J/A+A/695/A256 Isolated galaxies, pairs, and triplets (Argudo-Fernandez+, 2025)
Fundamental relation in isolated galaxies, pairs, and triplets in the
local universe.
Argudo-Fernandez M., Duarte Puertas S., Verley S.
<Astron. Astrophys. 695, A256 (2025)>
=2025A&A...695A.256A 2025A&A...695A.256A (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxies, spectra ; Abundances
Keywords: galaxies: evolution - galaxies: formation -
galaxies: fundamental parameters - galaxies: general -
galaxies: star formation
Abstract:
The correlations between star formation rate (SFR), stellar mass (M),
and gas-phase metallicity (12+log(O/H)) for star-forming (SF)
galaxies, known as global scaling relations or fundamental relations,
have been studied during the last decades to understand the evolution
of galaxies. However, the origin of these correlations and their
scatter, which may also be related to their morphology or environment,
is still a subject of debate. In this work, we establish fundamental
relations, for the first time, in isolated systems in the local
universe (with 0.005≤z≤0.080), which can give insight into the
underlying physics of star-formation. We use a sample of isolated
galaxies to explore whether star formation is regulated by smooth
secular processes. In addition, galaxies in physically bound isolated
pairs and isolated triplets may also interact with each other, where
interaction itself may enhance/regulate star-formation and the
distribution of gas and metals within galaxies. We compared our
results with a sample of star-forming galaxies in the SDSS. We found
that, on average, at a fixed stellar mass, the SIG SF galaxies have
lower SFR values than Main Sequence (MS) SF galaxies in the SDSS and
central galaxies in the SIP and SIT. On average, SIG galaxies have
higher 12+log(O/H) values than galaxies in the SIP, SIT, and
comparison sample. When distinguishing between central and satellite
galaxies in the SIP and SIT, centrals and SIG galaxies present similar
values (∼8.55) while satellites have values close to M33 (∼8.4). Using
the Dn(4000) parameter as a proxy of the age of the stellar
populations we found that, on average, SIG and central galaxies have
higher Dn(4000) values than satellites and comparison galaxies.
Based on our results for isolated galaxies, we propose a ground level
nurture free SFR-M and 12+log(O/H)-SFR-M relations for SF galaxies in
the local Universe.
Description:
Compiled data for the sample of star-forming galaxies in the SIG, SIP,
and SIT catalogues. We made use of published emission line fluxes
information from the Sloan Digital Sky Survey (SDSS) to identify SF
galaxies in the SDSS-based catalogue of isolated galaxies (SIG),
isolated pairs (SIP), and isolated triplets (SIT) compiled in
Argudo-Fernandez et al. (2015A&A...578A.110A 2015A&A...578A.110A, Cat. J/A+A/578/A110). We
also use these data to derive their aperture-corrected SFR and oxygen
abundance, 12+log(O/H), using bright lines calibrations. Stellar
masses for SIG, SIP, and SIT galaxies were estimated by fitting their
spectral energy distribution on the five SDSS bands.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 93 2950 Compiled data for the sample of star-forming
galaxies in the SIG, SIP, and SIT catalogues
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See also:
J/A+A/578/A110 : Isolated galaxies, pairs & triplets (Argudo-Fernandez+, 2015)
J/A+A/599/A71 : 209276 SDSS star-forming galaxies aperture-free
(Duarte Puertas+, 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 spectroscopic name
21- 25 F5.2 [Msun] logM log10 of the stellar mass (1)
27- 29 F3.1 [Msun] e_logM Uncertainty for log10 of the stellar mass
31- 35 F5.2 [Msun/yr] logSFR log10 of the aperture corrected star
formation rate (2)
37- 40 F4.2 [Msun/yr] e_logSFR Uncertainty for log10 of the aperture
corrected star formation rate
42- 45 F4.2 --- 12+log(O/H) ?=- Oxygen abundance (3)
47- 50 F4.2 --- e_12+log(O/H) ?=- Uncertainties for the
oxygen abundance
52- 55 F4.2 --- Dn(4000) Narrow definition of the 4000Å break
strength in Balogh et al.
1999ApJ...527...54B 1999ApJ...527...54B from the MPA-JHU
catalogue
57- 60 F4.2 --- e_Dn(4000) Uncertainties for the narrow definition
of the 4000Å break strength from the
MPA-JHU catalogue
62- 64 A3 --- Catalogue Indicates if the galaxy is coming from
the SIG, SIP, or SIT catalogues
66- 77 F12.8 deg RAdeg Right ascension (J2000)
79- 93 F15.11 deg DEdeg Declination (J2000)
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Note (1): Stellar masses were estimated using the five SDSS optical bands
(ugriz) with the routine kcorrect (Blanton & Roweis, 2007AJ....133..734B 2007AJ....133..734B)
with a Kroupa (2001MNRAS.322..231K 2001MNRAS.322..231K) universal initial mass function (IMF).
Note (2): SFR derivation using the refined method of Hopkins et al.
(2003ApJ...599..971H 2003ApJ...599..971H), as used in Duarte puertas et al. (2017A&A...599A..71D 2017A&A...599A..71D,
Cat. J/A+A/599/A71), as described in section 3.1.
Note (3): oxygen abundance using the empirical calibration S of Pilyugin &
Grebel (2016MNRAS.457.3678P 2016MNRAS.457.3678P), as described in section 3.2.
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References:
Argudo-Fernandez et al. 2015A&A...578A.110A 2015A&A...578A.110A, Cat. J/A+A/578/A110
Catalogues of isolated galaxies, isolated pairs, and isolated triplets
in the local Universe
Duarte Puertas et al. 2017A&A...599A..71D 2017A&A...599A..71D, Cat. J/A+A/599/A71
Aperture-free star formation rate of SDSS star-forming galaxies
Acknowledgements:
Maria del Carmen Argudo-Fernandez, margudo(at)ugr.es
(End) Patricia Vannier [CDS] 26-Feb-2025