Peer-Reviewed Journal Details
Mandatory Fields
Comito, C;Schilke, P;Rolffs, R;Lis, DC;Belloche, A;Bergin, EA;Phillips, TG;Bell, TA;Crockett, NR;Wang, S;Blake, GA;Caux, E;Ceccarelli, C;Cernicharo, J;Daniel, F;Dubernet, ML;Emprechtinger, M;Encrenaz, P;Gerin, M;Giesen, TF;Goicoechea, JR;Goldsmith, PF;Gupta, H;Herbst, E;Joblin, C;Johnstone, D;Langer, WD;Latter, WD;Lord, SD;Maret, S;Martin, PG;Melnick, GJ;Menten, KM;Morris, P;Muller, HSP;Murphy, JA;Neufeld, DA;Ossenkopf, V;Pearson, JC;Perault, M;Plume, R;Qin, SL;Schlemmer, S;Stutzki, J;Trappe, N;van der Tak, FFS;Vastel, C;Yorke, HW;Yu, S;Olberg, M;Szczerba, R;Larsson, B;Liseau, R;Lin, RH;Samoska, LA;Schlecht, E
2010
October
Astronomy and Astrophysics
Herschel observations of deuterated water towards Sgr B2(M)
Published
6 ()
Optional Fields
LINE OBSERVATIONS HOT CORES SAGITTARIUS-B2 SUBMILLIMETER EXCITATION ASTRONOMY VAPOR BAND
521
Observations of HDO are an important complement for studies of water, because they give strong constraints on the formation processes - grain surfaces versus energetic process in the gas phase, e. g. in shocks. The HIFI observations of multiple transitions of HDO in Sgr B2(M) presented here allow the determination of the HDO abundance throughout the envelope, which has not been possible before with ground-based observations only. The abundance structure has been modeled with the spherical Monte Carlo radiative transfer code RATRAN, which also takes radiative pumping by continuum emission from dust into account. The modeling reveals that the abundance of HDO rises steeply with temperature from a low abundance (2.5 x 10(-11)) in the outer envelope at temperatures below 100 K through a medium abundance (1.5 x 10(-9)) in the inner envelope/outer core at temperatures between 100 and 200 K, and finally a high abundance (3.5 x 10(-9)) at temperatures above 200 K in the hot core.
LES ULIS CEDEX A
0004-6361
10.1051/0004-6361/201015121
Grant Details