CAMPOS II. The onset of protostellar disk substructures and planet formation

Abstract

The 1.3 mm CAMPOS survey has resolved 90 protostellar disks with ~15 au resolution across the Ophiuchus, Corona Australis, and Chamaeleon star-forming regions. To address the fundamental question, `When does planet formation begin?', we combined the CAMPOS sample with literature observations of Class 0-II disks (bolometric temperature, $T_{bol}\le 1900K$). To investigate substructure detection rates as a function of $T_{bol}$, we restricted the sample to disks observed at the 1.3 mm wavelength, with inclinations below 75${}^{\circ }$, linear resolution $\le 20$ au and resolved with at least 4 resolution elements (${\theta }_{disk}/{\theta }_{res}\ge 4$). We also considered the effects of extinction correction and the inclusion of Herschel Space Telescope data on the $T_{bol}$ measurements to constrain the lower and upper limits of $T_{bol}$ for each source. We find that by $T_{bol}$ ~200-400 K, substructure detection rates increased sharply to ~60%, corresponding to an age of ~0.2-0.4 Myr. No substructures are detected in Class 0 disks. The ratio of disk-averaged brightness temperature to predicted dust temperature shows a trend of increasing values toward the youngest Class 0 disks, suggesting higher optical depths in these early stages. Our statistical analysis confirms that substructures similar to those in Class II disks are already common by the Class I stage, and the emergence of structures at early Class I could represent only an upper limit. Classifying disks with substructures into those with and without large central cavities, we find both populations coexisting across evolutionary stages, suggesting they are not necessarily evolutionarily linked. If protostellar disk substructures do follow an evolutionary sequence, then our results imply that disk substructures evolve very rapidly and thus can be present in all Class I/II stages and/or that they can be triggered at different times.

22 pages, 9 figures, 3 tables. Accepted by A&A 2025.6.24

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