All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=14.1cm,clip]{8260fig1.ps} \end{figure}$ Figure 1: Observed spectrum towards HH91A obtained with PMAS, with monochromatic fluxes plotted versus wavelength (in $\rm\AA$ ). The positions of the (3, 0) S(1)-S(14) lines are indicated. The (7, 3) S(11) line near 7978 $\rm\AA$ is marginally detected. Model spectra with emission from vibrational levels v'=3 and 7 are color-coded in blue and red, respectively (cf. Sect. 4). The emission near 8727 $\rm\AA$ arises from atomic carbon.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14.1cm,clip]{8260fig2.ps} \end{figure}$ Figure 2: Observed spectrum towards HH91A obtained with PMAS, with monochromatic fluxes (in relative units) plotted versus wavelength (in $\rm\AA$ ). The position of various emission lines in the (3, 0) and (4, 1) bands is indicated. The (8, 4) S(9) and (8, 4) S(11) lines near 8500 $\rm\AA$ and 8685 $\rm\AA$ , respectively, are marginally detected. The emission lines color-coded in blue, green, and red correspond to model spectra with emission from vibrational levels v'=3, 4, and 8, respectively (cf. Sect. 4).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.5cm,clip]{8260fig3.ps} \end{figure}$ Figure 3: J-band spectrum towards HH91A obtained with SOFI. Monochromatic fluxes are plotted in units of 10^-17 W m $^{-2}~\mu$ m^-1 vs. wavelength in units of $\rm\AA$ . The spectrum is dominated by strong emission lines which arise from the (2, 0), (3, 1), and (4, 2) S-branches. Faint emission from various lines in the (6, 3) and (7, 4) S-bands is detected. The positions of the various lines in the (6, 3) S-branch between 9500-10 000 $\rm\AA$ are indicated. The positions of several lines converging to the band-head of the (7, 4) S-branch between 10 030-10 050 $\rm\AA$ are also indicated. The emission near 9825 $\rm\AA$ and 9851 $\rm\AA$ arises from the ¹D₂-³P₁ and ¹D₂-³P₂ transition of [CI]. The theoretical H₂emission spectrum is reproduced in color, with emission from v'=2 and 3 in blue, from v'=4 in green, and from v'=6 and 7 in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.7cm,clip]{8260fig4.ps} \end{figure}$ Figure 4: J-band spectrum towards HH91A, with monochromatic fluxes in units of 10^-17 W m $^{-2}~\mu$ m^-1 vs. wavelength in units of $\rm\AA$ . The strong emission lines which arise from the (2, 0), (3, 1), (4, 2), and (5, 3) bands are identified. The expected position and strength of modeled emission from the (6, 4) S(3)-S(8) lines is also indicated (cf. Sect. 4). The theoretical H₂ emission spectrum is reproduced in color, see Fig. 3 for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.2cm,clip]{8260fig5.ps} \end{figure}$ Figure 5: H-band spectrum towards HH91A, with monochromatic fluxes in units of 10^-17 W m $^{-2}~\mu$ m^-1 vs. wavelength in units of $\rm\AA$ . The emission lines reproduced in color correspond to a model calculation that is presented in Sect. 4. Emission from v'=1, 2, and 3 in blue, v'=4 in green, v'=5 in magenta, and v'=6 and 7 in red. It is noted that emission from [FeII] ${\rm a}^4 {\rm D}_{7/2}- {\rm a}^4 {\rm F}_{9/2}$ near 16 440 $\rm\AA$ is absent.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.7cm,clip]{8260fig6.ps} \end{figure}$ Figure 6: H-band spectrum towards HH91A, see caption of Fig. 5 for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.6cm,clip]{8260fig7.ps} \end{figure}$ Figure 7: Ks-band spectrum towards HH91A obtained with SOFI, see caption of Fig. 5 for details. The wings in the (1, 0) S(1) line arise from an instrumental defect of SOFI and have no astrophysical significance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8260fig8.ps} \end{figure}$ Figure 8: H₂ excitation diagram with values of ${\rm ln} N(v'J')/g$ plotted versus excitation energy E(v'J'). Open triangles represent data points inferred from the column densities N(v'J') listed in Tables 1 and 2. Filled triangles are obtained from a model calculation where the emission arises from a two-component gas model, where the bulk of the material has a total H₂ column density of 1.24 $\times$ 10¹⁸ cm^-2 and is at a temperature of 2750 K, and where a fraction of 10¹⁶ cm^-2 of H₂ is at a temperature of 6000 K.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.2cm,clip]{8260fig9.ps} \end{figure}$ Figure 9: Modeled H₂ emission spectrum that results from a total column of N(H ₂) = 10¹⁸ cm^-2 of hot gas at a temperature of 2750 K, which contains a fraction of 1% of hot gas at 6000 K. Fluxes are in units of 10^-19 W m^-2 and wavelengths are in $\rm\AA$ . Emission lines are Voigt line profiles at a FWHM of 200 $\rm\AA$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9.9cm,clip]{8260fig10.ps} \end{figure}$ Figure 10: Residuals between observed and modeled H₂ spectra as shown in Fig. 1, covering the range of 7760-8160 $\rm\AA$ . The expected positions of the (3, 0) S(1)-S(14) lines are indicated.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9.9cm,clip]{8260fig11.ps} \end{figure}$ Figure 11: Residuals between observed and modeled H₂ spectra as shown in Fig. 2, covering the range of 8390-8820 $\rm\AA$ . The expected positions of various emission lines in the (3, 0) and (4, 1) bands are indicated. The feature near 8510 $\rm\AA$ is a spike and does not correspond to an H₂ emission line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=10.5cm,clip]{8260fig12.ps} \end{figure}$ Figure 12: Residuals between observed and modeled H₂ spectra as shown in Fig. 3, covering the range of 9400-12 800 $\rm\AA$ . The modeled flux in the (3, 1) S(9), S(10), S(11) blend near 11 200 $\rm\AA$ is too high by a factor of about 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=10.6cm,clip]{8260fig13.ps} \end{figure}$ Figure 13: Residuals between observed and modeled H₂ spectra as shown in Fig. 4, covering the range of 12 800-15 000 $\rm\AA$ . The modeled flux in the (3, 1) Q(7) line is too high by a factor of about 2. The spectral region between 13 500-14 500 $\rm\AA$ is characterized by poor atmospheric transmission.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=10.6cm,clip]{8260fig14.ps} \end{figure}$ Figure 14: Residuals between observed and modeled H₂ spectra as shown in Fig. 5, covering the range of 15 000-16 600 $\rm\AA$ . The flux in the (3, 1) O(5) and (2, 0) O(7) lines is too strong by a factor of about 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=10.9cm,clip]{8260fig15.ps} \end{figure}$ Figure 15: Residuals between observed and modeled H₂ spectra as shown in Fig. 6, covering the range of 16 350-18 000 $\rm\AA$ . The line wings in the (1, 0) S(7) and S(8) lines arise from an instrumental defect of SOFI and have no astrophysical significance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=10.4cm,clip]{8260fig16.ps} \end{figure}$ Figure 16: Residuals between observed and modeled H₂ spectra as shown in Fig. 7, covering the range of 20 000-23 000 $\rm\AA$ . The broad line wings in the (1, 0) S(1) line arise from an instrumental defect of SOFI.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.7cm,clip]{8260fig6.ps} \end{figure}$	Figure 6: H-band spectrum towards HH91A, see caption of Fig. 5 for details.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=15.6cm,clip]{8260fig7.ps} \end{figure}$	Figure 7: Ks-band spectrum towards HH91A obtained with SOFI, see caption of Fig. 5 for details. The wings in the (1, 0) S(1) line arise from an instrumental defect of SOFI and have no astrophysical significance.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=15.2cm,clip]{8260fig9.ps} \end{figure}$	Figure 9: Modeled H₂ emission spectrum that results from a total column of N(H ₂) = 10¹⁸ cm^-2 of hot gas at a temperature of 2750 K, which contains a fraction of 1% of hot gas at 6000 K. Fluxes are in units of 10^-19 W m^-2 and wavelengths are in $\rm\AA$ . Emission lines are Voigt line profiles at a FWHM of 200 $\rm\AA$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=9.9cm,clip]{8260fig10.ps} \end{figure}$	Figure 10: Residuals between observed and modeled H₂ spectra as shown in Fig. 1, covering the range of 7760-8160 $\rm\AA$ . The expected positions of the (3, 0) S(1)-S(14) lines are indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=9.9cm,clip]{8260fig11.ps} \end{figure}$	Figure 11: Residuals between observed and modeled H₂ spectra as shown in Fig. 2, covering the range of 8390-8820 $\rm\AA$ . The expected positions of various emission lines in the (3, 0) and (4, 1) bands are indicated. The feature near 8510 $\rm\AA$ is a spike and does not correspond to an H₂ emission line.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=10.5cm,clip]{8260fig12.ps} \end{figure}$	Figure 12: Residuals between observed and modeled H₂ spectra as shown in Fig. 3, covering the range of 9400-12 800 $\rm\AA$ . The modeled flux in the (3, 1) S(9), S(10), S(11) blend near 11 200 $\rm\AA$ is too high by a factor of about 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=10.6cm,clip]{8260fig13.ps} \end{figure}$	Figure 13: Residuals between observed and modeled H₂ spectra as shown in Fig. 4, covering the range of 12 800-15 000 $\rm\AA$ . The modeled flux in the (3, 1) Q(7) line is too high by a factor of about 2. The spectral region between 13 500-14 500 $\rm\AA$ is characterized by poor atmospheric transmission.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=10.6cm,clip]{8260fig14.ps} \end{figure}$	Figure 14: Residuals between observed and modeled H₂ spectra as shown in Fig. 5, covering the range of 15 000-16 600 $\rm\AA$ . The flux in the (3, 1) O(5) and (2, 0) O(7) lines is too strong by a factor of about 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=10.9cm,clip]{8260fig15.ps} \end{figure}$	Figure 15: Residuals between observed and modeled H₂ spectra as shown in Fig. 6, covering the range of 16 350-18 000 $\rm\AA$ . The line wings in the (1, 0) S(7) and S(8) lines arise from an instrumental defect of SOFI and have no astrophysical significance.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=10.4cm,clip]{8260fig16.ps} \end{figure}$	Figure 16: Residuals between observed and modeled H₂ spectra as shown in Fig. 7, covering the range of 20 000-23 000 $\rm\AA$ . The broad line wings in the (1, 0) S(1) line arise from an instrumental defect of SOFI.
Open with DEXTER