J/A+A/683/A46 ELG luminosity functions in the nearby Universe (Favole+, 2024)
Characterizing the ELG luminosity functions in the nearby Universe.
Favole G., Gonzalez-Perez V., Ascasibar Y., Corcho-Caballero P.,
Montero-Dorta A.D., Benson A.D., Comparat J., Cora S.A., Croton D., Guo H.,
Izquierdo-Villalba D., Knebe A., Orsi A., Stoppacher D., Vega-Martinez C.A.
<Astron. Astrophys. 683, A46 (2024)>
=2024A&A...683A..46F 2024A&A...683A..46F (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Galaxies, photometry ; Photometry, H-alpha ;
Photometry, H-beta
Keywords: galaxies: distances and redshifts -
galaxies: luminosity function, mass function - galaxies: Seyfert -
galaxies: starburst - galaxies: star formation -
galaxies: stellar content
Abstract:
Nebular emission lines are powerful diagnostics for the physical
processes at play in galaxy formation and evolution. Moreover,
emission-line galaxies (ELGs) are one of the main targets of current
and forthcoming spectroscopic cosmological surveys. We investigate the
contributions to the line luminosity functions (LFs) of different
galaxy populations in the local Universe, providing a benchmark for
future surveys of earlier cosmic epochs. The large statistics of the
observations from the SDSS DR7 Main galaxy sample and the MPA-JHU
spectral catalogue enabled us to precisely measure the Hα, Hβ,
[OII], [OIII], and, for the first time, the [NII], and [SII]
emission-line LFs over ∼2.4Gyrs in the low-z Universe, 0.02<z<0.22.
We present a generalized 1/Vmax LF estimator capable of simultaneously
correcting for spectroscopic, r-band magnitude, and emission-line
incompleteness. We studied the contribution to the LF of different
types of ELGs classified using two methods: (i) the value of the
specific star formation rate (sSFR), and (ii) the line ratios on the
Baldwin-Phillips-Terlevich (BPT) and the WHAN (i.e., Hα equivalent
width versus the [NII]/Hα line ratio) diagrams. The ELGs in our
sample are mostly star forming, with 84 per cent having
sSFR>10-11yr-1. When classifying ELGs using the BPT+WHAN diagrams, we
find that 63.3 per cent are star forming, only 0.03 are passively
evolving, and 1.3 have nuclear activity (Seyfert). The rest are
low-ionization narrow emission-line regions (LINERs) and composite
ELGs. We found that a Saunders function is the most appropriate to
describe all of the emission-line LFs, both observed and
dust-extinction-corrected. They are dominated by star-forming regions,
except for the bright end of the [OIII] and [NII] LFs (i.e.
L[NII]>1042erg/s, L[OIII]>1043erg/s), where the contribution of
Seyfert galaxies is not negligible.
Description:
We tabulate the Main ELG luminosity functions, both observed and
intrinsic ones, of the Main ELG sample and its different galaxy
components: star-forming, passive, Seyfert, LINERs, composite.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
com-i.dat 161 19 Intrinsic composite line luminosity functions
com-o.dat 161 19 Observed composite line luminosity functions
full-i.dat 161 19 Intrinsic full line luminosity functions
full-o.dat 161 19 Observed full line luminosity functions
liner-i.dat 161 19 Intrinsic LINERs line luminosity functions
liner-o.dat 161 19 Observed LINERs line luminosity functions
pass-i.dat 161 19 Intrinsic passive line luminosity functions
pass-o.dat 161 19 Observed passive line luminosity functions
seyf-i.dat 161 19 Intrinsic Seyfert line luminosity functions
seyf-o.dat 161 19 Observed Seyfert line luminosity functions
sfbpt-i.dat 161 19 Intrinsic star-forming BPT line luminosity functions
sfbpt-o.dat 161 19 Observed star-forming BPT line luminosity functions
sfssfr-i.dat 161 19 Intrinsic star-forming sSFR line luminosity functions
sfssfr-o.dat 161 19 Observed star-forming sSFR line luminosity functions
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Byte-by-byte Description of file: *-i.dat *-o.dat
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Bytes Format Units Label Explanations
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1- 5 F5.2 [10-7W] logL logarithmic line luminosity
7- 18 E12.6 Mpc-3 LFHa Line Halpha luminosity function (1)
20- 31 E12.6 Mpc-3 LFO2 Line [OII] luminosity function (1)
33- 44 E12.6 Mpc-3 LFO3 Line [OIII] luminosity function (1)
46- 57 E12.6 Mpc-3 LFHb Line Hbeta luminosity function (1)
59- 70 E12.6 Mpc-3 LFN2 Line [NII] luminosity function (1)
72- 83 E12.6 Mpc-3 LFS2 Line [SII] luminosity function (1)
85- 96 E12.6 Mpc-3 e_LFHa rms uncertainty on Halpha luminosity function (1)
98-109 E12.6 Mpc-3 e_LFO2 rms uncertainty on [SII] luminosity function (1)
111-122 E12.6 Mpc-3 e_LFO3 rms uncertainty on [OIII] luminosity function (1)
124-135 E12.6 Mpc-3 e_LFHb rms uncertainty on Hbeta luminosity function (1)
137-148 E12.6 Mpc-3 e_LFN2 rms uncertainty on [NII] luminosity function (1)
150-161 E12.6 Mpc-3 e_LFS2 rms uncertainty on [SII] luminosity function (1)
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Note (1): in Mpc-3.dex-1 unit.
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Acknowledgements:
Ginevra Favole, gfavole(at)iac.es
(End) Patricia Vannier [CDS] 23-Feb-2024