Water and ammonia abundances in S140 with the Odin satellite
Journal article, 2009

We investigate the effect of the physical environment on water and ammonia abundances across the S140 photodissociation region (PDR) with an embedded outflow. We used the Odin satellite to obtain strip maps of the ground-state rotational transitions of ortho-water and ortho-ammonia, as well as CO(5-4) and 13co(5-4) across the PDR, and H_2^18O in the central position. A physi-chemical inhomogeneous PDR model was used to compute the temperature and abundance distributions for water, ammonia, and CO. A multi-zone escape probability method then calculated the level populations and intensity distributions. These results are compared to a homogeneous model computed with an enhanced version of the RADEX code. H_2O, NH_3, and ^13CO show emission from an extended PDR with a narrow line width of ~3 km/s. Like CO, the water line profile is dominated by outflow emission, but mainly in the red wing. Even though CO shows strong self-absorption, no signs of self-absorption are seen in the water line. The H_2^18O molecule is not detected. The PDR model suggests that the water emission arises mainly from the surfaces of optically thick, high-density clumps with n(H_2)>10^6 cm^-3 and a clump water abundance, with respect to H_2, of 5*10^-8. The mean water abundance in the PDR is 5*10^-9 and between ~4*10^-8 - 4*10^-7 in the outflow derived from a simple two-level approximation. The RADEX model points to a somewhat higher average PDR water abundance of 1*10^-8. At low temperatures deep in the cloud, the water emission is weaker, likely due to adsorption onto dust grains, while ammonia is still abundant. Ammonia is also observed in the extended clumpy PDR, likely from the same high density and warm clumps as water. The average ammonia abundance is about the same as for water: 4*10^-9 and 8*10^-9 given by the PDR model and RADEX, respectively. The differences between the models most likely arise from uncertainties in density,beam-filling, and volume-filling of clumps. The similarity of water and ammonia PDR emission is also seen in the almost identical line profiles observed close to the bright rim. Around the central position, ammonia also shows some outflow emission, although weaker than water in the red wing. Predictions of the H_2O 1(1,0)-1(0,1) and 1(1,1)-0(0,0) antenna temperatures across the PDR are estimated with our PDR model for the forthcoming observations with the Herschel Space Observatory.


Line: formation

Line: profiles

ISM: molecules

ISM: abundances

ISM: individual (S140)

Radio lines: ISM


Carina Persson

Chalmers, Department of Radio and Space Science, Radio Astronomy and Astrophysics

Michael Olberg

Chalmers, Department of Radio and Space Science, Radio Astronomy and Astrophysics

Åke Hjalmarson

Chalmers, Department of Radio and Space Science, Radio Astronomy and Astrophysics

M. Spaans

University of Groningen

John H Black

Chalmers, Department of Radio and Space Science, Radio Astronomy and Astrophysics

U. Frisk

Swedish Space Corporation (SSC)

T Liljeström

Aalto University

Henrik Olofsson

Chalmers, Department of Radio and Space Science, National Facility for Radio Astronomy

D. R. Poelman

University of St Andrews

Aa. Sandqvist

AlbaNova University Center

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 2 494 637-646

Subject Categories

Astronomy, Astrophysics and Cosmology



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