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URL : https://hal.archives-ouvertes.fr/halshs-00261856

, Image composite en trois couleurs, bleu, vert, IR, obtenus avec les instruments ANTU et FORS1 au VLT au petit matin du 27 mars 1999. Le champ mesure 6.8×6.8' 2 . Crédit : ESO

, Courbes d'extinction pour 2.4<R V <3.6. Les zones grisées montrent la variance des courbes en fonction de la longueur d'onde. (Source : FITZPATRICK et MASSA, 2007.

, Albédos mesurés pour le milieu diffus (noir) et des milieux denses (rouge et bleu)

, )) sont tacés (lignes) pour aider la lecture, Les albédos prédits pour différentes populations de grains par le modèle THEMIS, 2015.

, Spectres illustrant l'absorption IR de sources en direction du centre galactique. Certaines signatures sont associées aux a-C :H (HAC) dans le milieu diffus, d'autres le sont aux glaces présentes dans les nuages moléculaires. (Source : TIELENS 2005; Fig. 5.8)

, Bandes interstellaires diffuses (DIB) dans la région 550-667 nm. L'extinction est normalisée à celle de la bande I. (Source : DRAINE 2003; Fig. 5)

, Les données d'observation viennent des spectres ?5-15 µm ISOCAM/CVF d'ISO et ?100-1000 µm de FIRAS/COBE, de la mesure AROME à 3.3 µm en bande étroite (triangle) et de la photométrie DIRBE/COBE (carrés), 2011.

I. Spectres and . Dans-l&apos;ir, Les spectres sont ceux de la protonébuleuse planétaire du Rectangle Rouge (HD 44179), de la nébuleuse planétaire NGC 7027 et deux positions dans la nébuleuse diffuse d'Orion. (Source : BOERSMA 2009; Fig. 1.1)

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. Van-diedenhoven, Variations de position et de profils des bandes IR. Les signatures à 3 µm et à 10-15 µm ne montrent que des variations mineures, contrairement à la gamme 6-9 µm. (Source : TIELENS, vol.18, 2004.

, Source : SELLGREN et al. 2010; Fig. 1). (b) Spectres à 3 µm de Elias 1 et HD 97048 montrant les signatures des diamants à 3.43 et 3.53 µm. Les spectres des mesures de laboratoires sur nano-cristaux de diamants sont aussi tracés. (Source : GUILLOIS et al. 1999; Fig. 2), Spitzer entre 5 et 20 µm de NGC 7023 et NGC 2023 montrant les signatures des fullerènes. Leurs positions à 7.0, 8.5, 17.4 et 18.9 µm sont indiquées par les traits mauves

, Les spectres de la comète Hale-Bopp (en bas à gauche) montre aussi les signatures de silicates cristallins. Les spectres de la forsterite et de l'enstatite présentent des signatures permettant d'expliquer celles observées, Spectres moyen IR d'environnements où sont observés les silicates cristallins : étoile jeune Herbig (en haut à gauche), 2005.

, Milieu : température de la poussière observée, T obs , à une résolution de 5'. Droite : indice spectral de poussière observé, ? obs , à une résolution de 30'. La figure est adaptée de PLANCK COLLABORATION, Cartes du ciel complet des paramètres issus de l'ajustement des données Planck à 353, 545 et 857 GHz et IRAS à 100 µm par un corps noir modifié, 2014.

. Schmidt, Le trait fin représente le spectre de son étoile centrale HD 44179, normalisé à 5000Å. La figure est adaptée de GODARD, 1980.

. .. , Carte Planck de la polarisation en émission dans le sub-millimétrique. Les lignes de champs magnétiques sont en sur-impression. (Crédit : Planck collaboration), p.22

, ERE (orange), bandes IR et émission thermique (rouge), émission de freinage (free-free) et synchrontron (vert) et AME (orange). L'énergie absorbée par la poussière est en bleu barré. L'encart montre la fraction de la lumière polarisée. (Source : GALLIANO et al. 2018; Fig. 1), Les principales sources d'émission et la partie du spectre associée sont représentées : étoiles (bleu), gaz (vert)

, Source de l'image : Wikipédia)

, Les formes allotropiques de la matière carbonée.(Source des images : EHRENFREUND et CHARNLEY (2000)

, oléfinique (jaune), aliphatique (vert), Représentation des types de liaisons dans la matière carbonée : aromatique (rouge)

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. .. , Représentation des structures amorphes (gauche) et cristallines (droite) des silicates. (La figure est adaptée de MOLSTER et KEMPER 2005; Fig. 1), p.27

, Représentation schématique des manteaux de glaces sur les grains à travers différentes phases denses et illustrant les processus physiques et chimiques à la surface des grains. Les phases 3 à 6 pourraient être celles des conditions dans les enveloppes et les disques autour des YSO. La taille des grains et l'épaisseur des manteaux sont nanométriques. (Source : BOOGERT et al. 2015; Fig. 10)

. .. , Niveaux énergétiques moléculaires aux fréquences (ou énergies) des différents domaines spectraux de photons. (Source : HUMBERT et al. 2012; Fig. 1), p.29

, Spectres d'absortpion IR pour trois échantillions de nano'particules (suies) produites en laboaratoire, des plus aromatiques (sample 1), aux plus aliphatiques

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