All Figures

	Figure 1: NIR broad-band ( filter) acquisition image of M1-78. The positions of the NIR slits (in red slit #1 with a PA of 50, and in cyan slit #2 with a PA of 140) are marked. The (0 , 0 ) position corresponds to RA = 212044.91 and Dec = (J2000.0). The H2 regions analysed in Sect. 4.7 are indicated. At a distance of 8.9 kpc, 1  corresponds to 0.043 pc.
Open with DEXTER


In the text

Figure 2: Red range of the optical spectra extracted from a slit position coincident with slit #1 of the NIR observations (see Fig. 1). The upper panel corresponds to the emission of the NE blob; the inset show an enlargment of the spectral area around the [N II] 5755 Å and He I 5876 Å lines. The middle and the lower panels show the red spectrum of the SW arc at different line-flux levels. The fluxes are not corrected for reddening. The identification of most emission lines and absorption features is indicated. The broad absorption features longward 6800 Å are due to the atmosphere.

Open with DEXTER


In the text

Figure 3: ( Left) Spectra of M1-78 extracted across ( top) slit #1 between -7 5 and 0 and ( bottom) slit #2 between -2 and 2 (see Fig. 1). The observed lines, their identification and their line fluxes are listed in Table 3. ( Right) Spectra extracted across slit #1 from 0 75  0 75 regions around the continua detected within the NE blob ( top) and the SW arc ( bottom). Note the logarithmic scale of the flux axis.

Open with DEXTER


In the text

Figure 4: ( Left) Spatial variation of Br and the two strongest He I lines at 2.058 and 2.112 m across slit #1 ( left) and slit #2 ( right). The normalized He I intensity distributions are compared to the Br profile (dashed line). ( Right) Spatial variation of the H2 1-0 S(1) transition at 2.121 m across slit #1 ( top) and slit #2 ( bottom) compared to the Br profile (dashed line). The different regions analysed in the text are identified (dotted lines). The origin corresponds to the (0 , 0 ) position of Fig. 1.

Open with DEXTER


In the text

	Figure 5: Spatial variation of the [Ne II] 12.8 m fine-structure line (solid line) and the 12 m dust continuum (dashed line) obtained with the mid-infrared spectrograph SpectroCam-10 mounted on the 5 m Hale Telescope at Palomar Observatory. These variations correspond to a 1   16 4 slit positioned along the same axis of our slit #1. We show the Br variation (dotted line) for comparison.
Open with DEXTER


In the text

Figure 6: Plot of the He I 2.112 43,1S-33,1P/2.161 73,1F-43,1D ratio against the He I 2.042 63P-43S/2.112 43,1S-33,1P ratio. Ratios measured for slit #1 are plotted by a black square, and by a black triangle for slit #2. The open triangles represent the theoretical predictions using the J-resolved code of Bauman et al. (2005) for 5000 K, 8000 K, 10 000 K and 12 500 K. Similarly, the open circles represent the predictions of Benjamin et al. (1999) for the same electron temperatures and three values of : 0, 10 and 100.

Open with DEXTER


In the text

	Figure 7: K-band [Fe III] line ratios. We show the theoretical predictions of Keenan et al. (2001) (dotted line) and Rodríguez (2002) (dashed line) for densities between log  and log  . The black square and triangle represent the line ratios measured for slit #1 and slit #2, respectively.
Open with DEXTER


In the text

	Figure 8: H2 excitation diagrams for each region. The lines represents the best fitting purely thermal single-temperature models. The solid line is the fit to the v=1 level only and the dotted line is the fit to all the data except the v=3 level.
Open with DEXTER


In the text