2013A&A...549L...3P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.25CET09:56:26

2013A&A...549L...3P - Astronomy and Astrophysics, volume 549, L3-3 (2013/1-1)

Warm water deuterium fractionation in IRAS 16293-2422. The high-resolution ALMA and SMA view.

PERSSON M.V., JORGENSEN J.K. and VAN DISHOECK E.F.

Abstract (from CDS):

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. To measure the water deuterium fractionation in the warm gas of the deeply-embedded protostellar binary IRAS 16293-2422. Observations toward IRAS 16293-2422 of the 532-441 transition of H218O at 692.07914GHz from Atacama Large Millimeter/submillimeter Array (ALMA) as well as the 313-220 of H218O at 203.40752GHz and the 312-221 transition of HDO at 225.89672GHz from the Submillimeter Array (SMA) are presented. The 692GHz H218O line is seen toward both components of the binary protostar. Toward one of the components, ``source B'', 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, ``source A'', the two HDO and H218O lines are detected as well with the SMA. From the H218O transitions the excitation temperature is estimated at 124±12K. The calculated HDO/H2O ratio is (9.2±2.6)x10–4 - 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. 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.

Abstract Copyright:

Journal keyword(s): astrochemistry - stars: formation - protoplanetary disks - ISM: abundances - ISM: general

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 562 0
2 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2727 2
3 QSO B1514-24 BLL 15 17 41.8135246339 -24 22 19.482167214   15.13 14.00 13.95   ~ 653 3
4 QSO B1622-253 QSO 16 25 46.89164010 -25 27 38.3267989   21.3 20.6 19.60   ~ 304 1
5 QSO B1622-297 QSO 16 26 06.02083867 -29 51 26.9710860   18.41 20.5 17.6   ~ 366 0
6 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3066 0
7 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1057 1
8 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 188 0
9 [W89] A2 Rad 16 32 22.866 -24 28 35.90           ~ 22 0
10 [W89] A1 Rad 16 32 22.887 -24 28 35.67           ~ 23 0
11 LDN 1689N DNe 16 32 31 -24 28.6           ~ 108 0
12 QSO B1730-130 QSO 17 33 02.70578476 -13 04 49.5481484   18 18.5 18.78 17.39 ~ 992 1
13 QSO B1921-293 BLL 19 24 51.05595514 -29 14 30.1210524   18.71 18.21 15.07   ~ 697 0

    Equat.    Gal    SGal    Ecl

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2020.10.25-09:56:26

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