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 (43)

• The Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory
• The Herschel-SPIRE instrument and its in-flight performance
• Some Aspects of Measurement Error in Linear Regression of Astronomical Data
• Hi-GAL: the Herschel infrared Galactic Plane Survey
• High-Mass Star and Massive Cluster Formation in the Milky Way
• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• Consistent dust and gas models for protoplanetary disks. I. Disk shape, dust settling, opacities, and PAHs
• Global Hierarchical Collapse In Molecular Clouds. Towards a Comprehensive Scenario
• Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues. First data release for Inner Milky Way: +68°> l > -70°
• Radiative transfer in very optically thick circumstellar disks
• Clump morphology and evolution in MHD simulations of molecular cloud formation
• 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
• The data reduction pipeline for the Hi-GAL survey
• CO outflows from high-mass Class 0 protostars in Cygnus-X
• How long does it take to form a molecular cloud?
• Far-Infrared Dust Temperatures and Column Densities of the MALT90 Molecular Clump Sample
• Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud
• The Bolocam Galactic Plane Survey. XIV. Physical Properties of Massive Starless and Star Forming Clumps
• ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results
• Calibration of evolutionary diagnostics in high-mass star formation
• On the simultaneous evolution of massive protostars and their host cores
• ALMA observations of fragmentation, sub-structure, and protostars in high-mass starless clump candidates
• Detection of a high-mass prestellar core candidate in W43-MM1
• A Mid-Infrared Census of Star Formation Activity in Bolocam Galactic Plane Survey Sources
• On the Modified Random Walk for Monte-Carlo Radiation Transfer
• 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
• Remarkable analytic relations among greybody parameters
• The fragmentation properties of massive protocluster gas clumps: an ALMA study
• Thermal balance and comparison of gas and dust properties of dense clumps in the Hi-GAL survey
• The Comparison of Physical Properties Derived from Gas and Dust in a Massive Star-Forming Region
• 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
• ALMA-IMF XVII -- Census and lifetime of high-mass prestellar cores in 14 massive protoclusters
• Simulated observations of star formation regions: infrared evolution of globally collapsing clouds
• Insights from Synthetic Star-forming Regions: II. Verifying Dust Surface Density, Dust Temperature & Gas Mass Measurements with Modified Blackbody Fitting
• Insights from Synthetic Star-forming Regions: III. Calibration of Measurement Techniques of Star-formation Rates
• Investigating the ultraviolet and infrared radiation through the turbulent life of molecular clouds

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