Molecular complexity in pre-stellar cores : a 3 mm-band study of L183 and L1544

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http://hdl.handle.net/10138/312306

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Lattanzi , V , Bizzocchi , L , Vasyunin , A I , Harju , J , Giuliano , B M , Vastel , C & Caselli , P 2020 , ' Molecular complexity in pre-stellar cores : a 3 mm-band study of L183 and L1544 ' , Astronomy & Astrophysics , vol. 633 , A118 . https://doi.org/10.1051/0004-6361/201936884

Title: Molecular complexity in pre-stellar cores : a 3 mm-band study of L183 and L1544
Author: Lattanzi, Valerio; Bizzocchi, Luca; Vasyunin, Anton I.; Harju, Jorma; Giuliano, Barbara M.; Vastel, Charlotte; Caselli, Paola
Contributor: University of Helsinki, Particle Physics and Astrophysics
Date: 2020-01-22
Language: eng
Number of pages: 17
Belongs to series: Astronomy & Astrophysics
ISSN: 0004-6361
URI: http://hdl.handle.net/10138/312306
Abstract: Context. Pre-stellar cores (PSCs) are units of star formation. Besides representing early stages of the dynamical evolution leading to the formation of stars and planets, PSCs also provide a substrate for incipient chemical complexity in the interstellar space. Aims. Our aim is to understand the influence of external conditions on the chemical composition of PSCs. For this purpose, we compared molecular column densities in two typical PSCs, L183 and L1544, which are embedded in different environments. Methods. A single-pointing survey of L183 at lambda = 3 mm was conducted using the IRAM 30-m single-dish antenna. This led to the detection of more than 100 emission lines from 46 molecular species. The molecular column densities and excitation temperatures derived from these lines were compared to the corresponding parameters in L1544. The data for L1544 were obtained from literature or publicly available surveys, and they were analysed using the same procedure as adopted for L183. An astrochemical model, previously developed for the interpretation of organic molecule emissions towards the methanol peak of L1544, was used to interpret the combined data. Results. Our analysis reveals clear chemical differences between the two PSCs. While L1544 is richer in carbon-bearing species, in particular carbon chains, oxygen-containing species are generally more abundant in L183. The results are well-reproduced by our chemical model. Conclusions. The observed chemical differentiation between the two PSCs is caused by the different environmental conditions: the core of L183 is deeply buried in the surrounding cloud, whereas L1544 lies close to the edge of the Taurus Molecular Cloud. The obscuration of L183 from the interstellar radiation field (ISRF) allows the carbon atoms to be locked in carbon monoxide, which ultimately leads to a large abundance of O-bearing species. In contrast, L1544, being more affected by the ISRF, can keep a fraction of carbon in atomic form, which is needed for the production of carbon chains.
Subject: ISM: molecules
line: identification
molecular data
molecular processes
radio lines: ISM
SUBMILLIMETER-WAVE SPECTRUM
ISOLATED STAR-FORMATION
LAMB-DIP SPECTRUM
HYPERFINE-STRUCTURE
LABORATORY DETECTION
ROTATIONAL SPECTRUM
DEUTERIUM FRACTIONATION
ASTROPHYSICAL INTEREST
INITIAL CONDITIONS
MICROWAVE-SPECTRA
115 Astronomy, Space science
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