J/MNRAS/456/4407 Star forming regions sulphur ICFs (Dors+, 2016)
Sulphur abundance determinations in star-forming regions.
I. Ionization correction factor.
Dors O.L., Perez-Montero E., Hagele G.F., Cardaci M.V., Krabbe A.C.
<Mon. Not. R. Astron. Soc., 456, 4407-4424 (2016)>
=2016MNRAS.456.4407D 2016MNRAS.456.4407D (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Abundances
Keywords: galaxies: abundances - galaxies: evolution - galaxies: formation -
galaxies: general - galaxies: ISM
Abstract:
In this work, we used a grid of photoionization models combined with
stellar population synthesis models to derive reliable ionization
correction factors (ICFs) for the sulphur in star-forming regions.
These models cover a large range of nebular parameters and yielding
ionic abundances in consonance with those derived through optical and
infrared observational data of star-forming regions. From our
theoretical ICFs, we suggested an α value of 3.27±0.01 in the
classical Stasinska formulae. We compared the total sulphur
abundance in the gas phase of a large sample of objects by using our
theoretical ICF and other approaches. In average, the differences
between the determinations via the use of the different ICFs
considered are similar to the uncertainties in the S/H estimations.
Nevertheless, we noted that for some objects it could reach up to
about 0.3dex for the low-metallicity regime. Despite of the large
scatter of the points, we found a trend of S/O ratio to decrease with
the metallicity, independently of the ICF used to compute the sulphur
total abundance.
Description:
We compiled from the literature emission-line intensities of HII
regions and star-forming galaxies obtained in the optical and infrared
spectral ranges. These measurements were used to obtain sulphur and
oxygen ionic abundances in order to verify if our photoionization
models are representative of real HIi regions, to check if the
theoretical ICFs are compatible with the ones derived directly from
observations and investigating the S/O-O/H relation.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 74 118 Dereddened line fluxes (relative to
Hβ=100.0) compiled from the literature
tablea2.dat 60 103 Fluxes of infrared emission lines (in W/cm2)
compiled from the literature
tablea3.dat 53 118 Electron temperature, electron density, ionic
and total oxygen abundances for the sample of
objects listed in Table A1
tablea4.dat 37 96 *Ionic abundances for the sample of objects
obtained listed in Table A2
refs.dat 104 28 References
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Note on tablea4.dat: calculated following the IR-lines method described in
Section 4.2 and assuming an electron temperature of 10000K.
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Object Object name
22- 27 F6.2 --- [OII]3727 ?=- Sum on [OII]λλ3726+3729
dereddened line flux
(relative to Hβ=100.0)
29- 33 F5.2 --- [OIII]4363 ?=- [OIII]λ4363 dereddened line flux
(relative to Hβ=100.0)
36- 41 F6.2 --- [OIII]5007 ?=- [OIII]λ5007 dereddened line flux
(relative to Hβ=100.0)
44- 48 F5.2 --- [SII]6717 ?=- [SII]λ6717 dereddened line flux
(relative to Hβ=100.0)
52- 56 F5.2 --- [SII]6731 ?=- [SII]λ6731 dereddened line flux
(relative to Hβ=100.0)
59- 63 F5.2 --- [SII]6725 ?=- Sum of the dereddened emission-line
intensities [SII]λ6717+6731
(relative to Hβ=100.0)
66- 70 F5.2 --- [SIII]9069 ?=- [SIII]λ9069 dereddened line flux
(relative to Hβ=100.0)
71 A1 --- n_[SIII]9069 [a] Note on [SIII]9069 (1)
73- 74 I2 --- Ref Fluxes reference, in refs.dat file
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Note (1): Note as follows:
a = Value computed from I([SIII]λ9069=0.4*I([SIII]λ9532)
b = Sum of the emission-line intensities [Sii]λλ6717, 6731
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 25 A25 --- Object Object name
26 A1 --- n_Object Note on Object (1)
27- 33 F7.3 W/cm2 FHI Flux of HI 4.05um emission line
34 A1 --- Note [ab] Note (1)
36- 43 F8.3 W/cm2 F[SIV] Flux of [SIV] 10.51um emission line
45- 51 F7.2 W/cm2 F[SIII] Flux of [SIII]18.71um
53- 57 A5 W/cm2 Flux Flux
59- 60 I2 --- Ref Reference, in refs.dat file
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Note (1): Notes as follows:
a = Flux computed from HI4.051um/HI2.63um = 1.74
b = Flux computed from HI4.051um/HI12.37um = 8.2
c = Flux obtained assuming the measurements at the different observed positions
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Object Object name
22- 27 F6.4 10+4K Te Electron temperature
30- 33 I4 cm-3 Ne ?=- Electron density (1)
35- 38 F4.2 [-] log(O+/H+) Ionic oxygen abundance
40- 43 F4.2 [-] 12+log(O/H) Total oxygen abundances
45- 48 F4.2 [-] log(S+/H+) Ionic S abundance
50- 53 F4.2 [-] log(S+2/H+) Ionic S abundance
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Note (1): The estimations were calculated following the Visible-lines method
described in Section 4.1. For the cases where was not possible to calculate
the electron density, a value of Ne=200cm-3 was assumed.
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 25 A25 --- Object Object name
29- 32 F4.2 [-] 12+log(S2+/H+) Ionic abundance S2+/H+
34- 37 F4.2 [-] 12+log(S3+/H+) Ionic abundance S3+/H+
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference code
4- 22 A19 --- BibCode BibCode
24- 48 A25 --- Aut Author's name
50-104 A55 --- Com Comments
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 07-Oct-2016