J/A+A/464/885 Abundances in 53 HII regions (Guseva+, 2007)
Balmer jump temperature determination in a large sample of low-metallicity
H II regions.
Guseva N.G., Izotov Y.I., Papaderos P., Fricke K.J.
<Astron. Astrophys. 464, 885 (2007)>
=2007A&A...464..885G 2007A&A...464..885G
ADC_Keywords: H II regions ; Abundances
Keywords: galaxies: irregular - galaxies: starburst - galaxies: ISM -
galaxies: abundances
Abstract:
Continuing the systematic determination of the electron temperature of
HII regions using the Balmer and/or Paschen discontinuities by Guseva
et al. (2006ApJ...644..890G 2006ApJ...644..890G) we focus here on 3.6m ESO telescope
observations of a large new sample of 69 HII regions in 45 blue
compact dwarf (BCD) galaxies. This data set spans a wide range in
metallicity (Z☉/60<Z<Z☉/3) and, combined with the sample
of 47 HII regions from Guseva et al. (2006ApJ...644..890G 2006ApJ...644..890G), yields the
largest spectroscopic data set ever used to derive the electron
temperature in the H+ zone. In the same way as in Guseva et al.
(2006ApJ...644..890G 2006ApJ...644..890G) we have used a Monte Carlo technique to vary
free parameters and to calculate a series of model spectral energy
distributions (SEDs) for each HII region. The electron temperature in
the H+ zones was derived from the best fitting synthetic and observed
SEDs in the wavelength range ∼3200-5100Å, which includes the Balmer
jump. On the base of the present large spectroscopic sample we find
that in hot (Te(H+)>11000K) HII regions the temperature of the O2+
zone, determined from doubly ionised oxygen forbidden lines, does not
differ statistically from the temperature of the H+ zone. Thus, we
confirm and strengthen the finding by Guseva et al.
(2006ApJ...644..890G 2006ApJ...644..890G). We emphasize that due to a number of modelling
assumptions and the observational uncertainties for individual
objects, only a large, homogeneous sample, as the one used here, can
enable a conclusive study of the relation between Te(H+) and Te(OIII).
Description:
Table 3 contains observed and corrected emission line fluxes and
equivalent widths in 53 HII regions.
Table 4 contains electron temperatures, ionic and total element
abundances of 53 HII regions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3a.dat 39 53 Extinction coefficient, observed Hβ flux
and equivalent width of hydrogen absorption
lines in 53 HII regions
table3b.dat 74 1696 Observed and corrected fluxes and equivalent
widths of the emission lines in 53 HII regions
table4.dat 201 53 Electron temperatures, ionic and total element
abundances in 53 HII regions
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See also:
VII/20 : Catalogue of HII Regions (Sharpless 1959)
J/A+A/416/475 : Long slit spectroscopy of HII regions (Marquez+, 2004)
J/A+A/416/515 : Long slit spectroscopy of HII regions (Marquez+, 2004)
J/A+AS/131/319 : HII regions catalogue (Petit+ 1998)
Byte-by-byte Description of file: table3a.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Name Source name
22- 26 F5.3 --- CHb Extinction coefficient
28- 34 F7.2 10-17W/s/m2 FHbeta Observed Hbeta flux (10-14erg/cm2/s)
36- 39 F4.2 0.1nm EWabs Equivalent width of hydrogen absorption lines
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Byte-by-byte Description of file: table3b.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Name Source name
22- 25 I4 0.1nm lambda Non-redshifted wavelength
27- 41 A15 --- Ion Emission-line identification
42- 48 F7.2 % Flux Observed emission-line flux relative to Hbeta (1)
49- 54 F6.2 % e_Flux 1σ relative flux error (1)
55- 61 F7.2 % Fluxc Corrected emission-line flux relative to Hbeta (1)
62- 67 F6.2 % e_Fluxc 1σ relative flux error (1)
68- 74 F7.1 0.1nm EW Equivalent width of the emission line
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Note (1): Multiplied by 100.
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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- 20 A20 --- Name Source name
22- 26 I5 K TOIII Electron temperature Te(OIII)
28- 31 I4 K e_TOIII Error of the electron temperature
33- 37 I5 K TOII Electron temperature Te(OII)
39- 42 I4 K e_TOII Error of the electron temperature
44- 48 I5 K TSIII Electron temperature Te(SIII)
50- 53 I4 K e_TSIII Error of the electron temperature
55- 59 F5.3 10-4 O+/H+ Abundance O+/H+ (multiplied by 104)
61- 65 F5.3 10-4 e_O+/H+ Error of O+/H+ (multiplied by 104)
67- 71 F5.3 10-4 O2+/H+ Abundance O++/H+ (multiplied by 104)
73- 77 F5.3 10-4 e_O2+/H+ Error of O++/H+ (multiplied by 104)
79- 83 F5.3 10-6 O3+/H+ Abundance O+++/H+ (multiplied by 106)
85- 89 F5.3 10-6 e_O3+/H+ Error of O+++/H+ (multiplied by 106)
91- 95 F5.3 10-4 O/H Abundance O/H (multiplied by 104)
97-101 F5.3 10-4 e_O/H Error of O/H (multiplied by 104)
103-107 F5.3 --- 12O/H Abundance 12+logO/H (in dex)
109-113 F5.3 --- e_12O/H Error of 12+logO/H (in dex)
115-119 F5.3 10-5 Ne2+/H+ Abundance Ne++/H+ (multiplied by 105)
121-125 F5.3 10-5 e_Ne2+/H+ Error of Ne++/H+ (multiplied by 105)
127-131 F5.3 --- ICFNe Ionization correction factor ICF(Ne)
133-138 F6.3 --- logNe/O Logarithm of Ne/O abundance ratio (in dex)
140-144 F5.3 --- e_logNe/O Error of logNe/O (in dex)
146-150 F5.3 10-6 Fe2+/H+1 Abundance Fe++/H+ from the line 4658A (1)
152-156 F5.3 10-6 e_Fe2+/H+1 Error of Fe++/H+ from the line 4658A (1)
158-162 F5.3 10-6 Fe2+/H+2 Abundance Fe++/H+ from the line 4988A (1)
164-168 F5.3 10-6 e_Fe2+/H+2 Error of Fe++/H+ from the line 4988A (1)
170-175 F6.3 --- ICFFe Ionization correction factor ICF(Fe)
177-182 F6.3 --- logFe/O1 Logarithm of Fe/O abundance ratio
from 4658Å line (in dex)
184-188 F5.3 --- e_logFe/O1 Error of logFe/O from the 4658A line (in dex)
190-195 F6.3 --- logFe/O2 Logarithm of Fe/O abundance ratio
from 4988Å line (in dex)
197-201 F5.3 --- e_logFe/O2 Error of logFe/O from the 4988A line (in dex)
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Note (1): Multiplied by 106.
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Acknowledgements:
Natalia Guseva, guseva(at)mao.kiev.ua
(End) Natalia Guseva [MAO, Ukraine], Patricia Vannier [CDS] 08-Jan-2007