Deuterated water in the solar-type protostars NGC 1333 IRAS 4A and IRAS 4B

作者：Coutens A; Vastel C; Cabrit S; Codella C; Kristensen L E; Ceccarelli C; van Dishoeck E F; Boogert A C A; Bottinelli S; Castets A; Caux E; Comito C; Demyk K; Herpin F; Lefloch B; McCoey C; Mottram J C; Parise B; Taquet V; van der Tak F F S; Visser R; Yildiz U A

来源：Astronomy & Astrophysics, 2013, 560: A39.

DOI：10.1051/0004-6361/201322400

• astrochemistry
• ISM: individual objects: NGC 1333 IRAS 4A
• ISM: individual objects: NGC 1333 IRAS 4B
• ISM: abundances
• ISM: molecules

Context. The measure of the water deuterium fractionation is a relevant tool for understanding mechanisms of water formation and evolution from the prestellar phase to the formation of planets and comets.
Aims. The aim of this paper is to study deuterated water in the solar-type protostars NGC 1333 IRAS 4A and IRAS 4B, to compare their HOD abundance distributions with other star-forming regions, and to constrain their HDO/H2O abundance ratios.
Methods. Using the Herschel/HIFI instrument as well as ground-based telescopes, we observed several HOD lines covering a large excitation range (E-ap/k = 22-168 K) towards these protostars and an outflow position. Non-local thermal equilibrium radiative transfer codes were then used to determine the HDO abundance profiles in these sources.
Results. The HDO fundamental line profiles show a very broad component, tracing the molecular outflows, in addition to a narrower emission component and a narrow absorbing component. In the protostellar envelope of NGC 1333 IRAS 4A, the HOD inner (T >= 100 K) and outer (T < 100 K) abundances with respect to H-2 are estimated with a 3 sigma uncertainty at 7.5(-3.0)(+3.5) x 10(-9) and 1.2(-0.4)(+0.4) x 10(-11), respectively, whereas in NGC 1333 IRAS 4B they are x 10(-8) and 1.2(-0.4)(+0.6) x 10(-10), respectively. Similarly to the low-mass protostar IRAS 16293-2422, an absorbing outer layer with an enhanced abundance of deuterated water is required to reproduce the absorbing components seen in the fundamental lines at 465 and 894 GHz in both sources. This water-rich layer is probably extended enough to encompass the two sources, as well as parts of the outflows. In the outflows emanating from NGC 1333 IRAS 4A, the HDO column density is estimated at about (2-4) x 100 cm(-2), leading to an abundance of about (0.7-1.9) x 10(-9). An HDO/H2O ratio between 7 x 10(-4) and 9 x 10(-2) is also derived in the outflows. In the warm inner regions of these two sources, we estimate the HDO/H2O ratios at about 1 x 10(-4)-4 x 10(-3). This ratio seems higher (a few %) in the cold envelope of IRAS 4A, whose possible origin is discussed in relation to formation processes of HOD and H2O.
Conclusions. In low-mass protostars, the HOD outer abundances range in a small interval, between similar to 10(-11) and a few 10(-10). No clear trends are found between the HDO abundance and various source parameters (L-bol, L-smm, L-smm/L-bol, T-bol, L-bol(0.6)/M-env). A tentative correlation is observed, however, between the ratio of the inner and outer abundances with the submillimeter luminosity.

• 出版日期2013-12