Low-mass star formation in R Coronae Australis: Observations of organic molecules with the APEX telescope
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Low-mass star formation in R Coronae Australis : Observations of organic molecules with the APEX telescope. / Schöier, F. L.; Jørgensen, J. K.; Pontoppidan, K. M.; Lundgren, A. A.
I: Astronomy and Astrophysics, Bind 454, Nr. 2, 01.08.2006, s. L67-L70.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Low-mass star formation in R Coronae Australis
T2 - Observations of organic molecules with the APEX telescope
AU - Schöier, F. L.
AU - Jørgensen, J. K.
AU - Pontoppidan, K. M.
AU - Lundgren, A. A.
PY - 2006/8/1
Y1 - 2006/8/1
N2 - This paper presents new APEX submillimetre molecular line observations of three low-mass protostars, IRS7A, IRS7B, and IRAS32, in the R Coronae Australis molecular cloud complex. The molecular excitation analysis is performed using a statistical equilibrium radiative transfer code. The derived beam averaged fractional abundances vary by less than a factor of two among the three sources, except those of H2CO and CH3OH, which show differences of about an order of magnitude. The molecular abundances are similar to those typically found in other star-forming regions in the Galaxy, such as the ρ Oph and Perseus molecular clouds. There is a marked difference in the kinetic temperatures derived for the protobinary source IRS7 from H2CO (≈40-60 K) and CH3OH (≈20 K), possibly indicating a difference in origin of the emission from these two molecules.
AB - This paper presents new APEX submillimetre molecular line observations of three low-mass protostars, IRS7A, IRS7B, and IRAS32, in the R Coronae Australis molecular cloud complex. The molecular excitation analysis is performed using a statistical equilibrium radiative transfer code. The derived beam averaged fractional abundances vary by less than a factor of two among the three sources, except those of H2CO and CH3OH, which show differences of about an order of magnitude. The molecular abundances are similar to those typically found in other star-forming regions in the Galaxy, such as the ρ Oph and Perseus molecular clouds. There is a marked difference in the kinetic temperatures derived for the protobinary source IRS7 from H2CO (≈40-60 K) and CH3OH (≈20 K), possibly indicating a difference in origin of the emission from these two molecules.
KW - Astrochemistry
KW - ISM: abundances
KW - ISM: molecules
KW - Stars: formation
UR - http://www.scopus.com/inward/record.url?scp=33746377955&partnerID=8YFLogxK
U2 - 10.1051/0004-6361:20065334
DO - 10.1051/0004-6361:20065334
M3 - Journal article
AN - SCOPUS:33746377955
VL - 454
SP - L67-L70
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
IS - 2
ER -
ID: 234019633