Multi-wavelength modelling of the circumstellar environment of the massive proto-star AFGL 2591 VLA 3

Abstract

We have studied the dust density, temperature and velocity distributions of the archetypal massive young stellar object (MYSO) AFGL 2591. Given its high luminosity ($L=2\times 10^5$ L${}_{\odot }$) and distance ($d=3.3$ kpc), AFGL 2591 has one of the highest $\sqrt{L}/d$ ratio, giving better resolved dust emission than any other MYSO. As such, this paper provides a template on how to use resolved multi-wavelength data and radiative transfer to obtain a well-constrained 2-D axi-symmetric analytic rotating infall model. We show for the first time that the resolved dust continuum emission from Herschel 70 $\mu$m observations is extended along the outflow direction, whose origin is explained in part from warm dust in the outflow cavity walls. However, the model can only explain the kinematic features from CH${}_3$CN observations with unrealistically low stellar masses ($<15$ M${}_{\odot }$), indicating that additional physical processes may be playing a role in slowing down the envelope rotation. As part of our 3-step continuum and line fitting, we have identified model parameters that can be further constrained by specific observations. High-resolution mm visibilities were fitted to obtain the disc mass (6 M${}_{\odot }$) and radius (2200 au). A combination of SED and near-IR observations were used to estimate the luminosity and envelope mass together with the outflow cavity inclination and opening angles.

34 pages, 22 figures, 15 tables, 4 appendices. Accepted for publication in MNRAS

References in corpus (20)

• The UKIDSS Galactic Plane Survey
• The SCUBA Legacy Catalogue: Continuum Objects Detected by SCUBA
• The earliest phases of high-mass star formation: a 3 square degree millimeter continuum mapping of Cygnus X
• Circumventing the radiation pressure barrier in the formation of massive stars via disk accretion
• Limiting Accretion onto Massive Stars by Fragmentation-Induced Starvation
• The Fragmentation of Magnetized, Massive Star-Forming Cores with Radiative Feedback
• The Luminosity Functions and Timescales of MYSOs and Compact HII regions
• A modular set of synthetic spectral energy distributions for young stellar objects
• Forming spectroscopic massive proto-binaries by disk fragmentation
• Protostellar Outflows and Radiative Feedback from Massive Stars. II. Feedback, Star Formation Efficiency, and Outflow Broadening
• Protostellar Outflows and Radiative Feedback from Massive Stars
• Resolved 24.5 micron emission from massive young stellar objects
• Multidimensional chemical modelling, II. Irradiated outflow walls
• Chemical complexity in high-mass star formation: An observational and modeling case study of the AFGL 2591 VLA 3 hot core
• The standard model of low-mass star formation applied to massive stars: a multi-wavelength picture of AFGL 2591
• Energetic radiation and the sulfur chemistry of protostellar envelopes: Submillimeter interferometry of AFGL 2591
• Modelling the interaction between relativistic and non-relativistic winds in binary pulsar systems: strong magnetization of the pulsar wind
• The HIFI spectral survey of AFGL 2591 (CHESS). II. Summary of the survey
• The HIFI spectral survey of AFGL 2591 (CHESS). III. Chemical structure of the protostellar envelope
• Herschel Hi-GAL imaging of massive young stellar objects

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• Disk fragmentation in high-mass star formation. High-resolution observations towards AFGL 2591-VLA 3
• The burst mode of accretion in massive star formation with stellar inertia
• The physical and chemical structure of high-mass star-forming regions. Unraveling chemical complexity with the NOEMA large program "CORE"
• High-Resolution M-band Spectroscopy of CO towards the Massive Young Stellar Binary W3 IRS5
• Clustered Formation of Massive Stars within an Ionized Rotating Disk