A&A 457, 477-484 (2006)
DOI: 10.1051/0004-6361:20054488
C. Kehrig1,2 - J. M. Vílchez1 - E. Telles2 - F. Cuisinier3 - E. Pérez-Montero4
1 - Instituto de Astrofísica de Andalucía (CSIC),
Apartado 3004, 18080 Granada, Spain
2 -
Observatório Nacional,
Rua José Cristino 77, 20.921-400 Rio de Janeiro - RJ, Brazil
3 -
GEMAC, Observatório do Valongo/UFRJ,
Ladeira do Pedro Antônio 43, 20.080-090 Rio de Janeiro - RJ, Brazil
4 -
Departamento de Física Teórica, C-XI, Universidad Autónoma de Madrid, 28049 Madrid, Spain
Received 7 November 2005 / Accepted 6 June 2006
Abstract
Aims. A detailed spectroscopic study covering the blue to near-infrared wavelength range (3700 Å-1
m) was performed for a sample of 34 HII galaxies in order to derive fundamental parameters for their HII regions and ionizing sources, as well as gaseous metal abundances. All the spectra included the nebular [SIII]
9069,9532 Å lines, given their importance in the derivation of the S/H abundance and relevant ionization diagnostics.
Methods. A systematic method was followed to correct the near-IR [SIII] line fluxes for the effects of the atmospheric transmission. A comparative analysis of the predictions of the empirical abundance indicators R23 and S23 was performed for our sample galaxies. The relative hardness of their ionizing sources was studied using the parameter and exploring the role played by metallicity.
Results. For 22 galaxies of the sample, a value of the electron temperature [SIII] was derived, along with their ionic and total S/H abundances. Their ionic and total O/H abundances were derived using direct determinations of
[OIII]. For the rest of the objects, the total S/H abundance was derived using the S23 calibration. The abundance range covered by our sample goes from 1/20 solar up to solar metallicity. Six galaxies present 12+log (O/H) < 7.8 dex. The mean S/O ratio derived in this work is log (S/O) = -1.68
0.20 dex, 1
below the solar (S/O)
value. The S/O abundance ratio shows no significant trend with O/H over the range of abundance covered in this work, in agreement with previous findings. There is a trend for HII galaxies with lower gaseous metallicity to present harder ionizing spectra. We compared the distribution of the ionic ratios O+/O++ vs. S+/S++ derived for our sample with the predictions of a grid of photoionization models performed for three different stellar effective temperatures. This analysis indicates that a large fraction of galaxies in our sample seem to be ionized by extremely hard spectra, in line with recent suggestions for extra ionizing sources in HII galaxies.
Key words: ISM: abundances - HII regions - galaxies: abundances - galaxies: dwarf - galaxies: evolution
HII galaxies are galaxies undergoing violent star
formation (Searle & Sargent 1972; Terlevich et al. 1991; Cairós
et al. 2000). Their optical spectra show strong emission lines
(recombination lines of hydrogen and helium, as well as forbidden
lines of elements like oxygen, neon, nitrogen, sulfur, among
others) that are very similar to the spectra of extragalactic HII regions. Analysis of their spectra shows that they are
low-metallicity objects with the metallicity varying from 1/40
to 1/2
(e.g. Terlevich et al. 1991; Telles 1995 and references therein; Vílchez &
Iglesias-Páramo 1998, 2003; Thuan & Izotov 2005). Among them we can find the least chemically-evolved galaxies in the local Universe.
The study of elemental abundances in emission-line galaxies gives information about their chemical evolution and star formation history. Outside the Local Group, emission lines from ionized gas represent the principal means of deriving abundances, as energy is concentrated in a few conspicuous emission lines. Abundances for the stellar population are derived from absorption features, which are more numerous and require much higher signal-to-noise spectra to be derived meaningfully.
In HII galaxies the metal enrichment of the interstellar medium by supernovae has been operating typically in low-metallicity environments. Oxygen is the most frequently used element in deriving abundances from emission lines: abundances are easily derived, as the main ionization stages are observable in the optical range. Furthermore, oxygen is particularly suitable for chemical evolution studies, as it traces the overall metallicity very well. It originates quasi exclusively from the nucleosynthesis in type II supernovae progenitors (Meynet & Maeder 2002; Pagel 1997; Woosley & Weaver 1995). While the sources of oxygen are well-determined and the most important ionization stages can be observed in the optical range, some uncertainties still remain about the sulfur yields and its sources. In addition, not all the ionization stages can be observed in the optical range and important ionization correction factors (ICFs) must be applied to derive the total sulfur abundance. Hence comparing S and O abundances can give us some clues to sulfur nucleosynthesis and the masses of the stars where the sulfur tends to be formed.
To derive oxygen abundances, one should first derive the
electron temperature, which requires the measurement of faint
auroral lines, like [OIII]4363 Å, which are often not
detected. The alternative is to use strong line-abundance
indicators, like R23
, which calibrated
empirically (Pagel et al. 1979; Pilyugin 2001) or through
photoionization models (e.g. McGaugh 1991). However, the relation
between R23 and oxygen abundance presents the noticeable
drawback of being double-valued.
Vílchez & Esteban (1996) proposed S23 as an alternative abundance indicator. In contrast to oxygen, S23 remains single-valued up to abundances above solar
value. Furthermore, sulfur should be as useful as oxygen for tracing
metallicity. From an observational point of view, S23 has the
advantage over R23 that the [SII] and [SIII] lines are less
affected by reddening (Pérez-Montero et al. 2006; hereinafter PM06).
To produce an accurate derivation of S/H abundance, the importance of using the nebular [SIII] lines can not
be overlooked (e.g. Dennefeld & Stasinska 1983; Vílchez et al. 1988; Garnett 1989; Bresolin et al. 2004). Photoionization models
indicate that S++ is the dominant sulfur ion (Garnett 1989; hereinafter G89), which
presents three forbidden transitions at [SIII]9069,9532
and
6312
in the optical to near-IR (NIR) range (analogs
to [OIII]
4959,5007
and
4363
). The [SIII]
6312
line is
faint, highly temperature-sensitive, and it can induce several biases in
the derived S/H abundance. The NIR [SIII] lines can be quite
strong, and a detailed telluric atmosphere correction has to be
applied to them. Pérez-Montero & Díaz
(2003) (hereinafter PMD03) and G89 derive the S++ ionic
abundance for samples of about one dozen emission-line galaxies,
both using the nebular [SIII]
9069
line. Recent work
by Izotov et al. (2006) (hereinafter I05) presents S/H abundances
for a large number of metal-poor emission-line galaxies from the
SDSS-DR3
;
however, the auroral line [SIII]
6312
was used in this work to calculate the S++ ionic abundance.
Here we present long-slit spectrophotometric
observations of a sample of 34 HII galaxies to make a detailed analysis of their chemical abundances. The wide coverage
of our spectra (3700 Å-1
m) for all the galaxies
in the sample provides us all the emission lines needed to
estimate the oxygen and sulfur abundances directly. All the S/H abundances were estimated using a nebular [SIII] line, so that uncertainties related to the use of the auroral line
[SIII]
6312 Å are avoided. In addition, this wavelength
coverage allowed us to study the properties of the ionizing
clusters of HII galaxies making use of the
parameter and
sequences of photoionization models.
In the next section we describe our sample of galaxies, the observations, and data reduction and present the line intensities. In Sect. 3 we perform a comparative study between R23 and S23 abundance indicators, present an analysis about ionization structure and ionizing sources, and discuss the abundance results for the sample. Finally in Sect. 4 we summarize our conclusions.
The data base of this work consists of 34 intermediate-resolution
spectra of HII galaxies covering a wavelength range from
3700 Å to 7000 Å (blue spectra; Kehrig et al. 2004), and from
6500 Å to 1 m (red spectra). For all the objects,
measurements of the emission lines of [OII]
3727 Å and
[SIII]
9069,9532 Å exist, except for the galaxy UM151, for which we do not have a measurement of the [OII]
3727 Å line.
The complete log and the characteristics of the sample objects are
given in Kehrig et al. (2004). The mean value for the distribution
of redshifts of the sample is 0.02. Depending on the redshift of
each galaxy, one of the two [SIII] lines (9069 Å or
9532 Å)
may fall in the range of telluric absorption in which
atmospheric correction is critical. For this reason, this
correction must be performed on a case by case basis.
Regarding the red spectra, the observations were conducted in
October and December 2002 (9 nights of observations in total) with
the Boller & Chivens spectrograph of the 1.52 m
telescope at the European Southern Observatory (ESO), La Silla,
Chile. The CCD used has a pixel size of 0.82 arcsec in spatial
direction. Typical seeing of the observations was 1-1.2''. All
observations were performed using grating #10 with an inverse
dispersion of 1.9 Å/pix, a slit width of 2.5'', and a spectral
range of 6000 Å-1
m. This configuration yielded an effective
instrumental resolution of
6 Å (FWHM) at 6000 Å. Total exposure times were typically 7200 s split into two exposures in order to eliminate cosmic rays during the
reduction procedure.
![]() |
Figure 1: Representative red spectra of galaxies of the sample. |
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Representative red spectra of three of the observed galaxies are shown in Fig. 1.
The CCD frames were reduced by employing standard IRAF
packages. The spectrophotometric standard stars (
7 observed
each night) used for flux calibration were chosen in order to have
an appropriate flux-point coverage in the NIR.
Ground-based NIR spectroscopy has always been hampered by strong and
variable absorption features due to the Earth's atmosphere. Even
within the well-established photometric bands such as J, H, and K,
telluric absorption bands are present. In analysis of the NIR sulfur
emission lines, a crucial step is the correction for the effects
produced by the earth's atmosphere on the spectra, especially between
8500 Å and 1 m (Vacca et al. 2003; Díaz et al. 1987). Exhaustive work was done to correct the whole sample for
these effects. We derived, for each night, the telluric correction as
a function of wavelength,
,
and its corresponding
standard deviation,
.
A minimum of five standard stars per night was used to obtain this correction. The mean
values for
and
are
80
and 4
,
respectively. We applied the telluric correction by
dividing each galaxy spectrum by its corresponding
.
The
of the
correction was taken into account when calculating the overall error
budget of the line fluxes.
The emission lines corresponding to the red spectra were measured following the same procedure as in Kehrig et al. (2004). Once the atmospheric correction was performed for each spectrum, we estimated the final error for each line flux by means of independent, repeated measurements.
We measured, for each galaxy, the main emission lines
from the blue to the near-IR: [OII]3727; [OIII]
4363; H
;
[OIII]
4959,5007; H
;
[NII]
6548,84;
[SII]
6717,31;
[SIII]
6312,9069,9532; [ArIII]
7136;
[OII]
7320,30; Pa9 and Pa8, among others. The other Hydrogen
Paschen lines series, from Pa13 to Pa8, were detected in some galaxies
of our sample. Reddening-corrected line intensity ratios (applying Whitford's 1958 extinction law) normalized to
H
= 100 are presented in Table 1, together with the
values of the reddening coefficient, C(H
), estimated using the H
/H
ratio from our blue spectra (Osterbrock 1989). Column (1) lists the
common names of the galaxies and, in those cases where the apertures
were centered on a secondary knot, there is an indication between
brackets for the position of the aperture (see Kehrig et al. 2004 for details).
As is well known, IIZw40 presents high extinction (Baldwin et al. 1982). For this galaxy
we measured the Paschen series from Pa17 to Pa8, thereby allowing a direct derivation of the reddening coefficient from its red spectrum.
In Fig. 2, we illustrate for this galaxy the observed ratio of the fluxes of
each Paschen line to H
,
relative to its theoretical ratio for
case B recombination (Storey & Hummer 1995),
[F(P
)/F(H
)]
/[F(P
)/F(H
)]
,
vs. the reddening function relative to H
,
f(H
) - f(P
).
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Figure 2:
The ratio between observed and theoretical Paschen to H![]() ![]() ![]() ![]() ![]() |
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In order to check the reliability of the reduction process, we carried
out two tests. Firstly, when the quality of the measurements allowed,
we compared the four brightest Paschen lines, normalized to H,
with the corresponding predictions for case B recombination (Storey &
Hummer 1995). The corrected
/H
values are found
to be consistent with the theoretical values, within the errors. In
the case of Pa8, we notice that the ratios are slightly above the
theoretical value. This is mainly due to the fact that the Pa8 and
[SIII]
9532 Å lines are blended, making the Pa8 flux suffer
from some contamination by the [SIII] line. In the second test we
compared the ratio of the two near-IR [SIII] lines,
Q[SIII] = [SIII]
9532/
9069 Å, with the theoretical
ratio of 2.44 (Mendoza & Zeippen 1982). The values of Q[SIII] are
consistent with the theoretical ratio to within the errors, although
many galaxies show Q[SIII] values slightly below the theoretical
ratio. This effect could be due to two factors: (a) the telluric
absorption features were not totally removed and/or (b) the
[SIII]
9532 Å line flux could be blended with the Pa8 line.
These two tests lead us to conclude that the correction for atmospheric absorption, though not perfect, has provided generaly satisfactory results for the purposes of this study.
Commonly used strong line empirical abundance indicators are R23(Pagel et al. 1979; Edmunds & Pagel 1984; McCall et al. 1985;
McGaugh 1991) and S23(4) (Vílchez & Esteban 1996; Díaz
& Pérez-Montero 2000; Oey & Shields 2000; PM06). Though widely
used, R23 presents the drawback of having a double-valued
relation with oxygen abundance, creating an intrinsic uncertainty on
the derived O/H abundances. The turnover region of the relation
R23 vs. O/H takes place for log R23
0.9,
corresponding to 8.0
12 + log (O/H)
8.4. In this
region, R23 is sensitive to ionization conditions but almost
insensitive to O/H. Most of the HII galaxies from our sample show
R23 values within this ill- defined region, which is what we want to explore.
The S23 parameter introduced by Vílchez & Esteban (1996)
has been used as an O/H abundance calibrator in Díaz &
Pérez-Montero (2000) and Pérez-Montero & Díaz 2005
(hereinafter PMD05). It has also been demonstrated that S23 is an efficient S/H abundance calibrator in PM06. It presents several advantages over R23. First, it has a lower dependence on the ionization parameter and remains single-valued up to metallicities
higher than solar, 12 + log (O/H) = 8.69 and 12 + log (S/H)
= 7.19 (Lodders 2003). Secondly, the sulfur emission
lines are less affected by reddening. However, the spectral regions
around the red [SIII] lines are affected by atmospheric absorption.
The N2 parameter has
also been proposed as an abundance indicator (Denicoló et al. 2002;
Van Zee et al. 1998). This parameter offers several advantages, because it
involves easily measurable lines that are available for a wide
redshift range (up to z
2.5). The N2 vs. O/H relation seems
monotonic and the [NII]/H
ratio does not depend on reddening
correction or flux calibration. The drawbacks are that the [NII] lines
can be affected by other excitation sources (see Van Zee et al. 1998). In addition, N2 is sensitive to ionization conditions and relative N/O abundance variations.
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Figure 3:
The left panel presents the relation between S23 and R23; the middle and right panels show the relations between log (1.3 x[NII]6584/H![]() |
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Figure 3a shows the relation between
S23 and
R23
for the
galaxies of our sample. Although log R23 values remain
approximately constant for most galaxies, log S23 values present
a variation of approximately 0.8 dex. We can see that for galaxies in
the turn-over region of the relation between R23 and O/H,
R23 does not correlate with S23. This fact is easily
understood since the relationship between S23 and O/H is not
bivaluate in the metallicity range that we are interested in. Besides,
Figs. 3b and c show that R23 does not correlate
with [NII]/H
,
contrary to the behavior of S23. Therefore, for objects located in the ill-defined region of R23 vs. O/H, S23 can be used to derive chemical abundances,
especially the S/H abundance.
In photoionized regions like the ones we consider here, the physical properties that determine line intensities are the luminosities and temperatures of the ionizing stars, the gas density, the optical thickness to the ionizing photons, and the chemical abundances. Because S23 is a combination of strong line intensities, it can be affected by several effects. Taking S23 as an abundance indicator, we are not considering, to first order, the detailed effects produced by changes in the physical properties mentioned above. For this reason, it is important to check the sensitivity of S23 to some of these properties.
The optical thickness to ionizing photons is the first to assess. As
can be seen in Fig. 4a, [NII]/H
and
[SII]/H
present a strong correlation, discarding density
boundary effects for the sample galaxies (see e.g. McCall et al. 1985); this correlation implies a statistically significant
relation between N+/N and S+/S, as expected from standard
HII region models.
Ratios of line intensities of elements in different ionization stages, such as [OIII]/[OII] or [SIII]/[SII], are sensitive to combinations of the luminosity, the gas density and geometry, and the radiation hardness; but they are insensitive to abundances at first order, as they originate in the same element. Any variation with respect to such line ratios indicates a sensitivity to these physical parameters, though in a combination that might not be straightforward to derive.
![]() |
Figure 4:
The left panel shows the relation of log ([SII]6717,31/H![]() ![]() |
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Figure 4b shows the dependence of S23 on
[SIII]/[SII]. While
[NII]/H
shows a well-known dependence on the excitation degree
(e.g. McCall et al. 1985), the dependence is much weaker for S23,
being mostly marginal. Despite the fact that S23 possesses a narrower
dynamical range than [NII]/H
,
we consider it a better
abundance indicator for our sample than [NII]/H
,
since S23 does not show any strong dependence on the ionization conditions.
Having a wide wavelength coverage has allowed us to
study the properties of the ionizing sources in our sample of HII galaxies.
This study could help to constrain the range of applicability of photoionization models
and stellar atmospheres in order to fit the observations, thus improving
our understanding of the mechanisms that heat the HII regions
in HII galaxies (Stasinska & Schaerer 1999; Thuan & Izotov 2005).
A convenient hardness index is the parameter
introduced by Vílchez &
Pagel (1988):
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Figure 5:
The left panel shows the relation log ![]() ![]() ![]() |
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In Fig. 5b we present the relationship between the ionic
ratios S+/S++ and O+/O++ for the subset of HII galaxies with electron temperature. In this figure we show the loci of
the average predictions of three sequences of single-star
photoionization models (computed with the photoionization code Cloudy 96; Ferland 2002), performed using CoStar model atmospheres
(Schaerer & de Koter 1997)
= 50 kK, 40 kK and 30 kK. Along each line, the
metallicities vary between
/20 and
/2, and the
ionization parameter changes from log U = -2 to log U = -3 (a detailed
description of the grids of the photo-ionization models used in this work
can be found in PMD05). According to these models, a large fraction of
the galaxies appear to harbor ionizing sources with spectra harder
than the spectrum produced by a 50 kK effective temperature CoStar
atmosphere (Schaerer & de Koter 1997). Kennicutt et al. (2000) have
found, for a sample of HII regions (in the Galaxy and Magellanic
Cloud), that empirically-based stellar-temperature indices present a decrease in mean stellar temperature with increasing abundance. They
show, however, that the typical
for their HII regions are below
55 kK (at
/5), in agreement with the model-based
results by Bresolin et al. (1999). Though any calibration of nebular
empirical parameters in terms of
should be a function of the
atmosphere and photoionization models used, it seems that
55 kK represents a reasonable upper limit for the
effective temperature in HII regions in contrast to HII galaxies.
These findings suggest the existence of very hard spectral energy
distributions as ionizing sources in some HII galaxies. Stasinska & Schaerer (1999), modelling the HII regions in IZw18, argue that extra heating sources might well exist, in
addition to ionizing clusters, giving rise to large temperature
variations and enhancing the [OIII]
4363 emission. I05 have
also invoked extra heating sources (i.e. X-ray ionizing sources) to explain
the high-ionization emission lines observed in some metal-poor
emission-line galaxies. More observations, covering a wide range in
wavelength, as well as dedicated work using photoionization models for
evolving starbursts with a library of different ionizing spectra, are needed
to further investigate the above suggestions.
The physical properties and chemical abundances of the ionized gas were calculated for these galaxies following the 5-level atom FIVEL program (Shaw & Dufour 1994) available in the task IONIC of the STSDAS package. The final quoted errors in the derived quantities were calculated by error propagation including errors in flux measurements, atmospheric corrections, and temperatures. For the [SIII] lines we adopted the most recent atomic coefficients (Tayal & Gupta 1999).
Electron densities were obtained from the
[SII]6717/
6731 Å line ratio. We could derive the
electron temperature values of
[SIII],
[OIII],
[OII], and
[SII] by combining the data from our blue
(Kehrig et al. 2004) and red spectra. Using the
[OIII]
4363 Å/
4959,5007 Å line ratio, we
derived the
[OIII] for 21 galaxies of the sample. The
[SIII] was calculated from the
[SIII]
6312/
9069,9532 Å line ratio for 14 galaxies with a measurement of the [SIII]
6312 Å line. For the 8 galaxies without any measurement of the
[SIII]
6312 Å line and with
[OIII], a theoretical
relation between [OIII] and [SIII] electron temperatures (PMD05) was used:
Regarding [SII] temperatures, for those objects without the [SII] auroral line at 4068 Å we took the approximation
[SII]
[OII] as valid. We could derive
[OII] using the [OII]
3727/7325 Å line
ratio for 16 objects of the sample. For the rest of the objects not
presenting any auroral line in the low excitation zone, we used the
model-predicted relations between
[OII] and
[OIII] found
in PMD03, which explicitly take the dependence of
[OII] on
electron density into account. In most cases the agreement between our
line-intensity measurements in the blue and in the red spectra is
good; we thus have adopted the values with the smaller observational
errors to derive line temperatures. Otherwise, for
[SIII] and
[SII], we used the line intensities corresponding to the red spectra.
The relationship between both temperatures, [OIII] and
[SIII], is shown in Fig. 6 for all our galaxies with
electron temperature and the sample of HII galaxies and HII regions compiled in PMD03, together with photoionization model relations. We note that there are two behaviors. While most HII regions show lower
[SIII] values than the ones provided by the
photoionization models relations, many HII galaxies present higher
[SIII] values than the ones predicted by the models. The same trend can be
noticed for the sample of metal-poor emission-line galaxies in I05 (their Fig. 4),
for a range of
[OIII] from 1
104 K to
2.0
104 K. This fact suggests that HII regions and HII galaxies probably present different spatial temperature structures.
In order to compute the total sulfur abundances, we need to
evaluate the corresponding ICF. A detailed study of the ICF scheme for
sulfur is described in PM06. According to this work, for the objects with log ([SIII]/[SII])
0.4, we made use of the formula of Barker with
= 2.5
(Barker 1980). For the rest of the objects in the sample, we used
the predictions of photoionization models for CoStar atmospheres (see
Fig. 3 in PM06). These predictions indicate rather low values of the ICF, independent of the ionizing effective temperature of the models.
With regard to the oxygen ICF, a small fraction of O/H is expected to
be in the form of O3+ ion in the high-excitation HII regions when
the HeII4686 emission line is detected. We have a measurement
of the HeII
4686 emission line in 6 galaxies of our
sample. According to the photoionization models from Stasinska &
Izotov (2003), the O3+/O can be on the order of 1
only in the
highest-excitation HII regions [O+/(O+ + O2+)
0.1]; therefore, taking our abundance results into account, we assumed
that this correction is negligible in our sample.
![]() |
Figure 6:
A comparison between the measured line temperatures of [OIII] and [SIII]. The electron temperatures, ![]() ![]() |
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Table 2: Physical properties and chemical abundances for the galaxies with S/H and O/H derived directly.
Physical conditions, chemical abundances, and ICFs of sulfur for the
galaxies with a measurement of the [SIII] are quoted in
Table 2. From this table we can see that there are six galaxies with 12 + log (O/H) varying between 7.4 and 7.8. These objects are among the galaxies with very low metallicity. For the objects without
[SIII], we used the strong line calibration of the total
S/H abundance as a function of S23, presented by PM06, to derive
the total S/H abundance.
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Figure 7:
The distribution of total sulfur abundance for our
sample of galaxies. The dashed and empty histograms show the number of galaxies
with S/H derived from ![]() |
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![]() |
Figure 8:
The observed sulfur-to-oxygen abundance ratio for the subset of
galaxies of the sample with ![]() ![]() |
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The only galaxy of our sample for which we can compare the S/H abundance derived in this work with previous S/H abundance determinations in the literature is IIZw40. This galaxy has been observed by G89 and PMD03. In Table 2 we present the results for IIZw40 obtained by the three works. In order to minimize possible reddening corrections effects in the abundance calculation for this galaxy, we referred the flux of each sulfur line we measured to a nearby hydrogen line. In the case of 12 + log (S+/H+) ionic abundance the three values are close to each other; the value of the 12 + log (S++/H+) ionic abundance, derived in this work is higher than the previous ones by up to some 0.2 dex. We believe that this fact could be the result of our systematic absorption correction procedure.
Figure 7 shows the distribution of sulfur abundance derived
for our sample of HII galaxies. The empty and dashed histograms
represent the distribution of S/H derived with S23 for all the
objects and obtained from [SIII], respectively. Most of the
galaxies present total S/H abundance values that are between 1/20 solar to solar
. This is an expected behavior since our sample is composed mainly of low-luminosity galaxies. Besides, we note that the
dashed histogram peak corresponds to total S/H abundance value lower
than the S/H maximum of the empty histogram. It suggests that, in order
to know the overall metallicity distribution of a sample of galaxies,
it would be worth making use of an efficient empirical abundance
indicator. Hoyos & Díaz (2006) found a similar result by
studying the O/H abundance for a sample of HII galaxies.
The abundances obtained in this work allow us to study the dependence
of S/H as a function of O/H in low metallicity environments. In
Fig. 8 we show the relationship between the S/O abundance
ratio and total O/H abundance for the subset of galaxies with [OIII] and
[SIII]. The value of the sigma weighted mean
for log(S/O) is -1.68
0.20 dex. The galaxy with nearly solar
metallicity (UM307) is classified as an SABd from HYPERLEDA
database
.
Evaluating the contribution of all observational errors to the derivation of these abundances, we can conclude at this level of uncertainty that there is no statistical
evidence of any systematic variation of S/O with O/H for this range
of abundances. Therefore, our results agree with a constant
S/O ratio and lower (1)
than the solar ratio for this type of emission-line object.
This result indicates that sulfur and oxygen appear to be produced by the same massive stars,
as expected by current nucleosynthesis prescriptions (see Pagel 1997 and references therein). In recent works, I05 and PM06 indicate that
HII galaxy data are consistent with a constant S/O ratio, but somewhat lower
than the current solar ratio. Regarding disk HII regions, the
dispersion in S/O appears much larger and the assumptions of a constant S/O
is questionable there. These results suggest that the
assumption that the S/O ratio is constant at all abundances remains
controversial (e.g. Bresolin et al. 2004) and should
be explored further, particularly at the not very well-known metallicity
ends: extremely metal deficient HII galaxies (i.e. very low O/H) and
HII regions in the inner disk of galaxies (i.e. metal rich central
parts with highest O/H).
In this work we have performed a long-slit spectroscopic study of
a sample of 34 HII galaxies observed in the blue and near-IR ranges
(3700 -1
m). The red spectra were carefully corrected for the effects of the
telluric atmospheric absorption. Measurements of the nebular [SIII] lines at
9069,9532 were obtained for all objects.
Whenever possible we derived values of [SIII],
[OIII],
[OII], and
[SII] by combining our data in the red with
our data in the blue. Regarding
[SIII], most of the observed
HII galaxies show values that are slightly higher than those predicted
from
[OIII] by photoionization models. This effect can be
especially important for the high-excitation objects.
We derived the total S/H abundance for the 34 objects in the
sample. Total S/H abundance was calculated
directly using the electron temperature [SIII] in 22 HII galaxies,
for which the O/H abundance was obtained directly from the
observations using
[OIII]. For the rest of the objects total
S/H abundances were computed using the empirical abundance indicator S23.
A comparative study was performed on the reliability of S23and R23 as abundance indicators. No systematic variation in derived S/H with the excitation degree of the HII regions was found. That means that S23 is not sensitive to ionization effects, at first order, making it a robust empirical abundance indicator.
The comparison between
and S23 parameters for our
sample indicates that harder ionizing spectra are found in the HII galaxies with lower gaseous metallicity.
Comparing the ionic ratios O+/O++ and S+/S++ with the predictions of single-star photoionization models, we note
that a large fraction of galaxies in our sample are probably ionized
by very hard spectra. This result points out that extra heating sources might
exist, as has been suggested by recent works (Stasinska & Schaerer 1999; I05).
Finally, we presented a study of the abundance of S/H as a function of O/H in low-metallicity environments. Our data, together with other studies of S/H based upon the near-IR [SIII] lines, are consistent with the conclusion that S/O remains constant as O/H varies among the sample of HII galaxies. The scatter in S/O (due mainly to observational errors) is still large to constrain the degree of variation in S/O over the whole O/H abundance range. The assumption that the S/O ratio remains constant at all abundances is still an open question that should be explored further.
Acknowledgements
C.K wishes to thank the Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq-Brasil) for a grant and the Consejo Superior de Investigaciones Científicas (CSIC-Spain) for an I3P fellowship. We thank the referee for useful suggestions. We thank H.Plana for carrying out part of the spectroscopic observations. We also thank E. Pérez, R.M. González-Delgado and D. Reverte Payá for their help in the initial stages of this project, and to Jorge Iglesias-Páramo for his fruitful comments and careful reading of the manuscript. This research was partially funded by project AYA2004-08260-C03-02 of the Spanish PNAYA.
Table 1:
Reddening corrected line fluxes, relative to H = 100, and corresponding extinction coefficients for the sample of galaxies.