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. En-revanche, informent exclusivement sur ce sujet. D'un sens, ce résultat a priori décourageant incite encore plusàplusà l'observation de cette transition On peut même s'attendre, grâcè a la cartographie des sources, ` a l'observation des mouvements de gazàgazà grandé echelle Concernant les raies isotopiques, il appara??tappara??t clairement que leurs détections dépendra fortement de l'abondance de l'isotope principal qui devrâ etre maximale pour l'obtention de résultats probants. Cependant, lespremì eres tentatives de détections depuis le sol sont encourageantes sur ce point (van der Tak et al., 2006) et on peut espérer que les observations futures confirmeront ces résultats. Il conviendraitégalementconviendraitégalement de réduire la résolution spectrale pour l'observation de certaines transitions. En effet, les résultats montrent que les profils s'´ etalent souvent sur de grandes plages de vitesse en montrant des variations sur des intervalles de l'ordre de ? 0.2 ? 1 km·s ?1 . On observe, par exemple, que l'ensemble des informations de la transitionsàtransitionsà 1113 GHz pour la source MM1 de IRAS 18151?1208 est disponible avec une résolution de 1 MHz (contre 0.5 MHz prévu actuellement) et une sensibilité de 100 mK (´ egale au programme actuel, cf. Figure 5.15) Le gain en temps est considérable : ` a sensibilitésensibilitéégale, il passe de 1400 s ` a 530 s. Dans ces conditions, il semble possible de réduire d'un facteur 2 la résolution spectrale de l'ensemble des transitions prévues, en observant tout d'abordàabordà la résolution initiale etàetà sensibilité plus basse (environ 140 mK, atteinte en 800 s environ), puis en lissant les profils d'un facteur 2 obtenus pour re-augmenter la sensibilité jusqu'` a 100 mK. Ainsi, le temps d'observation serait réduit d'un facteur 2, tout en garantissant une observation initiale de grande qualité si le besoin est, ce qui est loin d'? etre négligeable dans le contexte d'une observation spatiale Au final, les questions fondamentales sous-jacentesàjacentesà ce travail

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. B. Fig, ,1 ) et (2 2,0 ? 2 1,1 ) et de son isotope H 34 2 S (1 1,0 ? 1 0,1 ) Les abondances utilisées pour obtenir ces résultats sont respectivement de 3

. B. Fig, 4 ? Modélisation des raies d'´ emission moléculaires du SO (3?2), 5?4), (6?5) et (8 ? 7). Les abondances utilisées pour obtenir ces résultats sont respectivement de

. B. Fig, 14 ? 13 1,13 ) et (18 0,18 ? 17 0,17 ) Les abondances utilisées pour obtenir ces résultats sont respectivement

. B. Fig, Les abondances utilisées pour obtenir ces résultats sont respectivement de 3 ?1 ; pour l'espèce isotopique les abondances utilisées sont, ? 4) et (7?6) et de son isotope C 34 S (3?2) et (7?6)

. B. Fig, 7 ? Modélisation des raies d'´ emission moléculaires du OCS (8 ? 7), (13 ? 12) et (19 ? 18) Les abondances utilisées pour obtenir ces résultats sont respectivement de 3, avec une largeur de turbulencé egalè a 2

. B. Fig, 8 ? Modélisation des raies d'´ emission moléculaires du H 2 S (1 1,0 ? 1 0,1 ) et (2 2,0 ? 2 1,1 ) et de son isotope H 34 2 S (1 1,0 ? 1 0,1 ) Les abondances utilisées pour obtenir ces résultats sont respectivement de 1

. B. Fig, Les abondances utilisées pour obtenir ces résultats sont respectivement de 1, 6?5) et (8 ? 7) et de son isotope 34 SO avec une largeur de turbulencé egalè a 1.6 km·s ?1 ; pour l'espèce isotopique les abondances utilisées sont

. B. Fig, 10 ? Modélisation des raies d'´ emission moléculaires, Les abondances utilisées pour obtenir ces résultats sont respectivement

0. ?10, 0×10 ?10 (limite supérieure pour cettedernì ere valeur) avec une largeur de turbulencé egalè a 1, pp.6-7

B. Annexe, Résultats des modélisations desémissionsdesémissions de molécules soufrées 190

. B. Fig, 11 ? Modélisation des raies d'´ emission moléculaires du CS (3 ? 2) et (5 ? 4) et de son isotope C 34 S (3 ? 2) Les abondances utilisées pour obtenir ces résultats sont respectivement de 5.4×10 ?10 et 2.2×10 ?10 avec une largeur de turbulencé egalèegalè a 2.3 km·s ?1 ; pour l'espèce isotopique l'abondance utilisée

. B. Fig, 12 ? Modélisation des raies d'´ emission moléculaires du OCS (8 ? 7), (13 ? 12) et (19 ? 18) Les abondances utilisées pour obtenir ces résultats sont respectivement de

. B. Fig, 15 ? Modélisation des raies d'´ emission moléculaires du SO 2 (5 1,5 ? 4 0,4 ), (10 0,10 ? 9 1,9 ) et (14 0,14 ? 13 1,13 ) Les abondances utilisées pour obtenir ces résultats sont respectivement de 6

. B. Fig, 13 ? 12) et (19 ? 18) et de son isotope OC 34 S (8 ? 7) Les abondances utilisées pour obtenir ces résultats sont respectivement de 5.2×10 ?9 , 3.3×10 ?9 et 12×10 ?9 avec une largeur de turbulencé egalè a 2.0 km·s ?1 et 2.8 km·s ?1 pour la transition la plus haute enénergieenénergie ; pour l'espèce isotopique l'abondance utilisée est de 4.1×10 ?10, 1977.

. B. Fig, 17 ? Modélisation des raies d'´ emission moléculaires du H 2 S (1 1,0 ? 1 0,1 ) et (2 2,0 ? 2 1,1 ) Les abondances utilisées pour obtenir ces résultats sont respectivement de 3, 0×10 ?10 et 4.0×10 ?10 avec des largeurs de turbulencé egales respectivementàrespectivement`respectivementà 2.8 km·s ?1 et 2.0 km·s ?1 . Un effondrement au bord minimal de ?1.0 km·s ?1 a ´ eté rajouté pour cette source, ´ etendù a l'ensemble du modèle en suivant les résultats de Shu, 1977.

. B. Fig, Les abondances utilisées pour obtenir ces résultats sont respectivement de 25×10 ?10 , 0.9×10 ?10 , 1.0×10 ?10 et 40×10 ?10 avec une largeur de turbulencé egalè a 2.2 km·s ?1 ; pour l'espèce isotopique les abondances utilisées sont respectivement de 6, ? 5) et (8 ? 7) et de son isotope 34 SO (3 ? 2) et, 1977.