TY - JOUR
T1 - An interferometric study of the low-mass protostar IRAS 16293-2422
T2 - Small scale organic chemistry
AU - Bisschop, S. E.
AU - Jørgensen, J. K.
AU - Bourke, T. L.
AU - Bottinelli, S.
AU - Van Dishoeck, E. F.
PY - 2008/9/1
Y1 - 2008/9/1
N2 - Aims. We investigate the chemical relations between complex organics based on their spatial distributions and excitation conditions in the low-mass young stellar objects IRAS 16293-2422 "A" and "B".Methods. Interferometric observations with the Submillimeter Array have been performed at 5″ × 3″ (800 × 500 AU) resolution revealing emission lines of HNCO, CHCN, CHCO, CHCHO and CHOH. Rotational temperatures are determined from rotational diagrams when a sufficient number of lines are detected.Results. Compact emission is detected for all species studied here. For HNCO and CHCN it mostly arises from source "A", CHCO and CHOH have comparable strength for both sources and CHCHO arises exclusively from source "B". HNCO, CHCN and CHCHO have rotational temperatures > 200 K implying that they arise from hot gas. The -visibility data reveal that HNCO also has extended cold emission, which could not be previously determined through single dish data. Conclusions. The relative abundances of the molecules studied here are very similar within factors of a few to those found in high-mass YSOs. This illustrates that the chemistry between high- and low-mass objects appears to be relatively similar and thus independent of luminosity and cloud mass. In contrast, bigger abundance differences are seen between the "A" and "B" source. For instance, the HNCO abundance relative to CHOH is ~4 times higher toward "A", which may be due to a higher initial OCN ice abundances in source "A" compared to "B". Furthermore, not all oxygen-bearing species are co-existent, with CHCHO/CHOH an order of magnitude higher toward "B" than "A". The different spatial behavior of CHCO and CHOH compared with CHCHO suggests that successive hydrogenation reactions on grain-surfaces are not sufficient to explain the observed gas phase abundance of the latter. Selective destruction of CHCHO may result in the anti-coincidence of these species in source "A". These results illustrate the power of interferometric compared with single dish data in terms of testing chemical models.
AB - Aims. We investigate the chemical relations between complex organics based on their spatial distributions and excitation conditions in the low-mass young stellar objects IRAS 16293-2422 "A" and "B".Methods. Interferometric observations with the Submillimeter Array have been performed at 5″ × 3″ (800 × 500 AU) resolution revealing emission lines of HNCO, CHCN, CHCO, CHCHO and CHOH. Rotational temperatures are determined from rotational diagrams when a sufficient number of lines are detected.Results. Compact emission is detected for all species studied here. For HNCO and CHCN it mostly arises from source "A", CHCO and CHOH have comparable strength for both sources and CHCHO arises exclusively from source "B". HNCO, CHCN and CHCHO have rotational temperatures > 200 K implying that they arise from hot gas. The -visibility data reveal that HNCO also has extended cold emission, which could not be previously determined through single dish data. Conclusions. The relative abundances of the molecules studied here are very similar within factors of a few to those found in high-mass YSOs. This illustrates that the chemistry between high- and low-mass objects appears to be relatively similar and thus independent of luminosity and cloud mass. In contrast, bigger abundance differences are seen between the "A" and "B" source. For instance, the HNCO abundance relative to CHOH is ~4 times higher toward "A", which may be due to a higher initial OCN ice abundances in source "A" compared to "B". Furthermore, not all oxygen-bearing species are co-existent, with CHCHO/CHOH an order of magnitude higher toward "B" than "A". The different spatial behavior of CHCO and CHOH compared with CHCHO suggests that successive hydrogenation reactions on grain-surfaces are not sufficient to explain the observed gas phase abundance of the latter. Selective destruction of CHCHO may result in the anti-coincidence of these species in source "A". These results illustrate the power of interferometric compared with single dish data in terms of testing chemical models.
KW - Astrochemistry
KW - Line: identification
KW - methods: observational
KW - stars: formation
KW - Techniques: interferometric
UR - http://www.scopus.com/inward/record.url?scp=51949116177&partnerID=8YFLogxK
U2 - 10.1051/0004-6361:200809673
DO - 10.1051/0004-6361:200809673
M3 - Journal article
AN - SCOPUS:51949116177
SN - 0004-6361
VL - 488
SP - 959
EP - 968
JO - Astronomy and Astrophysics Supplement Series
JF - Astronomy and Astrophysics Supplement Series
IS - 3
ER -