galaxies
empirically corrected for aperture using
Iglesias-Paramo et al. (2016ApJ...826...71I 2016ApJ...826...71I):
oxygen and nitrogen-to-oxygen abundance and
related relevant data
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See also:
J/A+A/599/A71 : 209276 SDSS star-forming galaxies aperture-free (Duarte+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- specObjID SDSS-DR12 unique spectrum identification
21- 28 F8.4 deg RAdeg Right Ascension (J2000) from SDSS
30- 37 F8.4 deg DEdeg Declination (J2000) from SDSS
39- 44 F6.4 --- z Spectroscopic redshift
46- 52 F7.4 --- logOH 12+log(O/H) corrected for aperture
effects (1)
54- 59 F6.4 --- e_logOH Uncertainty of 12+log(O/H) corrected for
aperture effects (1)
61- 67 F7.4 --- logNO Log of nitrogen-to-oxygen abundance ratio
corrected for aperture effects (1)
69- 74 F6.4 --- e_logNO Uncertainty of Log of nitrogen-to-oxygen
abundance ratio corrected for aperture
effects (1)
76- 82 F7.4 [Msun/yr] logSFR Log of total star formation rate corrected
for aperture effects (2)
84- 89 F6.4 [Msun/yr] e_logSFR Uncertainty of Log of total star formation
rate corrected for aperture effects
91- 97 F7.4 --- Dn4000 Dn(4000) parameter (3)
99-104 F6.4 --- e_Dn4000 Uncertainty of Dn(4000) parameter (3)
106-112 F7.4 [Msun] logMass Log of total stellar mass (3)
114-119 F6.4 [Msun] E_logMass Uncertainty of Log of total stellar mass,
upper limit at the 1 sigma level (3)
121-126 F6.4 [Msun] e_logMass Uncertainty of Log of total stellar mass,
lower limit at the 1 sigma level (3)
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Note (1): Derived using Pilyugin & Grebel (2016MNRAS.457.3678P 2016MNRAS.457.3678P) equations as:
- For 12+log(O/H): R calibrator, equations 4 and 5
- For log(N/O): equation 13
Note (2): Taken from Duarte Puertas et al.
(2017A&A...599A..71D 2017A&A...599A..71D, Cat. J/A+A/599/A71).
Note (3): Taken from Max-Planck-Institut fuer Astrophysik and Johns Hopkins
University (MPA-JHU) public catalogue Kauffmann et al., 2003MNRAS.341...33K 2003MNRAS.341...33K;
Brinchmann et al., 2004MNRAS.351.1151B 2004MNRAS.351.1151B; Tremonti et al.,
2004ApJ...613..898T 2004ApJ...613..898T; Salim et al., 2007ApJS..173..267S 2007ApJS..173..267S
- E_logmass derived as: 84th percentile - median
- e_logmass derived as: median - 16th percentile
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Acknowledgements:
Salvador Duarte Puertas, salvador-manuel.duarte-puertas.1(at)ulaval.ca
(End) Patricia Vannier [CDS] 10-Oct-2022