Nitrogen hydrides in interstellar gas Herschel/HIFI observations towards G10.6-0.4 (W31C)
| Title | Nitrogen hydrides in interstellar gas Herschel/HIFI observations towards G10.6-0.4 (W31C) |
| Publication Type | Journal Article |
| Year of Publication | 2010 |
| Authors | Persson, CM, Black, JH, Cernicharo, J, Goicoechea, JR, Hassel, GE, Herbst, E, Gerin, M, De Luca, M, Bell, TA, Coutens, A, Falgarone, E, Goldsmith, PF, Gupta, H, Kazmierczak, M, Lis, DC, Mookerjea, B, Neufeld, DA, Pearson, J, Phillips, TG, Sonnentrucker, P, Stutzki, J, Vastel, C, Yu, S, Boulanger, F, Dartois, E, Encrenaz, P, Geballe, TR, Giesen, T, Godard, B, Gry, C, Hennebelle, P, Hily-Blant, P, Joblin, C, Kolos, R, Krelowski, J, Martin-Pintado, J, Menten, K, Monje, R, Perault, M, Plume, R, Salez, M, Schlemmer, S, Schmidt, M, Teyssier, D, Peron, I, Cais, P, Gaufre, P, Cros, A, Ravera, L, Morris, P, Lord, S, Planesas, P |
| Journal | Astronomy & Astrophysics |
| Volume | 521 |
| Date Published | Oct |
| ISBN Number | 0004-6361 |
| Accession Number | WOS:000284150900045 |
| Abstract | The HIFI instrument on board the Herschel Space Observatory has been used to observe interstellar nitrogen hydrides along the sight-line towards G10.6-0.4 in order to improve our understanding of the interstellar chemistry of nitrogen. We report observations of absorption in NH N = 1 <- 0, J = 2 <- 1 and ortho-NH2 1(1,1) <- 0(0,0). We also observed ortho-NH3 1(0) <- 0(0) and 2(0) <- 1(0), para-NH3 2(1) <- 1(1), and searched unsuccessfully for NH+. All detections show emission and absorption associated directly with the hot-core source itself as well as absorption by foreground material over a wide range of velocities. All spectra show similar, non-saturated, absorption features, which we attribute to diffuse molecular gas. Total column densities over the velocity range 11-54 km s(-1) are estimated. The similar profiles suggest fairly uniform abundances relative to hydrogen, approximately 6 x 10(-9), 3 x 10(-9), and 3 x 10(-9) for NH, NH2, and NH3, respectively. These abundances are discussed with reference to models of gas-phase and surface chemistry. |
