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Journal Article

Evolution of young protoclusters embedded in dense massive clumps. A new grid of population synthesis SED models and a new set of L/M evolutionary tracks

MPS-Authors

Molinari,  Sergio
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Baldeschi,  Adriano
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Robitaille,  Thomas P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Morales,  Esteban F. E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Schisano,  Eugenio
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Traficante,  Alessio
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Merello,  Manuel
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Molinaro,  Marco
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Vitello,  Fabio
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sciacca,  Eva
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Liu,  Scige J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.4508M
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Citation

Molinari, S., Baldeschi, A., Robitaille, T. P., Morales, E. F. E., Schisano, E., Traficante, A., et al. (2019). Evolution of young protoclusters embedded in dense massive clumps. A new grid of population synthesis SED models and a new set of L/M evolutionary tracks. Monthly Notices of the Royal Astronomical Society, 486, 4508-4525.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D2E1-F
Abstract
A grid of 20 millions 3-1100 μm spectral energy distribution (SED) models is presented for synthetic young clusters embedded in dense clumps. The models depend on four primary parameters: the clump mass Mclump and dust temperature Tdust, the fraction of mass fcore locked in dense cores, and the age of the clump tSF. We populate the young stellar object (YSO) clusters using the Kroupa initial mass function and the YSOs SED models grid of Robitaille et al. We conduct extensive testing of SED fitting using a simulated data set and we find that Mclump essentially depends on the submillimetre portion of the SED, while Tdust is mostly determined from the shape of the SED in the 70-350 μm range. Thanks to the large number of models computed, we verify that the combined analysis of L/M, [8-24] and [24-70] colours removes much of the SEDs fcore-tSF degeneracy. The L/M values are particularly useful to diagnose fcore. L/M ≤ 1 identifies protoclusters with fcore ≤ 0.1 and tSF \lower.6ex{~ }\raise.65ex\lt 10^5 yr, while L/M \lower.6ex{~ }\raise.65ex\gt 10 excludes fcore ≤ 0.1. We characterize lower limits of L/M where zero-age main sequence (ZAMS) stars are not found in models, and we also find models with L/M ≥10 and no ZAMS stars, in which [8-24] \lower.6ex{~ }\raise.65ex\gt 0.8± 0.1 independently from Mclump, temperature, and luminosity. This is the first set of synthesis SED models suited to model for embedded and unresolved clusters of YSOs. A set of new evolutionary tracks in the L/M diagram is also presented.