The Rosetta Stone Project. II. The correlation between star formation efficiency and L/M indicator for the evolutionary stages of star-forming clumps in post-processed radiative magnetohydrodynamics simulations

Abstract

Context. The evolution of massive star-forming clumps that are progenitors of high-mass young stellar objects are often classified based on a variety of observational indicators ranging from near-infrared to radio wavelengths. Among them, the ratio of the bolometric luminosity to the mass of their envelope, $L/M$, has been observationally diagnosed as a good indicator for the evolutionary classification of parsec-scale star-forming clumps in the Galaxy. Aims. We developed the Rosetta Stone project$\unicode{x2013}$an end-to-end framework designed to enable an accurate comparison between simulations and observations for investigating the formation and evolution of massive clumps. In this study, we calibrate the $L/M$ indicator in relation to the star formation efficiency (SFE) and the clump age, as derived from our suite of simulations. Methods. We performed multi-wavelength radiative transfer post-processing of radiative magnetohydrodynamics (RMHD) simulations of the collapse of star-forming clumps fragmenting into protostars. We generated synthetic observations to obtain far-infrared emission from $70$ to $500\mu$m, as was done in the Hi-GAL survey, and at $24\mu$m in the MIPSGAL survey, which were then used to build the spectral energy distributions (SEDs) and estimate the $L/M$ parameter. An additional $1.3$mm wavelength in ALMA Band 6 was also produced for the comparison with observational data. We applied observational techniques$\unicode{x2013}$commonly employed by observers$\unicode{x2013}$to the synthetic data in order to derive the corresponding physical parameters. Results. We find a correlation between $L/M$ and the SFE, with a power-law form $L/M\propto {\mathrm{SFE}}^{1.20_{-0.02}^{+0.02}}$. This correlation is independent of the mass of the clumps and the choice of initial conditions of the simulations in which they formed. (Abridged)

To appear in Astronomy & Astrophysics. The series of 3 papers is accepted for publication

References in corpus (16)

• Some Aspects of Measurement Error in Linear Regression of Astronomical Data
• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• Radiative transfer in very optically thick circumstellar disks
• From the warm magnetized atomic medium to molecular clouds
• The Birth of Molecular Clouds: Formation of Atomic Precursors in Colliding Flows
• Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ }<\ell <67.0^{\circ }$)
• Towards a more realistic sink particle algorithm for the RAMSES code
• ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results
• Multi-scale dynamics in star-forming regions: the interplay between gravity and turbulence
• The SQUALO project (Star formation in QUiescent And Luminous Objects) I: clump-fed accretion mechanism in high-mass star-forming objects
• The Comparison of Physical Properties Derived from Gas and Dust in a Massive Star-Forming Region
• Thermal balance and comparison of gas and dust properties of dense clumps in the Hi-GAL survey
• The accretion history of high-mass stars: An ArTéMiS pilot study of Infrared Dark Clouds
• Hyper: Hybrid Photometry and Extraction Routine
• Accuracy of ALMA estimates of young disk radii and masses. Predicted observations from numerical simulations
• The initial conditions of high-mass star formation: radiative transfer models of IRDCs seen in the Herschel Hi-GAL survey

Cited by in corpus (1)

• The fragmentation properties of massive star-forming regions in 30Dor-10 at 2000 au resolution