Chemical complexity in high-mass star formation: An observational and modeling case-study of the AFGL2591 VLA3 hot core

Gieser, C., Semenov, D., Beuther, H., Ahmadi, A., Mottram, J.C., Henning, Th., Beltran, M., Maud, L.T., Bosco, F., Leurini, S., and others. (2019) Chemical complexity in high-mass star formation: An observational and modeling case-study of the AFGL2591 VLA3 hot core. Astronomy and Astrophysics, 631 . Article Number A142. ISSN 0004-6361. (doi:10.1051/0004-6361/201935865) (KAR id:76481)

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Official URL: http://dx.doi.org/10.1051/0004-6361/201935865

Abstract

Aims: In order to understand the observed molecular diversity in high-mass star-forming regions, one has to discern the underlying physical and chemical structure of those regions at high angular resolution and over a range of evolutionary stages. Methods: We present a detailed observational and modeling study of the hot core VLA3 in the high-mass star-forming region AFGL 2591, which is a target region of the NOrthern Extended Millimeter Array (NOEMA) large program CORE. Using NOEMA observations at 1.37mm with an angular resolution of ~0.0042 (1 400 au at 3.33 kpc), we derived the physical and chemical structure of the source. We modeled the observed molecular abundances with the chemical evolution code MUSCLE (MUlti Stage ChemicaL codE. Results: With the kinetic temperature tracers CH3CN and H2CO we observe a temperature distribution with a power-law index of q = 0:41+- 0:08. Using the visibilities of the continuum emission we derive a density structure with a power-law index of p = 1:7 +- 0:1. The hot core spectra reveal high molecular abundances and a rich diversity in complex molecules. The majority of the molecules have an asymmetric spatial distribution around the forming protostar(s), which indicates a complex physical structure on scales < 1 400 au. Using MUSCLE, we are able to explain the observed molecular abundance of 10 out of 14 modeled species at an estimated hot core chemical age of ~21 100 years. In contrast to the observational analysis, our chemical modeling predicts a lower density power-law index of p < 1:4. Reasons for this discrepancy are discussed. Conclusions: Combining high spatial resolution observations with detailed chemical modeling allows us to derive a concise picture of the physical and chemical structure of the famous AFGL 2591 hot core. The next steps are to conduct similar analysis for the whole CORE sample and by that constrain the chemical diversity in high-mass star formation to much greater depth.

Item Type:	Article
DOI/Identification number:	10.1051/0004-6361/201935865
Uncontrolled keywords:	ISM, individual objects, AFGL 2591, Astrochemistry, ISM: molecules, Stars: massive
Subjects:	Q Science > QB Astronomy
Divisions:	Divisions > Division of Natural Sciences > Physics and Astronomy
Depositing User:	James Urquhart
Date Deposited:	16 Sep 2019 08:16 UTC
Last Modified:	05 Nov 2024 12:41 UTC
Resource URI:	https://kar.kent.ac.uk/id/eprint/76481 (The current URI for this page, for reference purposes)

University of Kent Author Information

Urquhart, J.S..

Creator's ORCID:	https://orcid.org/0000-0002-1605-8050
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