TY - JOUR
T1 - Warm water deuterium fractionation in IRAS 16293-2422
T2 - the high-resolution ALMA and SMA view
AU - Persson, Magnus Vilhelm
AU - Jørgensen, Jes Kristian
AU - van Dishoeck, E. F.
PY - 2012
Y1 - 2012
N2 - Context. Measuring the water deuterium fractionation in the inner warm regions of low-mass protostars has so far been hampered by poor angular resolution obtainable with single-dish ground- and space-based telescopes. Observations of water isotopologues using (sub)millimeter wavelength interferometers have the potential to shed light on this matter. Aims. To measure the water deuterium fractionation in the warm gas of the deeply-embedded protostellar binary IRAS16293-2422. Methods. Observations toward IRAS16293-2422 of the 53,2-44,1 transition of H2 18O at 692.07914GHz from Atacama Large Millimeter/submillimeter Array (ALMA) as well as the 31,3-22,0 of H2 18O at 203.40752GHz and the 31,2-22,1 transition of HDO at 225.89672GHz from the Submillimeter Array (SMA) are presented. Results. The 692GHz H2 18O line is seen toward both components of the binary protostar. Toward one of the components, "sourceB", the line is seen in absorption toward the continuum, slightly red-shifted from the systemic velocity, whereas emission is seen off-source at the systemic velocity. Toward the other component, "sourceA", the two HDO and H2 18O lines are detected as well with the SMA. From the H2 18O transitions the excitation temperature is estimated at 124±12K. The calculated HDO/H2O ratio is (9.2±2.6)×10-4 - significantly lower than previous estimates in the warm gas close to the source. It is also lower by a factor of ∼5 than the ratio deduced in the outer envelope. Conclusions. Our observations reveal the physical and chemical structure of water vapor close to the protostars on solar-system scales. The red-shifted absorption detected toward source B is indicative of infall. The excitation temperature is consistent with the picture of water ice evaporation close to the protostar. The low HDO/H2O ratio deduced here suggests that the differences between the inner regions of the protostars and the Earth's oceans and comets are smaller than previously thought.
AB - Context. Measuring the water deuterium fractionation in the inner warm regions of low-mass protostars has so far been hampered by poor angular resolution obtainable with single-dish ground- and space-based telescopes. Observations of water isotopologues using (sub)millimeter wavelength interferometers have the potential to shed light on this matter. Aims. To measure the water deuterium fractionation in the warm gas of the deeply-embedded protostellar binary IRAS16293-2422. Methods. Observations toward IRAS16293-2422 of the 53,2-44,1 transition of H2 18O at 692.07914GHz from Atacama Large Millimeter/submillimeter Array (ALMA) as well as the 31,3-22,0 of H2 18O at 203.40752GHz and the 31,2-22,1 transition of HDO at 225.89672GHz from the Submillimeter Array (SMA) are presented. Results. The 692GHz H2 18O line is seen toward both components of the binary protostar. Toward one of the components, "sourceB", the line is seen in absorption toward the continuum, slightly red-shifted from the systemic velocity, whereas emission is seen off-source at the systemic velocity. Toward the other component, "sourceA", the two HDO and H2 18O lines are detected as well with the SMA. From the H2 18O transitions the excitation temperature is estimated at 124±12K. The calculated HDO/H2O ratio is (9.2±2.6)×10-4 - significantly lower than previous estimates in the warm gas close to the source. It is also lower by a factor of ∼5 than the ratio deduced in the outer envelope. Conclusions. Our observations reveal the physical and chemical structure of water vapor close to the protostars on solar-system scales. The red-shifted absorption detected toward source B is indicative of infall. The excitation temperature is consistent with the picture of water ice evaporation close to the protostar. The low HDO/H2O ratio deduced here suggests that the differences between the inner regions of the protostars and the Earth's oceans and comets are smaller than previously thought.
U2 - 10.1051/0004-6361/201220638
DO - 10.1051/0004-6361/201220638
M3 - Letter
SN - 0004-6361
VL - 549
JO - Astronomy and Astrophysics Supplement Series
JF - Astronomy and Astrophysics Supplement Series
M1 - L3
ER -