TY - JOUR
T1 - The Prebiotic Molecular Inventory of Serpens SMM1: II. The Building Blocks of Peptide Chains
AU - Ligterink, Niels F. W.
AU - Ahmadi, Aida
AU - Luitel, Bijaya
AU - Coutens, Audrey
AU - Calcutt, Hannah
AU - Tychoniec, Łukasz
AU - Linnartz, Harold
AU - Jørgensen, Jes K.
AU - Garrod, Robin T.
AU - Bouwman, Jordy
PY - 2022
Y1 - 2022
N2 - This work aims to constrain the abundances of interstellar amides, by searching for this group of prebiotic molecules in the intermediate-mass protostar Serpens SMM1-a. ALMA observations are conducted toward Serpens SMM1. A spectrum is extracted toward the SMM1-a position and analyzed with the CASSIS line analysis software for the presence of characteristic rotational lines of a number of amides and other molecules. NH
2CHO, NH
2CHO ν
12= 1, NH
2
13CHO, CH
3C(O)NH
2ν = 0, 1, CH
2DOH, CH
3CHO, and CH
3C(O)CH
3are securely detected, while trans-NHDCHO, NH
2CDO, CH
3NHCHO ν = 0, 1, CH
3COOH, and HOCH
2CHO are tentatively identified. The results of this work are compared with detections presented in the literature. A uniform CH
3C(O)NH
2/NH
2CHO ratio is found for a group of interstellar sources with vast physical differences. A similar ratio is seen for CH
3NHCHO, based on a smaller data sample. The D/H ratio of NH
2CHO is about 1-3% and is close to values found in the low-mass source IRAS 16293-2422B. The formation of CH
3C(O)NH
2and NH
2CHO is likely linked. Formation of these molecules on grain surfaces during the dark cloud stage is a likely scenario. The high D/H ratio of NH
2CHO is also seen as an indication that these molecules are formed on icy dust grains. As a direct consequence, amides are expected to be present in the most pristine material from which planetary systems form, thus providing a reservoir of prebiotic material.
AB - This work aims to constrain the abundances of interstellar amides, by searching for this group of prebiotic molecules in the intermediate-mass protostar Serpens SMM1-a. ALMA observations are conducted toward Serpens SMM1. A spectrum is extracted toward the SMM1-a position and analyzed with the CASSIS line analysis software for the presence of characteristic rotational lines of a number of amides and other molecules. NH
2CHO, NH
2CHO ν
12= 1, NH
2
13CHO, CH
3C(O)NH
2ν = 0, 1, CH
2DOH, CH
3CHO, and CH
3C(O)CH
3are securely detected, while trans-NHDCHO, NH
2CDO, CH
3NHCHO ν = 0, 1, CH
3COOH, and HOCH
2CHO are tentatively identified. The results of this work are compared with detections presented in the literature. A uniform CH
3C(O)NH
2/NH
2CHO ratio is found for a group of interstellar sources with vast physical differences. A similar ratio is seen for CH
3NHCHO, based on a smaller data sample. The D/H ratio of NH
2CHO is about 1-3% and is close to values found in the low-mass source IRAS 16293-2422B. The formation of CH
3C(O)NH
2and NH
2CHO is likely linked. Formation of these molecules on grain surfaces during the dark cloud stage is a likely scenario. The high D/H ratio of NH
2CHO is also seen as an indication that these molecules are formed on icy dust grains. As a direct consequence, amides are expected to be present in the most pristine material from which planetary systems form, thus providing a reservoir of prebiotic material.
UR - http://www.scopus.com/inward/record.url?scp=85125634410&partnerID=8YFLogxK
U2 - 10.1021/acsearthspacechem.1c00330
DO - 10.1021/acsearthspacechem.1c00330
M3 - Article
SN - 2472-3452
VL - 6
SP - 455
EP - 467
JO - ACS Earth and Space Chemistry
JF - ACS Earth and Space Chemistry
IS - 3
ER -