Volume 527, March 2011
|Number of page(s)||16|
|Section||Interstellar and circumstellar matter|
|Published online||08 February 2011|
Figure A.1 shows maps in the H2 0–0 S(0) line emission at 28.2 μm obtained with the IRS long-low module towards N7023E, the Horsehead, rho Oph, and N2023N. Maps in the H2 0–0 S(1) line emission at 17.03 μm are presented in Fig. 3. Figure A.2 shows maps in the H2 0–0 S(2) and S(3) lines emission at 12.29 and 9.66 μm obtained with the IRS short-low module towards the Horsehead. Projection onto the same spatial grid (2.5″/pixel) and convolution into the same beam (Gaussian with a full width high maximum of 10.7″) were performed to compare the different line maps obtained. There is a good agreement in the intensity distribution between the H2 lines. The same substructures are present in the maps. The emission in the lowest rotational line 0–0 S(0) is somewhat more extended and peaks more inside the nebula. This is easily to understand since the upper state of this line is relatively low-lying. The signal-to-noise ratio in the 0–0 S(0) line maps is lower than in the other line maps since this line is fainter. Towards the Horsehead, the spatial distribution of the excited 0–0 S(2) and S(3) lines is comparable. The 0–0 S(3) line is slighlty shifted nearer the edge.
Map of the H2 0–0 S(0) emission line obtained with the IRS low spectral resolution mode. The black boxes show the region where the spectra of Fig. 1 have been averaged.
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Map of the H2 0–0 S(2) and S(3) emission line obtained with the IRS low spectral resolution mode towards the Horsehead nebula. The black boxes show the region where the spectra of Fig. 1 have been averaged.
|Open with DEXTER|
© ESO, 2011
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