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<!-- DOI: 10.1051/0004-6361/200912408 -->

<h2 class="sec">Online Material</h2>

<p></p><h2 class="sec"><a name="SECTION000100000000000000000"></a>
Appendix A: Physical structure of previously analysed jets
</h2>

<p>In this appendix we present the results obtained by 
applying spectral diagnostics to HH&nbsp;1 (jet and bow), HH&nbsp;2, HH 83, and HH 24.
These jets have been already analysed in previous papers with the same
diagnostics, but are re-analysed here with higher spatial sampling
(
<!-- MATH: $\Delta x \sim 1.2$ -->
<IMG SRC="img73.png" ALT="$\Delta x \sim 1.2$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="54">
<!-- MATH: $^{\prime\prime}$ -->
<IMG SRC="img18.png" ALT="$^{\prime\prime}$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="10">)
and an improved version of the diagnostic code 
as explained in Sect.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#sect:diag">3</a>. 
The values presented are used for investigating dust reprocessing 
in these jets (see Sect.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#sect:dust">5</a>).

</p><p></p><h3 class="sec2"><a name="SECTION000101000000000000000"></a><A NAME="sect:hh1"></A>
A.1 HH 1/2: the jet and its terminal bows
</h3>

<p>The physical structure of the HH 1 jets and its terminal bows has been 
previously analysed by <A NAME="aaref52"></A><a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#solf91">Solf &amp; B&#xf6;hm (1991)</a>, <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#nisini05">Nisini et&nbsp;al. (2005)</a>, and 
<A NAME="aaref12"></A><a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bohm85">B&#xf6;hm &amp; Solf (1985)</a>, <A NAME="aaref53"></A><a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#solf88">Solf et&nbsp;al. (1988)</a>, <A NAME="aaref18"></A><a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#eisloffel94">Eisl&#xf6;ffel et&nbsp;al. (1994)</a>, <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bally02">Bally et&nbsp;al. (2002)</a>.
In our observations the slit is aligned along the jet and it covers the fainter
western/eastern parts of HH&nbsp;1 and HH&nbsp;2 respectively, 
i.e. the knots&nbsp;B and&nbsp;G, which are located to the west of the
HH&nbsp;1 bow apex (knot F), and the knots&nbsp;L, J, G, B, T, and&nbsp;Q 
located to the east of the bright H and A knots in HH&nbsp;2.

</p><p>The results obtained by applying the BE technique to the HH&nbsp;1 jet are shown in
Fig.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#hh1_phys">A.1</a>. 
The values for the physical parameters are in a good agreement with the ones 
obtained in <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#nisini05">Nisini et&nbsp;al. (2005)</a> but here the spatial sampling is two times better.

</p><p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="hh1_phys"></A><!-- end Label--><A NAME="1009"></A><A NAME="figure882" HREF="img74.png"><IMG SRC="Timg74.png" ALT="\begin{figure}
\par\includegraphics[width=8.cm]{12408fA1.eps}
\end{figure}" HEIGHT="132" WIDTH="86"></A><!-- HTML Figure number: 9 --></td>
<td class="img-txt"><span class="bold">Figure A.1:</span><p>
Variation of the physical parameters for the HH&nbsp;1 jet as a 
function of distance from the source.
<i> From top to bottom panel</i>: 
intensity profiles of the optical lines, the electron density, <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">,
in units
of 10<sup>3</sup>&nbsp;cm<sup>-3</sup>, the ionisation fraction, <IMG SRC="img3.png" ALT="$x_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">,
the temperature, <IMG SRC="img4.png" ALT="$T_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">,
in units
of 10<sup>4</sup>&nbsp;K, and the total density, <IMG SRC="img5.png" ALT="$n_{\rm H}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="18">,
in units of 10<sup>4</sup>&nbsp;cm<sup>-3</sup>.</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=9&DOI=10.1051/0004-6361/200912408" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="bow1_2_phys"></A><!-- end Label--><A NAME="1010"></A><A NAME="figure888" HREF="img75.png"><IMG SRC="Timg75.png" ALT="\begin{figure}
\par\includegraphics[width=13cm]{12408fA2.eps}
\end{figure}" HEIGHT="114" WIDTH="143"></A><!-- HTML Figure number: 10 --></td>
<td class="img-txt"><span class="bold">Figure A.2:</span><p>
Analysis of the excitation conditions in the HH&nbsp;1 jet and its
terminal bows HH&nbsp;1 and HH&nbsp;2 as a 
function of distance from the source.
<i> From top to bottom panel</i>: 
intensity profiles of the optical lines, 
the electron density, <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">,
in units of 10<sup>3</sup>&nbsp;cm<sup>-3</sup>, 
and the [N  <small>II</small>]/[O  <small>I</small>]&nbsp;ratio.</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=10&DOI=10.1051/0004-6361/200912408" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p>We could not apply the diagnostic to the terminal bows.
The BE technique, in fact, relies on the assumption of low excitation
conditions, i.e. S being totally ionised but there is no&nbsp;S<sup>++</sup>, and oxygen 
and nitrogen are ionised at most once (<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bacciotti99">Bacciotti &amp; Eisl&#xf6;ffel  1999</a>).
This assumption is satisfied for the jet where gas interacts
with material already in motion from previous outflow events, 
but may not be correct when dealing with the terminal bows.
This picture is confirmed by proper motions studies by <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bally02">Bally et&nbsp;al. (2002)</a> which
indicate shock velocities lower than 30&nbsp;km&nbsp;s<sup>-1</sup>&nbsp; in the jet and velocity 
jumps of up to 100-200&nbsp;km&nbsp;s<sup>-1</sup>&nbsp; in the bows.
Moreover,  <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bohm85">B&#xf6;hm &amp; Solf (1985)</a> and <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#solf88">Solf et&nbsp;al. (1988)</a> detected many
high excitation lines in HH&nbsp;1 and HH&nbsp;2 such as O<sup>++</sup>, S<sup>++</sup>, 
and&nbsp;Ar<sup>+++</sup>.

</p><p>Even if in our case the slit covers the lateral part of the bows
the excitation conditions may still be too high.
This is indicated by the detection of the high excitation [Ar  <small>III</small>]<IMG SRC="img1.png" ALT="$\lambda $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">7135.8 
line in our spectra and by the fact that the [N  <small>II</small>]&nbsp;lines, 
which are faint in the jet, show strong emission in the bows, 
comparable to the [S  <small>II</small>]&nbsp;lines (see the upper panel of Fig.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bow1_2_phys">A.2</a>).

</p><p>In order to compare the physical conditions in the jet and in the bows 
we computed the electron density, <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">,
and the [N  <small>II</small>]/[O  <small>I</small>]&nbsp; ratio along all the slit length.
The electron density does not show large differences.
It varies between 0.05-
<!-- MATH: $4\times 10^3$ -->
<IMG SRC="img7.png" ALT="$4\times 10^3$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="45">&nbsp;cm<sup>-3</sup>&nbsp; along all the jet.
While in the jet <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">&nbsp; is decreasing with distance from the source, 
both in the HH&nbsp;1 and in HH&nbsp;2 bows, on the contrary, 
there is a decreasing trend going from the shock apex toward the source.
This is expected behind a shock front and confirms the results found by
<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bohm85">B&#xf6;hm &amp; Solf (1985)</a> and <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#solf88">Solf et&nbsp;al. (1988)</a>.
Our values of <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">&nbsp; are lower than those inferred by <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bohm85">B&#xf6;hm &amp; Solf (1985)</a>, however,
because of the different slit alignment (on the brightest spots at the apex 
of HH&nbsp;1 and HH&nbsp;2 for <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bohm85">B&#xf6;hm &amp; Solf 1985</a>, and on the bows wings in our case)
and show that the density in the two bows is maximum at the apex and 
fades towards the wings.
The [N  <small>II</small>]/[O  <small>I</small>]&nbsp; ratio is a good indicator of excitation conditions and, 
in particular, of the ionisation state of the gas.
Figure&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bow1_2_phys">A.2</a> shows that [N  <small>II</small>]/[O  <small>I</small>]&nbsp; is &lt;1 in the jet 
and in knot L, while it is &gt;1 in the HH&nbsp;1 and HH&nbsp;2 bows, indicating
that the excitation level is much higher in the bows, and a higher value of
<IMG SRC="img3.png" ALT="$x_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">&nbsp; is expected.

</p><p></p><h3 class="sec2"><a name="SECTION000102000000000000000"></a><A NAME="sect:hh83"></A>
A.2 HH 83: the physical structure of the inner knots
</h3>

<p>The physical structure of the HH 83 jet has been already derived in 
<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#podio06">Podio et&nbsp;al. (2006)</a>.
Thanks to the high&nbsp;S/N of these data, however, we obtained a
sampling which is four times larger in comparison to previous results.
Moreover the good quality of the data, which allowed us to properly 
subtract the continuum emission from the reflection nebula 
Re&nbsp;17 (<A NAME="aaref49"></A><a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#rolph90">Rolph et&nbsp;al.  1990</a>),
and the use of the improved diagnostic code
allowed us to estimate the
gas physical conditions in the inner part of the jet, where emission from the
[N  <small>II</small>]&nbsp;lines is comparable to the [S  <small>II</small>]&nbsp; and [O  <small>I</small>]&nbsp;emission.

</p><p>The derived parameters, shown in Fig.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#hh83_phys">A.3</a>, indicate that the excitation conditions are very high
in the knots close to the source (knots from&nbsp;A to&nbsp;D) 
with <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">&nbsp;<IMG SRC="img15.png" ALT="$\sim$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">&nbsp;400-700&nbsp;cm<sup>-3</sup>, and high values of the ionisation fraction
and temperature (<IMG SRC="img3.png" ALT="$x_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">&nbsp;<IMG SRC="img15.png" ALT="$\sim$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">&nbsp;0.4-0.7, and <IMG SRC="img4.png" ALT="$T_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">&nbsp;<IMG SRC="img15.png" ALT="$\sim$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">&nbsp;1.5-
<!-- MATH: $2\times 10^4$ -->
<IMG SRC="img47.png" ALT="$2\times 10^4$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="45">&nbsp;K).

</p><p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="hh83_phys"></A><!-- end Label--><A NAME="1011"></A><A NAME="figure915" HREF="img76.png"><IMG SRC="Timg76.png" ALT="\begin{figure}
\par\includegraphics[width=6.5cm]{12408fA3.eps}
\end{figure}" HEIGHT="113" WIDTH="73"></A><!-- HTML Figure number: 11 --></td>
<td class="img-txt"><span class="bold">Figure A.3:</span><p>
Variation of the physical parameters for the HH&nbsp;83 jet as a 
function of distance from the source.
<i> From top to bottom panel</i>: 
intensity profiles of the optical lines, the electron density, <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">,
in units
of 10<sup>3</sup>&nbsp;cm<sup>-3</sup>, the ionisation fraction, <IMG SRC="img3.png" ALT="$x_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">,
the temperature, <IMG SRC="img4.png" ALT="$T_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">,
in units
of 10<sup>4</sup>&nbsp;K, and the total density, <IMG SRC="img5.png" ALT="$n_{\rm H}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="18">,
in units of 10<sup>3</sup>&nbsp;cm<sup>-3</sup>.</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=11&DOI=10.1051/0004-6361/200912408" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>  

<p></p><h3 class="sec2"><a name="SECTION000103000000000000000"></a><A NAME="sect:hh24"></A>
A.3 The HH 24 jets
</h3>

<p>The physical parameters along the jets HH 24 C, E, and A, have already been
derived in <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#bacciotti99">Bacciotti &amp; Eisl&#xf6;ffel (1999)</a> and <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#podio06">Podio et&nbsp;al. (2006)</a>. 
In our observations the slit has been aligned along the axis HH&nbsp;24 M-A-E and
thus only partially covers the knots of the HH&nbsp;24&nbsp;C jet up to&nbsp;40
<!-- MATH: $\hbox{$^{\prime\prime}$ }$ -->
<IMG SRC="img17.png" ALT="$\hbox{$^{\prime\prime}$ }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="15">
(knot&nbsp;C6).
This is why the line profiles in the upper panel of 
Fig.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#hh24_phys">A.4</a> show fainter emission in the knots of group&nbsp;C, 
contrary to what was found in <a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#podio06">Podio et&nbsp;al. (2006)</a>, where the slit was aligned
along the HH&nbsp;24&nbsp;C jet.  
The variation of the physical parameters obtained by applying the BE&nbsp;technique
is shown in Fig.&nbsp;<a href="/articles/aa/full_html/2009/41/aa12408-09/aa12408-09.html#hh24_phys">A.4</a>.
The sampling is improved by around one third with respect to previous analyses 
(<A NAME="tex2html103" HREF="#bacciotti99">Bacciotti &amp; Eisl&#xf6;ffel  1999</A>; <A NAME="tex2html104" HREF="#podio06">Podio et&nbsp;al.  2006</A>) 
allowing us to highlight the different excitation conditions in the
various groups of knots detected in the HH&nbsp;24 complex 
(HH&nbsp;24&nbsp;A, HH&nbsp;24&nbsp;M/E, and HH&nbsp;24&nbsp;C) 
and supporting the idea that these knots may belong to different jets. 
</p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="hh24_phys"></A><!-- end Label--><A NAME="1012"></A><A NAME="figure930" HREF="img77.png"><IMG SRC="Timg77.png" ALT="\begin{figure}
\par\includegraphics[width=13cm]{12408fA4.eps}
\end{figure}" HEIGHT="109" WIDTH="145"></A><!-- HTML Figure number: 12 --></td>
<td class="img-txt"><span class="bold">Figure A.4:</span><p>
Variation of the physical parameters for the HH&nbsp;24&nbsp;C/E jet as a 
function of distance from the source.
<i> From top to bottom panel</i>: 
intensity profiles of the optical lines, the electron density, <IMG SRC="img2.png" ALT="$n_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="15">,
in units
of 10<sup>3</sup>&nbsp;cm<sup>-3</sup>, the ionisation fraction, <IMG SRC="img3.png" ALT="$x_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">,
the temperature, <IMG SRC="img4.png" ALT="$T_{\rm e}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="16">,
in units
of 10<sup>4</sup>&nbsp;K, and the total density, <IMG SRC="img5.png" ALT="$n_{\rm H}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="18">,
in units of 10<sup>4</sup>&nbsp;cm<sup>-3</sup>.</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=12&DOI=10.1051/0004-6361/200912408" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div>
<p></p><p></p>
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