J/A+A/559/A114 Updated O3N2 and N2 abundance indicators (Marino+, 2013)
The O3N2 and N2 abundance indicators revisited: improved calibrations based on
CALIFA and Te-based literature data.
Marino R.A., Rosales-Ortega F.F., Sanchez S.F., Gil de Paz A., Vilchez J.,
Miralles-Caballero D., Kehrig C., Perez-Montero E., Stanishev V.,
Iglesias-Paramo J., Diaz A.I., Castillo-Morales A., Kennicutt R.,
Lopez-Sanchez A.R., Galbany L., Garcia-Benito R., Mast D., Mendez-Abreu J.,
Monreal-Ibero A., Husemann B., Walcher C.J., Garcia-Lorenzo B., Masegosa J.,
del Olmo Orozco A., Mourao A.M., Ziegler B., M.Molla, Papaderos P.,
Sanchez-Blazquez P., Gonzalez Delgado R.M., Falcon-Barroso J., Roth M.M.,
van de Ven G., CALIFA team
<Astron. Astrophys. 559, A114 (2013)>
=2013A&A...559A.114M 2013A&A...559A.114M
ADC_Keywords: H II regions ; Spectroscopy ; Abundances
Keywords: Galaxy: abundances - Galaxy: evolution - ISM: abundances -
HII regions - techniques: spectroscopic
Abstract:
The use of integral field spectroscopy is since recently allowing to
measure the emission line fluxes of an increasingly large number of
star-forming galaxies both locally and at high redshift. Many studies
have used these fluxes to derive gas-phase metallicity of the galaxies
by applying the so-called strong-line methods. However, the
metallicity indicators that these datasets use were empirically
calibrated using few direct abundance data points (Te-based
measurements). Furthermore, a precise determination of the prediction
intervals of these indicators is commonly lacking in these
calibrations. Such limitations might lead to systematic errors in
determining the gas-phase metallicity, especially at high redshift,
which might have a strong impact on our understanding of the chemical
evolution of the Universe. The main goal of this study is to review
the most widely used empirical oxygen calibrations, O3N2 and N2, by
using new direct abundance measurements. We pay special attention to
(1) the expected uncertainty of these calibrations as a function of
the index value or abundance derived and (2) the presence of possible
systematic offsets. This is possible thanks to the analysis of the
most ambitious compilation of Te-based Hii regions to date. This new
dataset compiles the Te-based abundances of 603 Hii regions extracted
from the literature but also includes new measurements from the CALIFA
survey.
Description:
We present here the compilation of HII regions from the literature and
from the CALIFA survey where we revisited the O3N2 and N2 abundance
indicators.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 77 16 Dereddened emission line ratios relative to Hβ
fluxes of the CALIFA Te sample along with errors
table3.dat 42 16 Temperatures and oxygen abundances derived for the
CALIFA Te sample using the [OIII]4363 auroral line
table4.dat 48 624 Oxygen, O3N2 and N2 index abundances for
Te-based HII regions abundances (Figs. 2 and 4)
table5.dat 45 3406 Oxygen, O3N2 and N2 index abundances for the
complexes detected within the CALIFA galaxies
(figs. 3 and 5)
table1.dat 72 18 Bibliographic references to the original works
for the compiled Te-sample
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See also:
J/MNRAS/361/1063 : Oxygen abundances of HII regions (Perez-Montero+, 2005)
J/A+A/462/535 : Low-metallicity HII regions and galaxies (Yin+, 2007)
J/ApJ/735/71 : Oxygen abundances in outlying HII regions (Werk+, 2011)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- ID ID for the Te-CALIFA HII regions
19- 22 F4.2 --- 3726 Emission line ratio [OII]3726,29/Hβ (1)
24- 27 F4.2 --- e_3726 Error on [OII]3726,29/Hβ ratio
29- 33 F5.3 --- 4363 Emission line ratio [OIII]4363/Hβ (1)
35- 39 F5.3 --- e_4363 Error on [OIII]4363/Hβ ratio
41- 44 F4.2 --- 5007 Emission line ratio [OIII]5007/Hβ (1)
46- 49 F4.2 --- e_5007 Error on [OIII]5007/Hβ ratio
51- 54 F4.2 --- 6583 Emission line ratio [NII]6583/Hα (1)
56- 59 F4.2 --- e_6583 Error on [NII]6583/Hα ratio
61- 67 F7.2 10-19W/m2 FHb Hβ flux (in 10-16erg/cm2/s)
69- 72 F4.2 10-19W/m2 e_FHb Error on FHb
74- 77 F4.2 mag AV V-bhand extinction obtained from the Balmer
decrement (Hα/Hβ) (2)
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Note (1): The observed lines are dereddened with a Cardelli et al.
(1989ApJ...345..245C 1989ApJ...345..245C) extinction law.
Note (2): with adopting a Milky Way extinction law, A(V)/A(Hβ)=1.164,
Cardelli et al. (1989ApJ...345..245C 1989ApJ...345..245C).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- ID ID for the Te-CALIFA HII regions
19- 22 F4.1 --- S/N [3/17] Signal to noise ratio from [OIII]4363
24- 28 I5 K T3 Temperature derived for the Te-CALIFA HII regions
30- 32 I3 K e_T3 Error on T3
34- 37 F4.2 [-] Ab(O) [7.8/8.5] Oxygen abundance (12+log(O/H)) derived
for the Te-CALIFA HII regions
39- 42 F4.2 [-] e_Ab(O) Error on Ab(O)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number (in table1.dat)
4- 20 A17 --- ID ID for the Te HII region (literature+CALIFA data)
21- 28 F8.5 [-] [O3N2] log[([OIII]5007/Hβ)/([NII]6583/Hα)]
abundance
31- 38 F8.5 [-] [N2] log([NII]6583/Hα) abundance
42- 48 F7.5 --- Ab(O) Oxygen abundance 12+log(O/H) derived for the
Te-HII regions
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- ID ID for the CALIFA-ONS HII regions
18- 25 F8.5 --- [O3N2] log[([OIII]5007/Hβ)/([NII]6583/Hα)]
abundance
28- 35 F8.5 --- [N2] log([NII]6583/Hα) N2 abundance
39- 45 F7.5 --- Ab(O) ?=- Oxygen abundance 12+log(O/H) derived for the
CALIFA-ONS
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 26 A23 --- Aut Author's name
28- 46 A19 --- BibCode BibCode
48- 50 I3 --- nHII Number of HII regions for this reference
52- 72 A21 --- Al Auroral lines for this reference (1)
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Note (1): The corresponding wavelengths of the auroral lines are
[OIII]4363, [NII]5755, [SIII]6312.
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Acknowledgements:
Raffaella Anna Marino, ramarino(at)ucm.es, Universidad Complutense Madrid
(End) Raffaella Marino [UCM-CEI], Patricia Vannier [CDS] 07-Oct-2013