text:
\section{Introduction}

Oxygen is the main abundance tracer in HII regions and HII galaxies, but its abundance is
rather uncertain in those cases in which no direct determinations of the electron
gas temperature exist therefore requiring the use of empirical or semi-empirical methods.
 These methods are based on the cooling properties
of ionised nebulae which ultimately reflect on a relation between
emission line intensities and oxygen abundance. In fact, when the
cooling is dominated by oxygen, the electron temperature depends
inversely on oxygen abundance. Since the intensities of collisionally
excited lines depend exponentially on temperature, a relation is
expected to exist between these intensities and oxygen abundances. The
O$_{23}$ parameter, also known as R$_{23}$ and defined as the sum of the intensities of the [OII]
$\lambda\lambda$ 3727,29 \AA\ and [OIII]  $\lambda\lambda$ 4959, 5007 \AA\
emission lines relative to
H$\beta$ (Pagel et al., 1979), has been widely used for these purposes.

The relation between O$_{23}$ and oxygen abundance is however
two-folded
since at high metallicities, the efficiency of the oxygen as a cooling agent
decreases the strength of the oxygen emission lines while at low
metallicities the cooling is mainly exerted by hydrogen
and the oxygen line strengths increase with metallicity. A value of
12+log(O/H) of about 8.2 divides the two different abundance regimes. Although some line
ratios have been proposed in order to break this degeneracy, the fact that
a large number of HII regions/HII galaxies lie right
on the turnover region is of great concern.

On the other hand, the use of S/H as an abundance tracer has been
frequently overlooked.  Similarly to oxygen, sulphur is an element
produced in massive stars through explosive nucleosynthesis and its
yield should follow that of O. Nebular S/H abundances are therefore expected
to follow O/H and the S/O is expected to remain constant at
approximately the solar neighborhood value, log S/O $\simeq$ -1.6
(e.g. Lodders 2003; Bresolin et al. 2004). Empirical tests exploring
this have been performed confirming the cosmic nucleosynthetic ratio
though the results of some works suggest that this relation should be
explored further, particularly at the not 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 abundances).

   \begin{table*}
      \caption[]{Reddening corrected line fluxes for sulphur normalized to I(H$\beta$)=100
measured in spectra of SDSS low
metallicity galaxies referred in Kniazev et al. (2003), along with their reddening constants}
         \label{lines}

{
    $$
         \begin{array}{cccccc}

            \hline
            \noalign{\smallskip}
            Object      &  [SIII] \lambda 6312 \AA & [SII] \lambda 6716 \AA
& [SII] \lambda 6731 \AA & [SIII] \lambda 9069 \AA & C(H\beta) \\

\hline
SDSS J0133+1342 & 0.9\pm0.2 & 9.9\pm0.2 & 8.0\pm0.4 & 5.8\pm 0.4 & 0.03 \\
KUG 0203-100    & --        & 23.0\pm1.1 & 18.6\pm1.1 & 19.6\pm 1.1 & 0.19 \\
HS 0822+3542    & 1.4\pm0.3 & 2.8\pm0.2 & 2.2\pm0.2 & 6.0\pm 0.2 & 0.17 \\
I Zw 18 - NW    & 0.8\pm0.1 & 2.0\pm0.3 & 1.4\pm0.1 & 3.9\pm 0.3 & 0.05 \\
I Zw 18 - SE    & 0.5\pm0.2 & 3.9\pm0.2 & 2.8\pm0.2 & 3.4\pm 0.5 & 0.12 \\
SBS 1102+606    & 1.6\pm0.3 & 9.6\pm0.6 & 6.7\pm0.6 & 10.1\pm 0.6 & 0.15 \\
A1116+517       & 1.3\pm0.3 & 7.9\pm0.2 & 5.3\pm0.2 & 7.7\pm 1.8 & 0.17 \\
SDSS J1121+0324 & 1.3\pm0.4 & 12.2\pm0.8 & 9.6\pm0.8 & 4.2\pm 0.6 & 0.20 \\
SDSS J1201+0211 & 1.0\pm0.2 & 5.4\pm0.2 & 3.7\pm0.2 & 5.0\pm 0.3 & 0.14 \\
CGCG 269-049    & 1.4\pm0.3 & 6.5\pm0.3 & 3.1\pm0.3 & 5.9\pm 0.7 & 0.10 \\

\noalign{\smallskip}

            \noalign{\smallskip}
            \hline
         \end{array}
$$
}
   \end{table*}

The strong nebular lines of sulphur are analogous to those of oxygen
and hence similar reasonings may be put forward regarding the use of
the S$_{23}$ parameter, S$_{23}$ = [SII]$\lambda\lambda$6717,6731 +
[SIII]$\lambda\lambda$9069,9532)/H$\beta$ (V\'{\i}lchez \& Esteban, 1996) as an alternative
abundance indicator (D\'{\i}az \& P\'erez-Montero, 2000),
which in fact presents several advantages against
oxygen: 1) due to the longer wavelengths of the lines implied, its
relevance as a cooling agent starts at lower temperatures (higher
metallicities) what makes the relation to remain single-valued up to
solar abundances; 2) their lower dependence on electron temperature,
renders the lines observable even at over-solar abundances; 3) the
lines of both [SII] and [SIII] can be measured relative to nearby
hydrogen recombination lines, thus minimizing the effect of any
reddening and/or calibration uncertainties. On the negative side,
[SIII] lines shift out of the far red spectral region for redshifts
higher than 0.1. Given these properties, here we reccommend the use of
spectroscopy in the red-to-near infrared wavelength range in order to
derive physical properties and abundances, of HII regions, including
the lines from [SIII]$\lambda$ 6312 \AA , [SII]$\lambda$ 6717,31 \AA\
up to the [SIII]$\lambda$9069,9532 \AA . These lines can constitute a
convenient analogue in this wavelength range to the role played by the
[OII] and [OIII] lines in the optical. In additon, within this wavelength range
the effects of the extinction are less severe, thus favouring the
application of this calibration to the study of HII regions located
in the Milky Way disk, in the inner regions
of galaxies, or to star-forming galaxies/regions affected by a large amount of extinction.

In this paper, following earlier work by Christensen et al. (1997) and by Vermeij et al. (2002),
we have explored the behaviour of the sulphur emission lines in order to provide a useful abundance
calibration of S/H versus S$_{23}$ over the whole abundance range. This empirical calibration is based
on the bright sulphur lines and encompasses the whole range of abundance currently found in HII region studies.
This calibration appears to be independent of both, O/H and O$_{23}$, and is especially suited for
observations including (only) the red to near-infrared spectral range (from [SIII]$\lambda$ 6312 \AA ,
H$\alpha$ up to the 1$\mu$ CCD cut-off). For this wavelength regime, the sulphur lines can be easily scaled to
their respective closest Balmer or Paschen recombination line, H${\lambda}$ --instead of to H${\beta}$--
and $S_{23}$ can be written as follows:

\[S_{23}  = S'_{23} x \left(\frac{H{\lambda}}{H{\beta}}\right)_o \]

\noindent where S'$_{23}$ is the scaled value of S$_{23}$ and
$(H\lambda/H\beta)_o$ is the theoretical case B recombination ratio.

The calibrations can be extended further to the infrared to include the [SIV] 10.52 $\mu$ line
to S$_{23}$ and defining a new parameter, S$_{234}$ (Oey \& Shields, 2000).
However, the lack of [SIV] data renders difficult to check its reliability.

In the next section we present the sample of objects that we have used here to stablish the sulphur abundance
calibration as well as all the selected objects for which reliable ISO [SIV] data have been published.
Section 3 is devoted to the study of the ionisation correction factor (ICF),--not yet well stablished for sulphur--,
using selected data of HII regions including [SIV] infrared line fluxes, together with predictions
of photoionisation models. In Section 4 we present and discuss the proposed empirical calibration of
S/H versus S$_{23}$ and we summarize our conclusions.

\section{The selected sample of objects and sulphur abundances}

Our sample is a combination of different emission line objects ionised by
young massive stars: diffuse HII regions in the Galaxy and the Local Group, Giant
Extragalactic HII regions (GEHR) and HII galaxies, and therefore does not include planetary
nebulae or objects with non-thermal activity.
The emission line data along with their corresponding errors have been taken from the literature
for all objects except for the extremely metal-poor galaxies studied by Kniazev et al. (2003)
that present the strong [SIII] emission line at 9069 {\AA}.
The spectra of these objects have been taken from the data base of the DR3 of the Sloan Digital
Sky Survey (SDSS\footnote{The SDSS Web site is http://www.sdss.org}) and
the line fluxes have been measured and analyzed using the task SPLOT of the software package IRAF
\footnote{IRAF is distributed by the National Optical Astronomy Observatory}, following the
same procedure as in P\'erez-Montero \& D\'{\i}az (2003; hereinafter PMD03). We have found a good
agreement between the oxygen emission lines listed by Kniazev et al. (2003) and our measurements.
The reddening corrected sulphur emission line fluxes, normalized to I(H$\beta$) = 100,
 which are relevant for this work are listed in table \ref{lines}, together with their corresponding
reddening constants and errors.

   \begin{table*}
      \caption[]{Sulphur abundances and values of log S$_{23}$ for the sample of objects.
Objects marked with $^a$($^b$) have S$^+$(S$^{2+}$) abundances derived using electron temperatures based on
models from t([OIII]). See text for details. }
         \label{Ab}

    $$
         \begin{array}{cccc|cccc}

            \hline
            \noalign{\smallskip}
            Object      &  Ref.^a & 12+\log \left( \frac{S^++S^{2+}}{H^+} \right) & \log S_{23} &
	    Object      &  Ref.^a & 12+\log \left( \frac{S^++S^{2+}}{H^+} \right) & \log S_{23} \\
            \noalign{\smallskip}
            \hline

M51 - CCM10 & 1   & 6.95\pm0.10^a &  0.02\pm0.05  & N4A        & 4  & 6.74^a & 0.02    		     \\
M51 - CCM53 & 1   & 6.95\pm0.14^a &  0.01\pm0.06  & N79E       & 4  & 6.59^{a,b} & 0.00    		\\
M51 - CCM54 & 1   & 6.91\pm0.12^a &  0.08\pm0.05  & N191A      & 4  & 6.80^a & 0.14    		\\
M51 - CCM55 & 1   & 7.04\pm0.11^a &  0.05\pm0.06  & N80        & 4   & 6.02^{a,b} & -0.25    		\\
M51 - CCM57 & 1   & 6.82\pm0.15^a & -0.03\pm0.06  & N83        & 4   & 6.24^{a,b} & -0.09    		\\
M51 - CCM72 & 1   & 6.90\pm0.13^a & -0.03\pm0.06  & N13        & 4   & 6.20 & -0.08		\\
NGC1232 - 04  & 2   & 6.43\pm0.21^a & -0.05\pm0.08  & N81        & 4   & 6.29^b & -0.07    \\
NGC1232 - 05  & 2   & 7.01\pm0.16^a &  0.16\pm0.17  & N66        & 4   & 6.01^{a,b} & -0.31    		\\
NGC1232 - 07  & 2   & 7.02\pm0.21^a &  0.08\pm0.06  & NGC604 - A  & 5   & 6.82\pm0.03^{a,b}& 0.00\pm0.02   \\
NGC1232 - 14  & 2   & 6.84\pm0.16^a &  0.16\pm0.07  & NGC604 - C  & 5   & 6.78\pm0.02^{a,b} & 0.09\pm0.03   \\
NGC1365 - 05  & 2   & 6.92\pm0.08^a &  0.08\pm0.01  & NGC604 - D  & 5   & 7.03\pm0.13^a & 0.18\pm0.01   \\
NGC1365 - 08  & 2   & 6.81\pm0.08^a &  0.07\pm0.01  & NGC604 - E  & 5   & 7.00\pm0.14^a & 0.23\pm0.03   \\
NGC1365 - 14  & 2   & 6.96\pm0.11^a &  0.05\pm0.01  & NGC604      & 5   & 6.85\pm0.01^{a,b} & 0.06\pm0.01   \\
NGC1365 - 15  & 2   & 7.00\pm0.05^a &  0.23\pm0.01  & NGC604    & 8,5 & 6.79\pm0.09^b & -0.01\pm0.07   \\
NGC1365 - 16  & 2   & 6.69\pm0.13^a &  0.03\pm0.01  & NGC604    & 8,22 & 6.66\pm0.16 & -0.01\pm0.07   \\
NGC2997 - 04  & 2   & 6.85\pm0.18^a &  0.18\pm0.08  & NGC604    & 8,33 & 6.68\pm0.09^b & -0.01\pm0.07   \\
NGC2997 - 05  & 2   & 6.97\pm0.16^a &  0.18\pm0.08  & NGC595    & 8,33 & 6.78\pm0.15^b &  0.13\pm0.08   \\
NGC2997 - 06  & 2   & 6.92\pm0.16^a &  0.14\pm0.07  & IC 131     & 8,22 & 6.50\pm0.18^b &  0.06\pm0.08   \\
NGC2997 - 07  & 2   & 6.92\pm0.17^a &  0.13\pm0.08  & IC 131     & 8,33 & 6.65\pm0.15^b &  0.06\pm0.08 	\\
NGC2997 - 13  & 2   & 7.10\pm0.14^a &  0.15\pm0.07  & NGC588    & 8,22 & 6.42\pm0.14^b &  0.08\pm0.07 \\
NGC5236 - 03  & 2   & 6.92\pm0.17^a &  0.12\pm0.07  & NGC588    & 8,33 & 6.63\pm0.09^b &  0.08\pm0.07\\
NGC5236 - 06  & 2   & 7.00\pm0.20^a &  0.12\pm0.08  & NGC5471   & 8,24 & 6.18\pm0.13^b & -0.17\pm0.07\\
NGC5236 - 11  & 2   & 7.35\pm0.11^a &  0.30\pm0.07  & IC 10-2    & 8,23 & 6.61\pm0.06^b &  0.09\pm0.06\\
NGC5236 - 16  & 2   & 7.25\pm0.13^a &  0.25\pm0.07  & II Zw 40   & 8,7 & 6.13\pm0.05 & -0.22\pm0.06 \\
NGC628 - H13   & 3   & 6.41\pm0.07^a & -0.05\pm0.02 & II Zw 40   & 8,14 & 6.06\pm0.12 & -0.22\pm0.06\\
NGC1232 - CDT1 & 3   & 7.13\pm0.16^a & 0.11\pm0.03  & II Zw 40   & 8,21 & 6.11\pm0.06^b & -0.22\pm0.06\\
NGC1232 - CDT2 & 3   & 6.52\pm0.16^a & 0.21\pm0.03  & II Zw 40   & 8,23 & 6.14\pm0.06^b & -0.22\pm0.06\\
NGC1232 - CDT3 & 3   & 6.92\pm0.09^a & 0.16\pm0.02  & II Zw 40   & 8,24  & 6.12\pm0.06^b & -0.22\pm0.06 \\
NGC1232 - CDT4 & 3   & 6.93\pm0.07^a & 0.16\pm0.02  & NGC4861   & 8,6  & 6.37\pm0.12 & -0.02\pm0.12\\
NGC2467         & 4   & 6.39^b & -0.03 		& NGC2363   & 8,26 & 5.83\pm0.14 & -0.40\pm0.13\\
\eta Car   & 4   & 6.99 & 0.19   		& I Zw 123   & 8,7 & 5.92\pm0.16^b & -0.27\pm0.15\\
M17        & 4   & 6.92^b & 0.20   		& Mrk 36     & 8,15  & 5.91\pm0.17^b & -0.19\pm0.17\\
M20        & 4   & 6.99^a & 0.20    		& Mrk 36     & 8,7 & 5.88\pm0.14^b & -0.19\pm0.17\\
NGC3576   & 4   & 7.14^b & 0.46    		& Mrk 600    & 8,24  & 6.00\pm0.14^b & -0.34\pm0.13\\
Orion 1    & 4   & 6.93 & 0.03    		& I Zw 18    & 8,23 & 5.49\pm0.15^{a,b} & -0.68\pm0.18\\
Orion 2    & 4   & 6.97^b & 0.26    		& I Zw 18    & 8,24  & 5.51\pm0.19^{a,b} & -0.68\pm0.18\\
N59A       & 4   & 6.60^a & -0.01    		& M101 - H681& 9 & 6.06\pm0.09^{a,b} & -0.20\pm0.07\\
N44B       & 4   & 6.84^a & 0.09    		& M51 - CCM10 & 10 & 7.16\pm0.20^a &  0.20\pm0.05 \\
N55A       & 4   & 6.88^a & 0.04    		& M51 -	CCM72 & 10  & 7.56\pm0.02^a &  0.41\pm0.00\\
N113D      & 4   & 6.90^a & 0.25    		& NGC2403 - VS35 & 11 &  6.77\pm0.17 & 0.10\pm0.03\\
N127A      & 4   & 6.83 & 0.12 			& NGC2403 - VS24 & 11 & 7.04\pm0.11 & 0.10\pm0.04\\
N159A      & 4   & 6.53^{a,b} & 0.02    		& NGC2403 - VS38 & 11 & 6.87\pm0.09 & 0.06\pm0.02\\
N214C      & 4   & 6.75^a & 0.12    		& NGC2403 - VS44 & 11 & 6.63\pm0.07 & 0.04\pm0.02\\

            \noalign{\smallskip}

            \noalign{\smallskip}
            \hline
         \end{array}
     $$
}
\begin{list}{}{}
\item[$^{\mathrm{a}}$] {\scriptsize References are:
1. Bresolin et al., 2004; 2. Bresolin et al., 2005;
3. Castellanos et al., 2002;
4. Dennefeld \& Stasinska, 1983; 5. D\'\i az et al., 1987; 6. Dinnerstein \& Shields, 1986;
7. French, 1980; 8. Garnett, 1992; 9. Garnett \& Kennicutt, 1994; 10. Garnett et al., 2004; 11. Garnett et al., 1997;
12. Gonz\'alez-Delgado et al., 1995; 13. Gonz\'alez-Delgado et al., 1994
14. Guseva et al., 2000; 15. Izotov \& Thuan, 1988; 16. Izotov et al., 1994;
17. Izotov et al., 1997; 18. Kennicutt et al., 2003; 19. Kinkel \& Rosa, 1994;
20. Kniazev et al., 2003; 21. Kunth \& Sargent, 1983; 22. Kwitter \& Aller, 1981;
23. Lequeux et al., 1979; 24. Pagel et al., 1992; 25. Pastoriza et al., 2003; 26. Peimbert et al., 1986;
27. P\'erez-Montero \& D\'\i az, 2003;
28. Skillman \& Kennicutt, 1993;
29. Skillman et al., 1994; 30. Terlevich et al., 1991; 31. Vermeij et al., 2002;
32. V\'\i lchez \& Esteban, 1996; 33. V\'\i lchez et al., 1988; 34.This work.}

\end{list}
   \end{table*}
   \begin{table*}
    \setcounter{table}{1}
      \caption{Continued.}
         \label{Ab02}

    $$
         \begin{array}{cccc|cccc}

            \hline
            \noalign{\smallskip}
            Object      &  Ref.^a & 12+\log \left( \frac{S^++S^{2+}}{H^+} \right) & \log S_{23} &
	    Object      &  Ref.^a & 12+\log \left( \frac{S^++S^{2+}}{H^+} \right) & \log S_{23} \\
            \noalign{\smallskip}
            \hline

NGC2403 - VS51 & 11 & 6.75\pm0.17 & 0.06\pm0.06 &  NGC3310 - M     & 25 & 6.85\pm0.01^b & 0.06\pm0.01   \\
NGC2403 - VS3  & 11 & 6.62\pm0.04 & 0.06\pm0.03 &  II Zw 40      & 27,7 & 6.06\pm0.04 & -0.28\pm0.02     \\
NGC2403 - VS49 & 11 & 6.59\pm0.17 & 0.06\pm0.05 &  II Zw 40      & 27,14 & 6.04\pm0.05 & -0.28\pm0.02    \\
NGC2403 - VS48 & 11 & 6.60\pm0.26 & 0.08\pm0.09 &  II Zw 40      & 27,21 & 6.06\pm0.04 & -0.28\pm0.02  \\
NGC7714 - A    & 12 & 6.81\pm0.05^a & 0.19\pm0.01 & II Zw 40      & 27,23 & 6.10\pm0.04 & -0.28\pm0.02   \\
NGC7714 - N110 & 12 & 6.99\pm0.11^a & 0.18\pm0.05 & II Zw 40      & 27,24 & 6.06\pm0.04 & -0.28\pm0.02   \\
NGC7714 - B    & 12 & 6.31\pm0.06^a & 0.01\pm0.02 & Mrk 5         & 27,15 & 6.19\pm0.09 & 0.07\pm0.02\\
NGC7714 - C    & 12 & 6.41\pm0.18^a & 0.00\pm0.09 & SBS0749+568   & 27,17 & 6.04\pm0.11 & -0.17\pm0.04\\
NGC7714 - N    & 12 & 6.95\pm0.11^a & 0.22\pm0.05 & SBS0926+606   & 27,17 & 6.04\pm0.11 & -0.17\pm0.04\\
NGC2363 - A2   & 13 & 5.92\pm0.08 & -0.41\pm0.02 & Mrk 709       & 27,30 & 5.97\pm0.10 & -0.04\pm0.02\\
M101 - H1013	& 18 & 7.12\pm0.07 & 0.21\pm0.02 & Mrk 22        & 27,16 & 6.12\pm0.11 & -0.11\pm0.05\\
M101 - H1105	& 18 & 6.95\pm0.06 & 0.18\pm0.02 & Mrk 1434      & 27,17 & 5.76\pm0.08 & -0.38\pm0.03\\
M101 - H1159	& 18 & 6.68\pm0.09 & 0.10\pm0.03 & Mrk 36        & 27,7  & 5.96\pm0.12 & -0.21\pm0.04\\
M101 - H1170	& 18 & 7.08\pm0.08 & 0.36\pm0.03 & Mrk 36        & 27,15 & 5.98\pm0.13 & -0.21\pm0.04\\
M101 - H1176	& 18 & 6.82\pm0.06 & 0.14\pm0.02 & VIIZw403      & 27,17 & 6.10\pm0.11 & -0.27\pm0.04\\
M101 - H1216	& 18 & 6.55\pm0.07 & 0.01\pm0.03 & UM461         & 27,15 & 5.74\pm0.06 & -0.35\pm0.02\\
M101 - H128	& 18 & 6.81\pm0.07 & 0.11\pm0.02 & UM462         & 27,15 & 6.13\pm0.10 & -0.13\pm0.04\\
M101 - H143	& 18 & 6.73\pm0.09 & 0.13\pm0.03 & Mrk209        & 27,17 & 5.94\pm0.10 & -0.28\pm0.04\\
M101 - H149	& 18 & 6.72\pm0.07 & 0.12\pm0.02 & IZw18 - SE     & 28 & 5.31\pm0.12^b & -0.78\pm0.07\\
M101 - H336 (S5)	& 18 & 7.10\pm0.09 & 0.21\pm0.03 & IZw18 - NW     & 28 & 5.13\pm0.10^b & -0.93\pm0.08\\
M101 - H409	& 18 & 6.63\pm0.07 & 0.08\pm0.03 & UGC4483        & 29 & 5.77\pm0.13 & -0.39\pm0.05\\
M101 - H67	& 18 & 6.60\pm0.14 & 0.07\pm0.03 &  N160 - A1      & 31 & 6.91\pm0.06 & 0.17\pm0.03\\
M101 - NGC 5471A& 18 & 6.29\pm0.07 & -0.11\pm0.03&  N160 - A2     & 31 & 6.86\pm0.07 & 0.14\pm0.03\\
M101 - NGC 5471B& 18 & 6.31\pm0.08 & 0.02\pm0.03 & N159 - 5      & 31 & 7.01\pm0.10 & 0.22\pm0.03\\
M101 - NGC 5471C& 18 & 6.42\pm0.08 & -0.05\pm0.03& N157 - B      & 31 & 6.87\pm0.09 & 0.24\pm0.04\\
M101 - NGC 5471D& 18 & 6.51\pm0.10 & -0.02\pm0.03 & 30Dor - 1      & 31 & 6.72\pm0.08 & 0.06\pm0.02\\
M101 - S5       & 19 & 7.31\pm0.04 & 0.31\pm0.00  & 30Dor - 2      & 31 & 6.80\pm0.09 & 0.11\pm0.02\\
SDSS J0133+1342 & 20,34 & 5.58\pm0.13^a & -0.42\pm0.03 & 30Dor - 3      & 31 & 6.87\pm0.06 & 0.14\pm0.02\\
KUG 0203-100    & 20,34 & 6.02\pm0.04^a & 0.04\pm0.05  & 30Dor - 4      & 31 & 6.79\pm0.08 & 0.12\pm0.02\\
HS 0822+3542    & 20,34 & 5.27\pm0.19^a & -0.59\pm0.01 & N11 - A        & 31 & 6.78\pm0.09 & 0.10\pm0.03\\
I Zw 18 - NW    & 20,34 & 5.08\pm0.18^a & -0.78\pm0.04 & N83 - B        & 31 & 6.82\pm0.07 & 0.13\pm0.03\\
I Zw 18 - SE    & 20,34 & 5.19\pm0.23^a & -0.73\pm0.06 & N79 - A        & 31 & 6.96\pm0.07 & 0.19\pm0.02 \\
SBS 1102+606    & 20,34 & 5.67\pm0.19^a & -0.29\pm0.02 & N4 - A         & 31 & 6.79\pm0.07 & 0.10\pm0.02 \\
A1116+517       & 20,34 & 5.49\pm0.31^a & -0.40\pm0.09 & N88 - A        & 31 & 5.92\pm0.10 & -0.32\pm0.03\\
SDSS J1121+0324 & 20,34 & 5.49\pm0.31^a & -0.44\pm0.06 & N66            & 31 & 6.23\pm0.15 & -0.08\pm0.05\\
SDSS J1201+0211 & 20,34 & 5.28\pm0.18^a & -0.58\pm0.02 & N81            & 31 & 6.22\pm0.10 & -0.17\pm0.03\\
CGCG 269-049    & 20,34 & 5.39\pm0.21^a & -0.50\pm0.05 & S209       & 32   & 5.76\pm0.20^b & -0.35\pm0.07\\
M101 - NGC5455    & 22   & 6.75\pm0.10^{a,b} &  0.14\pm0.05 & S127       & 32   & 6.42\pm0.29^b & -0.12\pm0.07 \\
M101 - NGC5471    & 22   & 6.31\pm0.10^{a,b} & -0.06\pm0.05 & S128       & 32   & 6.40\pm0.29^b & -0.09\pm0.06 \\
NGC3310 - A        & 25 & 6.82\pm0.03^a & 0.00\pm0.02   & MA2        & 33   & 6.94\pm0.34^b & 0.08\pm0.02  \\
NGC3310 - B        & 25 & 6.78\pm0.02^b & 0.09\pm0.03   & NGC 604    & 33   & 6.76\pm0.03^b & 0.06\pm0.01  \\
NGC3310 - C        & 25 & 7.03\pm0.13 & 0.18\pm0.01   & NGC 595    & 33   & 7.02\pm0.09^b & 0.36\pm0.02  \\
NGC3310 - E        & 25 & 7.00\pm0.14 & 0.23\pm0.03   &  & & & \\

            \noalign{\smallskip}

            \noalign{\smallskip}
            \hline
         \end{array}
     $$
}
\begin{list}{}{}
\item[$^{\mathrm{a}}$] {\scriptsize  References are:
1. Bresolin et al., 2004; 2. Bresolin et al., 2005;
3. Castellanos et al., 2002;
4. Dennefeld \& Stasinska, 1983; 5. D\'\i az et al., 1987; 6. Dinnerstein \& Shields, 1986;
7. French, 1980; 8. Garnett, 1992; 9. Garnett \& Kennicutt, 1994; 10. Garnett et al., 2004; 11. Garnett et al., 1997;
12. Gonz\'alez-Delgado et al., 1995; 13. Gonz\'alez-Delgado et al., 1994
14. Guseva et al., 2000; 15. Izotov \& Thuan, 1988; 16. Izotov et al., 1994;
17. Izotov et al., 1997; 18. Kennicutt et al., 2003; 19. Kinkel \& Rosa, 1994;
20. Kniazev et al., 2003; 21. Kunth \& Sargent, 1983; 22. Kwitter \& Aller, 1981;
23. Lequeux et al., 1979; 24. Pagel et al., 1992; 25. Pastoriza et al., 2003; 26. Peimbert et al., 1986;
27. P\'erez-Montero \& D\'\i az, 2003;
28. Skillman \& Kennicutt, 1993;
29. Skillman et al., 1994; 30. Terlevich et al., 1991; 31. Vermeij et al., 2002;
32. V\'\i lchez \& Esteban, 1996; 33. V\'\i lchez et al., 1988; 34. This work.}

\end{list}
   \end{table*}

For all the objects of the sample measurements of the emission lines of [SII] at 6717,31 {\AA}
and of [SIII] at 9069,9532 {\AA} exist, thus allowing the simultaneous determination of the  S$_{23}$
parameter and the abundances of S$^+$ and S$^{2+}$.

The physical conditions of the ionised gas in each sample object, including electron temperatures,
electron density and sulphur abundances,
have been computed from the original emission line data using the same procedures as in
PMD03, based on the five-level statistical
equilibrium model in the task TEMDEN and IONIC, respectively, of the software package IRAF
(De Robertis, Dufour \& Hunt, 1987; Shaw \& Dufour, 1995). The atomic coefficients used are the
same as in PMD03 (see Table 4 of that work). Electron densities are determined
from the the [SII] $\lambda$ 6717{\AA} / $\lambda$ 6731{\AA} line ratio. Electron temperatures
have been calculated from the [SIII] ($\lambda$ 9069{\AA}+$\lambda$9532{\AA})/
$\lambda$ 6312{\AA} line ratio for all but 44 objects of the sample
for which the [OIII] ($\lambda$
4959{\AA}+$\lambda$5007{\AA})/$\lambda$ 4363{\AA} line ratio has been used.
For these objects, marked with $^b$ in table 2, a theoretical relation between [OIII] and [SIII]
electron temperatures has been used:
\[t([SIII]) = 1.05t([OIII]) - 0.08\]

This relation is based on the grids of photo-ionisation models described in P\'erez-Montero \& D\'\i az (2005)
and differs
slightly from the empirical relation found by Garnett (1992), mostly
due to the introduction of the new atomic coefficients
for S$^{2+}$ from Tayal \& Gupta (1999).

Regarding [SII] temperatures, for those objects without the [SII] auroral lines
at 4068,4074 \AA. we have taken the approximation
t[SII] $\approx$ t[OII] as valid.
For 124 objects of the sample it has been possible to
derive t[OII] from the [OII]($\lambda$ 3726{\AA}+$\lambda$3729{\AA})
/$\lambda$ 7325{\AA} line ratio. \begin{footnote}{The [OII] $\lambda$7319{\AA}+$\lambda$7330{\AA}
lines can have a contribution
by direct recombination which increases with temperature. Using
the calculated [OIII] electron temperatures, we have estimated these contributions  to be less than 4 \% in all cases
and therefore we have not corrected for this effect}\end{footnote}. For
the rest of the objects of the sample, marked with $^a$ in table 2
, not presenting any auroral line in the low excitation zone,
we have resorted to the model
predicted relations between
t([OII]) and t([OIII]) found in PMD03 that take explicitly into account the dependence of t([OII])
on electron density. This can affect the deduced abundances of $S^+/H^+$
by non-negligible factors, larger in all cases than the reported
errors.

 For those objects for which multiple observations exist we have considered
each one of them as independent.
The final quoted errors in the derived quantities have been calculated
by propagating the measurement errors in the emission lines provided by
the different authors. This information is not provided for the objects from Dennefeld \& Stasi\'nska (1983;
reference 4). The ionic abundances of sulphur, S$^+$/H$^+$  and S$^{2+}$/H$^+$, together with
the values of the S$_{23}$ parameter for each object are given in table \ref{Ab}.

It is important to emphasize here that this database include objects covering all the
abundance range from low metallicity HII galaxies, at 1/40 of the solar abundance, up
to HII regions in the disks of spirals populating the high metallicity range,
up to $\approx$ 3 Z$_\odot$. Although he data selected for this study have been obtained using different
apertures and instrumental configurations and therefore do not constitute a homogeneous sample, they have been reanalysed and ionic abundances have been  derived in a homogeneous manner. Using this sample we can study on a firmer basis the
empirical relationship between the sulphur abundance and the parameter S$_{23}$. In order
to do that we explore first the sum of the abundances of S$^+$ and S$^{2+}$ as
a function of S$_{23}$ and, on a second step, we will derive the calibration of
the total abundance of sulphur as a function of S$_{23}$.  The result is plotted in
figure \ref{S23_S_01}, showing a relationship with  very low scatter for which we have
obtained the following quadratic fit:

\[12+\log\left(\frac{S^++S^{2+}}{H^+}\right) = 6.540 + 2.071 \log S_{23} + 0.348 \left( \log S_{23} \right) ^ 2 \]

\noindent with a typical dispersion of 0.17 dex, defined as the standard deviation of the residuals
of the points.

   \begin{figure}[t]
   \centering
   \includegraphics[width=8.5cm,clip=]{s23_S_02.eps}
   \caption{The calculated sulphur abundance for the objects of the sample
versus the S$_{23}$ parameter. The thick line represents the quadratic fit of the points.}
              \label{S23_S_01}
    \end{figure}

After the advent of the ISO mission, it has also been possible to obtain data of
the [SIV] at 10.52 $\mu$ emission line for a selected sample of objects, thus allowing
the derivation of the S$^{3+}$/H$^+$ ionic abundance ratio. We have collected data
for 11 HII regions (plus one supernova remnant) in the Large and Small Magellanic Clouds
(Vermeij et al., 2002) and for the HII galaxy Mrk209 (Nollenberg et al., 2002).
For all these objects the $S^{3+}$ ionic abundances have been recalculated following
the procedure described above and using the most recent atomic coefficients from
Saraph \& Storey (1999). The calculated abundances are listed in table 3.

It has been a matter of debate for some time now what is the exact contribution of the
S$^{3+}$/H$^+$ ionic abundance to the total abundance of sulphur. It is clear that an
efficient solution to this problem could be reached making use of the measurements of
the infrared lines of [SIV] --not available for a large sample of objects yet--.

This question takes us straight into the issue of the ionisation correction factor, a
necessary step for the derivation of the empirical sulphur abundance calibration. In any
case, it has been already pointed out that a one-zone ionisation scheme may provide some
insight into the situation for not ionisation bounded HII regions of moderate to low ionisation,
where the various ions coexist throughout the nebula (e.g. Pagel 1978). For this reason we
have presented above the general correlation between S$^+$ + S$^{2+}$ and S$_{23}$. A
study of the ionisation correction factor scheme for sulphur is presented in the next section.

   \begin{table}
      \caption{Abundances of S$^{3+}$ for the objects for which there are ISO observations of the
[SIV] 10.52 $\mu$ emission line and the corresponding ICF(S$^+$+S$^{2+}$).}
         \label{Ab2}
    $$
         \begin{array}{cccc}

            \hline
            \noalign{\smallskip}
            Object      &  Ref.^a & 12+\log \left( \frac{S^{3+}}{H^+} \right) & ICF(S^++S^{2+})\\
            \noalign{\smallskip}
            \hline
\\
Mrk209     & 1   & 5.93\pm0.20 & 1.97\pm0.62  \\
Mrk209^b   & 1 & 5.68\pm0.23  &  1.56\pm0.76 \\
N160-A1    & 2   & 6.08\pm0.11 & 1.15\pm0.05  \\
N160-A2    & 2   & 5.90\pm0.10 & 1.11\pm0.03  \\
N159-5     & 2   & 6.03\pm0.10 & 1.10\pm0.04  \\
N157-B     & 2   & 5.54\pm0.12 & 1.05\pm0.02  \\
30Dor-1    & 2   & 6.16\pm0.11 & 1.27\pm0.10  \\
30Dor-2    & 2   & 6.24\pm0.11 & 1.27\pm0.10  \\
30Dor-3    & 2   & 6.16\pm0.10 & 1.20\pm0.06  \\
30Dor-4    & 2   & 6.15\pm0.10 & 1.23\pm0.07  \\
N83-B       & 2  & 5.45\pm0.12 & 1.04\pm0.02  \\
N4-A        & 2  & 6.17\pm0.15 & 1.24\pm0.11  \\
N88-A       & 2  & 5.80\pm0.10 & 1.75\pm0.27  \\
N66         & 2  & 5.73\pm0.15 & 1.32\pm0.19  \\
N81         & 2  & 5.45\pm0.11 & 1.17\pm0.07  \\
\hline

\noalign{\smallskip}

            \noalign{\smallskip}
            \hline
         \end{array}
     $$
\begin{list}{}{}
\item[$^{\mathrm{a}}$] {\scriptsize The corresponding references for the emission line data
of [SIV] at 10.5 $\mu$ are: 1. Nollenberg et al., 2002; 2. Vermeij et al., 2002}
 \item[$^{\mathrm{b}}$] {\scriptsize Assumming a constant $S^{3+}/S^{2+}$ ratio from the [SIII] lines in the near-IR from PMD03}
\end{list}
   \end{table}

\section{The ICF Scheme}

Perhaps one of the most difficult aspects in the derivation of total
abundances is the question of the ionisation correction factor, ICF.
The ICF for sulphur accounts for the contribution of the ionic species
not detected in the optical.
In high excitation nebulae a large fraction of the sulphur can be found in the S$^{3+}$ stage, whose
prominent emission lines of [SIV] are observed in the mid-IR at 10.52 $\mu$. Therefore, in order to derive the total abundance of
sulphur it is necessary to correct for the presence of S$^{3+}$ in those objects for which there are not  observations
in the mid-IR, as follows.

\[\frac{N(S)}{N(H)} = ICF(S^++S^{2+}) \cdot \frac{N(S^++S^{2+})}{N(H^+)} =\]
\[= \frac{N(S^++S^{2+}+S^{3+})}{N(S^++S^{2+})} \cdot \frac{N(S^++S^{2+})}{N(H^+)}\]

The first proposed ICF scheme for sulphur (Peimbert \& Costero, 1969) was based on the similarity of the ionisation
potentials of O$^+$ (35.1 eV) and S$^{2+}$ (34.8 eV)

\[ICF(S^++S^{2+}) = \frac{N(O)}{N(O^+)}\]

Nevertheless, some authors have pointed out that this relation has a
strong correlation with the ionisation degree of the nebula
(e.g. Barker 1978; Pagel 1978), thus implying an overestimation of the
sulphur abundance in nebulae with low electron temperature. Barker
(1980) proposed a new relation, based on the photoionisation models of
Stasi\`{n}ska (1978):

\[ICF(S^++S^{2+}) = \left[ 1-\left( 1-\frac{N(O^+)}{N(O)} \right)^\alpha\right]^{-1/\alpha} \]

\noindent for which he proposed a value of $\alpha$ = 3. The ICF from Peimbert \& Costero corresponds to a value for $\alpha$ = 1 in this expresion.
Later, Izotov et al. (1994), based on photoionisation models from Stasi\`{n}ska (1990) gave a fit for this ICF that,
in fact, is quite similar to the Barker formula for $\alpha$ = 2.

In figure 2 we show our computation of the ICF(S$^++S^{2+}$) as a
function of log ($O^+/O$) using the data listed in table 3, for three
different values of $\alpha$ =1,2,3. It is apparent in this plot that
most points are better matched for
$\alpha$ values between 2 and 3. Only one point, corresponding to a
HII galaxy (Mrk 209, solid square), shows an ICF for a value of $\alpha$ even lower than 2. Since the
$S^{2+}$ abundances obtained from the [SIII] line at 18.71 $\mu$ from the ISO observations from
Nollenberg et al. (2002) are much higher than those obtained from the near-IR [SIII] (PMD03),
we have recalculated $S^{3+}$ abundances assuming a constant $S^{3+}$/$S^{2+}$ ratio.
This value is showed in table 3 and is represented as an open square in figures 2 and 3.
Although showing a large error bar,
the new value lies within the zone of $\alpha$ between 2 and 3, in better
 agreement to the values predicted by photo-ionisation models (PMD03).

   \begin{figure}[t]
   \centering
   \includegraphics[width=8.5cm,clip=]{icfs.eps}
   \caption{Ionisation correction factor for the sum of $S^{+}$ and $S^{2+}$ versus the $O^+/O$ ratio for the
sample of objects listed in table 3. The solid lines represent the Barker's formula for different values of the
$\alpha$ parameter. Squares represent different values for Mrk209 (see text for details), diamonds for
HII regions in the Large Magellanic Cloud and circles in the Small Magellanic Cloud.}
              \label{ICF_01}
    \end{figure}

Since the relevant lines for sulphur abundance determination are in
the red to near infrared range, it is worth trying to relate the ICF
scheme of sulphur to the ionisation structure as seen in this
wavelength range. This aproach has the extra bonus of reducing the
effect of reddening in the line ratios currently used.  In order to
derive a new ICF scheme for sulphur based only on the red-to-near
infrared information, we need to combine available data and compute
new models for reference objects, for which we know all the relevant
ionic abundances of sulphur. We have computed this relation and is
shown in figure~\ref{ICF02}.  In this plot, we present the
ICF(S$^{+}$ + S$^{++}$) vs. log ([SIII]/[SII]) predicted by
photo-ionisation models using CoStar model atmospheres of
different effective temperatures (35kK, 40kK, 50kK, P\'erez-Montero \& D\'\i az, 2005)
and HII galaxy models (P\'erez-Montero \& D\'\i az, 2004),
together with all the observed points available.  Clearly, the ICF
predicted by a model with a single-star of Teff=35kK is always giving
ICF=1 no matter the excitation. The ICF predicted for objects
presenting log([SIII]/[SII]) $\le$0.2 remains small, 1.0$\le$ICF$\le$1.05.
Above log([SIII]/[SII])=0.4, the ICF model predictions begin to
diverge. Up to some point, this behaviour seems to be followed by the
data. Giant HII regions points cluster around the
locus of 40kK models, except in the notable case of N88A, a SMC reddened, very young
HII region breaking out its natal cloud (Heydari-Malayeri et al., 1999).
In this plot this giant HII region is located closed to Mrk209, the only HII galaxy in table 3.
This fact indicates a hotter ionising source and a larger ICF. It is suggested here that
this behaviour could be consistent with the prediction from single
burst evolutionary models (e.g. Stasi\'nska et al. 2001) since typically
HII galaxies host younger ionizing clusters than giant HII regions (Terlevich et al. 2004).
Under this assumption, the equivalent
width of H$\alpha$, an age indicator, should provide a useful constraint.

   \begin{figure}[t]
   \centering
   \includegraphics[width=8.5cm,clip=]{icfs_s2s3mg_02.eps}
   \caption{Ionisation correction factor for the sum of $S^{+}$ and $S^{2+}$ versus log ([SIII]/[SII]) for the
sample of objects listed in table 3. The dashed lines represent the results from photo-ionisation models for CoStar
single star atmospheres with the labelled effective temperature. Crosses represent results from photo-ionisation tailored models
of HII galaxies. The rest of symbols are the same as in figure 2.}
              \label{ICF02}
    \end{figure}

\section{Discussion}

Earlier works by Christensen et al. (1997) and by Vermeij et al. (2002) have explored the abundance
calibration of S/H versus S$_{23}$.
Christensen et al. (1997) proposed a linear S$_{23}$ calibration as follows

\[12+\log\left(\frac{S}{H}\right) = 6.485 + 1.218 \log S_{23}\]

\noindent using data from giant HII regions and HII galaxies
available to this date, and complementary model predictions from
Stasi\'nska (1990). Though these points included some high metallicity
HII regions of M51 from Diaz et al. (1991), as well as lower
metallicity objects from Garnett (1992), still the whole abundance
range was not sufficiently well sampled. They claimed that more data were
needed before a definite conclusion could be drawn.

   \begin{figure}[t]
   \centering
   \includegraphics[width=8.5cm,clip=]{s23_S_03.eps}
   \caption{Calculated total sulphur abundance for the objects of the sample
versus the S$_{23}$ parameter. The thick line represents the empirical calibration proposed in this work}
              \label{s23S03}
    \end{figure}

Vermeij et al.(2002) derived sulphur abundances for a new data set of
optical and infrared spectra of HII regions in the Large and Small
Magellanic Clouds. This information allowed these authors to derive
all the ionic fractions of sulphur; including S$^{+3}$ from ISO
[SIV] 10.5 $\mu$ line for their sample objects. They present a
comparison of their S/H abundances points vs. S$_{23}$ and S$_{234}$
with model calculations for log U = 0, -1, -2, and -3. The following
relation was found between log S$_{23}$ and log(S/H)

\[\log\left(\frac{S}{H}\right) = -5.65 + 1.50 \log S_{234}\]

However no relation was proposed for S/H and S$_{23}$.

In this work,we present an empirical abundance calibration, based on
the bright sulphur lines, which encompasses the whole range of abundance
currently found in HII region studies. This calibration is firmly
based on an extended homogeneous data base.  In figure 4 we
present the relation for all the objects of our sample between the
S$_{23}$ parameter and the total abundance of sulphur, taking into
account the ionic abundances of S$^+$, S$^{2+}$ and the ICF
corresponding to the formula of Barker for $\alpha$ = 2.5 which is the
value that better fits the available points. The best quadratic fit to
the data gives:

\[12+\log\left(\frac{S}{H}\right) = 6.622 + 1.860 \log S_{23} + 0.382 \left( \log S_{23} \right) ^ 2 \]

\noindent with a dispersion of 0.185 dex in the range of -1.0 $\le$ log(S$_{23}$) $\le$ 0.5.

This calibration is, to first order, independent of both, O/H and O$_{23}$,
and is especially suited for observations including only the red to
near-infrared spectral ranges (from [SIII]$\lambda$ 6312 \AA ,
H$\alpha$ up to the 1$\mu$ CCD cut-off). Though the S$_{23}$ parameter is
possibly double valued, like
R$_{23}$, the turnover region for S$_{23}$ is located above the range
of sulphur abundance currently found in disk HII regions.

   \begin{figure}[t]
   \centering
   \includegraphics[width=8.5cm,clip=]{SO_O.eps}
   \caption{Representation of the quotient of S/O versus O/H for the compiled sample and the solar value }
              \label{SO_O}
    \end{figure}

The calibration is, to some extent, affected by the ICF calculation scheme.
However only 34\% of the objects in our sample show an ICF larger than 1.2
as derived from Barker's expression ($\alpha$ = 2.5) and all of them show
log ([SIII]/[SII]) $>$ 0.4, where model predictions are more uncertain. In fact,
the calibration of (S$^+$+S$^{2+}$)/H$^+$ vs. S$_{23}$ does not differ much
from that of S/H vs. S$_{23}$ (see figures 1 and 4) and the values obtained
from both for a given S$_{23}$ are within the quoted uncertainty in most cases.

This calibration makes possible the use of S/H as metallicity tracer in ionized
nebulae. Its translation however to an O/H abundance relies on the assumption that
the S/O ratio remains constant at all abundances. This point though remains
controversial (see e.g.Lodders, 2003; Bresolin et al. 2004). Figure 5 shows
the S/O ratio vs. 12+log(O/H) for the objects in our sample. For all of them, the
O/H abundance has been calculated following the scheme presented in
P\'erez-Montero \& D\'{\i}az (2005). It can be seen from the figure that HII galaxy data
are consistent with a constant S/O ratio, but significantly lower than the solar ratio. Four
galaxies deviate from this trend (UGC4483, KUG 0203-100, Mrk709 and SDSS J1121+0324).
One of them, Mrk 709, also shows a large value of N/O (PMD03).
Regarding disk HII regions the dispersion is much larger and the assumptions of a
constant S/O is highly questionable.

Summarizing, following earlier work by Christensen et al and Vermeij et
al, we have derived an empirical calibration of the abundance of S/H
as a function of the S$_{23}$ parameter, defined using bright sulphur
lines, which we recommend as a useful tool to derive S/H within a
large abundance range of 2 dex, keeping a statistical error of 0.18
dex rms. This abundance range appears well suited to deal with objects
from low metallicity HII galaxies to high metallicity HII regions
located in the inner parts of the disks of spirals.

\begin{acknowledgements}
      This work has been partially supported by projects AYA-2004-08260-C03-02
and AYA-2004-08260-C03-03 of the Spanish National Plan for Astronomy and
Astrophysics.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


Description: Isabelle Karst Durnam (1906-1990) on a horse with David Angus "Kid" Johnston (1851-1938) on the back. There is a child on a stool and two women in front. Kid Johnston had a saloon in Manhattan, Montana. They are at the Karst Kamp and Stage Stop, Gallatin Canyon, Montana. Vintage 4.75x4 in. copy neg.
Description: Isabelle Karst Durnam (1906-1990), Pete Karst's step-daughter, hunting near the asbestos mine at Karst Stage Stop, Gallatin Canyon, Montana. She is on a horse holding a rifle. Vintage 4.75x4 in. copy neg.
Description: Isabelle Karst Durnam (1906-1990), Pete's step-daughter, standing on bridge over Gallatin River, looking North. In the early 1900s, the wagons crossed the river at this location. The bridge was later moved below the present location. Vintage 5x4 in. copy neg.
Description: Eddie (1895-1970) and Isabelle Karst Durnam 1906-1990) with Ray Hill and pack horses, Karst Kamp and Stage Stop, Gallatin Canyon, Montana. Ray Hill was a hunting guide for Pete Karst. Vintage 5x4 in. copy neg.
Description: Eddie (1895-1970) and Isabelle Karst Durnam (1906-1990) working their lettuce fields with other helpers. Isabelle was Pete's step-daughter. The lettuce fields were located one and a half miles south of Karst Stage Stop. There is a sign there today that says "Durnam Meadows." Vintage 5x4 in. copy neg.


text:
Q: SQL update within same table based on summation I have this table called t, as shown below.
   cust_id|    brand|    bill_amt|       AA|        BB|
   1234   |       AA|         100|     NULL|      NULL|
   5678   |       AA|         300|     NULL|      NULL|
   5678   |       BB|         350|     NULL|      NULL|
   5678   |       BB|         600|     NULL|      NULL|

I have around hundred thousands of records in my data, is there anyway I can update t table as shown below?
   cust_id|    brand|    bill_amt|       AA|        BB|
   1234   |       AA|         100|      100|      NULL|
   5678   |       AA|         300|      300|       950|
   5678   |       BB|         350|      300|       950|
   5678   |       BB|         600|      300|       950|

How can I show the bill_amt values under the AA and BB columns?
How can I sum up the bill_amt spent on the brand within the same customer?
For example, looking at customer 5678, she spent $350 and $600 on different days for brand BB, how can I show in BB Column the summation of the bill_amt she spent for BB?
Also, the same customer has spent $300 on AA, how can I show this value in the AA column?

A: To select the summary without actually creating a summary field in the table, you can simply use OVER; creating this as a view would most likely allow you the same advantages without altering the table.
SELECT CUST_ID, BRAND, BILL_AMT,
  SUM(CASE WHEN brand='AA' THEN bill_amt ELSE NULL END)
    OVER (PARTITION BY cust_id) AA,
  SUM(CASE WHEN brand='BB' THEN bill_amt ELSE NULL END)
    OVER (PARTITION BY cust_id) BB
FROM t;

To actually update the table, you can use a common table expression, however I'd sincerely advise against this except possibly for historical data that can never change, as changes to the data will no longer automatically update the summary.
WITH cte AS (
  SELECT *,
    SUM(CASE WHEN brand='AA' THEN bill_amt ELSE NULL END)
      OVER (PARTITION BY cust_id) AA2,
    SUM(CASE WHEN brand='BB' THEN bill_amt ELSE NULL END)
      OVER (PARTITION BY cust_id) BB2
  FROM t
)
UPDATE cte SET AA=AA2, BB=BB2;

An SQLfiddle for testing both ways.

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text:
package com.kwala.app.quiz.take_quiz;

import android.content.Context;
import android.util.AttributeSet;
import android.view.LayoutInflater;
import android.widget.Button;
import android.widget.RelativeLayout;

import com.kwala.app.R;
import com.kwala.app.models.RQuizAnswer;

/**
 * @author jacobamuchow@gmail.com
 */

public class AnswerCell extends RelativeLayout {
    private static final String TAG = AnswerCell.class.getSimpleName();

    private Button answerButton;

    public AnswerCell(Context context) {
        super(context);
        initialize();
    }

    public AnswerCell(Context context, AttributeSet attrs) {
        super(context, attrs);
        initialize();
    }

    public AnswerCell(Context context, AttributeSet attrs, int defStyleAttr) {
        super(context, attrs, defStyleAttr);
        initialize();
    }

    private void initialize() {
        LayoutInflater.from(getContext()).inflate(R.layout.quiz_answer_cell, this);

        answerButton = (Button) findViewById(R.id.quiz_answer_cell_answer_text);
    }

    public void setViewData(RQuizAnswer answer) {

        answerButton.setText(answer.getAnswer());
    }

    @Override
    public void setOnClickListener(OnClickListener l) {
        if (answerButton != null) {
            answerButton.setOnClickListener(l);
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
By Jacob Gepner, Hartland, WI
"I don't know. It's just fun. I've been around it my whole life."
Tyler M is 17 years old. He loves cars—but more than cars; really, he just loves mechanics.
"My dad has been tinkering around with cars since I can remember," says Tyler. "Naturally, I liked to help him, and I absolutely fell in love with it. Just taking something that's broken and fixing it with your own hands…it's just an awesome feeling."
Tyler's first experience with mechanics came when his dad bought him a go-kart. He was 13 at the time.
"Yeah, I had been bugging him for a go-kart for years. When he took me out to the garage and I saw it, I was in disbelief. It was probably the coolest thing he's gtten for me."
The only catch was it didn't run, and his dad wasn't going to help him.
"He told me I had to fix it by myself. He'd buy the parts, but he wouldn't do any work."
So Tyler started diagnosing and taking it apart. His third day on the job, he finally got the go-kart to run.
"Me and my friend were in the garage and we thought it was ready to run. So we pulled the cord, and it ran, alright. Right out of the garage. I couldn't believe it. The thing went by itself and was flying out of the garage. It took a hard left out of the garage and into the backyard. We were chasing after it, but that thing was cruising. There was no way we'd catch it. So it's flying across the yard and it turns left again…right into our swimming pool. It bent the support bar and left a dent in the side of the pool. It was absolutely hilarious. The best part was my parents were selling the house that week and the people that bought it never saw the dent."
The problem was a high idle. The carburetor needed to be adjusted.
"We took care of that no problem."
He eventually moved on from fixing his go-kart to fixing his car.
"They're the same, basically. Just more parts on the car. It's a little more challenging, but I love it."
Tyler plans to attend WCTC for Auto Mechanics, go figure. He is excited to be able to pursue mechanics.
"I can't believe I can actually turn what I love to do into my career. It's everybody's dream, and I can actually do it."
By Shawna Burhans
Interview with Teacher Deepika G.
By Saarthak Gupta
Military Brat: Ear to Freedom
By Emily Clifton
Havelock, NC
By Ashley Loroff
Hartland, WI
Falling in and out of love…
By Danielle McConnohie
Nashotah, WI
The infinite sadness of girl, 17
By Rachell Li SILVER
Sydney, Other
Rachell Li SILVER, Sydney, Other

redpajama_set_name: RedPajamaCommonCrawl


There are several neurotransmitters that are responsible for your mood, but Serotonin is the one to study today. The other two, Oxytocin and Dopamine are the others. However, the other two have a somewhat iffy reputation. Dopamine is the high you get from certain addictive behaviors and Oxitocin has a stronger meaning for women than men, with the chemical allowing for mothers to bond better with their newborns.
Amazon - Supporting ZEN commuter never got easier. When you shop you donate.


text:
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Published on July 21, 2017 in Life/WTF by Natalie Dailey
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Published on July 11, 2017 in Against The Politics/Darwin Award/Fail/Life/LOL/Racy/Weird/Win/WTF by Rebecca Travis
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Published on June 14, 2017 in Crime/Disgusting/Life/Racy/WTF by Rebecca Travis
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We play video games for many reasons. Some play as a social hobby. Some play by themselves. Most play for entertainment. However, can playing video games actually have emotional benefits? Some say yes; some say no. Playing video games allows you to understand a bit more about what it is like to be in someone…
We all have these feels, and we may not always know the names for them. Here are words for a
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Published on June 8, 2017 in Life/LOL/Weird by Jenny Mason
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Why France's Presidential Election Is Exciting Even If You Aren't French
By Josh Lowe On 4/18/17 at 1:49 PM EDT
A supporter of far-left candidate Jean-Luc Mélenchon holds a French flag during a rally in Toulouse, Southwestern France, April 16. Regis Duvignau/Reuters
World Marine Le Pen Francois Fillon
There's an election in France! On Sunday! You probably know this. You probably also know that it involves a whole load of Presidential candidates, mostly dark-haired men whose names all end with "-on." And there's a lot of stuff about the EU all mixed up in there.
But here's why you should be paying even more attention. The 2017 French presidential election is probably going to be Europe's most important and exciting poll this year. Here's five reasons to watch closely:
A battle of the extremes
Unlike, say, the U.S. Presidential race, where a politically conventional Democrat went up against a much more unconventional Republican, in France, most of the main candidates are unconventional, and some are pretty extreme.
On the right, there's Marine le Pen, a hardline anti-Islam populist who has promised a moratorium on all immigration and wants to reverse decades of trade liberalizations.
There's also Francois Fillon, candidate for the center-right Republicans. He's the closest the race has to a "normal" candidate but as an admirer of former British Prime Minister Margaret Thatcher who mixes traditionalist social values with a free market economic agenda he's actually pretty unusual in statist France.
And, on the left, both the mainstream Socialist Party candidate Benoit Hamon and Jean-Luc Melenchon are proposing bold redistributive policies, while the former wants a universal basic income and the latter plans bottom-up reform of France's democratic system.
The fight for the center
Whether you think the moderate center ground in politics must be preserved at all costs or you welcome a return to a more combative, ideological political battleground, France's centrist candidate and frontrunner Emmanuel Macron is one to watch.
Macron's politics aren't unconventional : he is offering targeted state spending accompanied by overall budget cuts and an internationalist, pro-EU foreign policy. His ideology is the one that has run the western world for the past couple of decades. But he is interesting because he is making that case without shame even as the rest of his country's politics becomes more protectionist or nationalist.
And Macron is fighting without the support of an established party: his movement, En Marche! (Onwards!) is only a year old.
If Macron storms to victory, it will signal that despite the rise of populism, western electorates still have time for such messages if sold correctly. If he crashes and burns, it will add to the weight of evidence supporting the opposite view.
Russia's watching
Just like in the U.S., there are fears of Russian interference. Le Pen, Melenchon and Fillon are all Vladimir Putin-sympathetic to varying degrees, and the Russian President could benefit from any of them emerging victorious. France's polling commission issued a warning in February over a false Russian news report suggesting conservative candidate Francois Fillon led the race for the presidency.
Meanwhile Macron's campaign says he has been the victim of a series of targeted cyber-attacks. Foreign Minister Jean-Marc Ayrault denounced the interference as "unacceptable" in a February interview.
There is as yet no evidence of Russian meddling, and it may be that the Kremlin isn't playing any direct role in the French political process. But even if that's the case, the election result could be a big boost for Putin, and it's worth paying attention.
Crunch time for Europe
After Brexit, the refugee crisis, the 2015 Greek debt crisis and a host of smaller squabbles, the EU is not at its strongest point right now. But at the same time, it is more resilient than many give it credit for: as it stands, the union is not on the brink of collapse.
But the French election could change the game somewhat. The far-right candidate Marine le Pen is running in second place in the polls. Her platform includes a referendum on France's continued membership of the euro, and she is a strong Euroskeptic. Meanwhile Melenchon, an independent left-winger, is creeping into third place, and wants to renegotiate swathes of EU treaties. Victory for either candidate would bring the EU several steps toward crisis point.
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