M. Emprechtinger, D. Lis, P. Schilke, R. Rolffs, R. Monje, The Chess Team

NGC 6334 I D=1.7 kpc M=200 M  Four embedded cores with 3-60 M  SMA 1 and SMA 2 emit rich and complex spectra 1.3 mm continuum taken from Hunter et al. 2006

HIFI Observations All Bands except 6a have been observed Emission lines of ~35 molecules + isotopologues identified Strong CH 3 -O-CH 3 and methanol lines.

Water in NGC6334 I H 2 16 O: 16 lines detected. 8 lines of p-H 2 O and 8 lines of o-H 2 O. E lower = K. 6 H 2 18 O lines (3 ground state transition+ 3 excited lines) 6 H 2 17 O lines (3 ground state transition+ 3 excited lines) Four HDO lines ( in absorption + 3 emission lines.  In total 32 lines of water detected.

Individual Components Main component: v lsr =6-8 km/s, FWHM= 5 km/s Foreground 0, +6 and +8 km/s, seen in H 2 16 O ground state transitions. Two outflow components (broad and narrow outflow)

Foreground Components Cold foreground(?): T ex of o-H 2 O = 6.5K.  excitation has to be considered for H 2 O Using HF to determine the H 2 column density of FG clouds x(H 2 O)=5x in agreement with models. Previously reported o/p ratio of 2, based on the H 2 O & line is too low. Including H 2 O leads to o/p ratio of 3

Outflow: Broad outflow H 2 17 O H 2 18 O H 2 16 O H 2 17 O HDO H 2 16 O is optically very thick (τ>300); only a small fraction (15%) of the continuum subject to absorption. x(H 2 O)=4x10 -5, based on H 2 18 O & CO data. Desorption of water ice by sputtering. H 2 18 O/H 2 17 O = 3.7(0.6) (= elemental 18 O/ 17 O ration) HDO/H 2 O=2x10 -4 Abundances agree with predictions of warm (>100 K) gas.

Outflow: Narrow outflow  Narrow outflow as not been detected so far  Narrow outflow detected in excited lines.  Hot outflow is optically thick (  =2.5-80).  Model with LVG code (Radex): T kin =100 K n=3e7 cm

Dense Cores: H 2 16 O Hot Core lines: E up >400 K v LSR =-8.1 km/s (most likely associated with SMA 2) Five “hot core” lines detected. All but one show potential maser activity.

Dense Cores: Rare isotopologues  Dense core lines identified by velocity (-8.1 km/s), all excited lines of H 2 18 O, H 2 17 O, and HDO are coming from the dense core  H 2 18 O/H 2 17 O=1.2-2 ⇒  (H 2 17 O)=  H 2 18 O much weaker than corresponding H 2 16 O line ⇒ Dense core is embedded in lower density envelope. H 2 18 O H 2 17 O

Dense Cores: Rare isotopologues Modeling lines assuming LTE (XCLASS), assuming a source size of 4’’ Isotop.Temp.Col. Density H 2 18 O43 K3.6 x cm -2 H 2 17 O50 K8 x cm -2 HDO50 K4 x cm -2  Comparing H 2 18 O column density with core mass results in x(H 2 O)=10 -6, 100 times lower than expected.  HDO/H 2 O=3x10 -4 similar to the value found in the outflow.

Ratran Model  Source model based on the model by Rolffs et al Power-law density density and self consistent temperature profile.  Non spherical outflow feature which covers parts of the source is added.  Water abundances of 3 x (T 100 K).  Outflow:T kin = K n=1e5 cm -3

Ratran Model-Para H 2 O

Ratran Model-Ortho H 2 O

Summary  H 2 O abundance in cold gas and outflow as predicted by chemical models. In hot cores the water abundance is by a factor 100 to low.  Ortho/Para ratio is everywhere close to the statistical value of three.  Second narrow outflow component was detected.  H 2 18 O and H 2 17 O abundances are as expected from 18 O and 17 O abundances.  HDO/H 2 O = in the outflow and the hot core. Almost all water we see is formed in warm gas.