English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

During the journey from the cloud to the disc, the chemical composition ofthe protostellar envelope material can be either preserved or processed tovarying degrees depending on the surrounding physical environment. This worksaims to constrain the interplay of solid (ice) and gaseous methanol (CH$_3$OH)in the outer regions of protostellar envelopes located in the Coronet clusterin Corona Australis (CrA), and assess the importance of irradiation by theHerbig Ae/Be star R CrA. CH$_3$OH is a prime test-case as it predominantlyforms as a consequence of the solid-gas interplay (hydrogenation of condensedCO molecules onto the grain surfaces) and it plays an important role in futurecomplex molecular processing. We present 1.3 mm Submillimeter Array (SMA) andAtacama Pathfinder Experiment (APEX) observations towards the envelopes of fourlow-mass protostars in the Coronet. Eighteen molecular transitions of sevenspecies are identified. We calculate CH$_3$OH gas-to-ice ratios in thisstrongly irradiated cluster and compare them with ratios determined towardsprotostars located in less irradiated regions such as the Serpens SVS 4 clusterin Serpens Main and the Barnard 35A cloud in the $\lambda$ Orionis region. TheCH$_3$OH gas-to-ice ratios in the Coronet vary by one order of magnitude (from1.2$\times$10$^{-4}$ to 3.1$\times$10$^{-3}$) which is similar to lessirradiated regions as found in previous studies. We find that the CH$_3$OHgas-to-ice ratios estimated in these three regions are remarkably similardespite the different UV radiation field intensities and formation histories.This result suggests that the overall CH$_3$OH chemistry in the outer regionsof low-mass envelopes is relatively independent of variations in the physicalconditions and hence that it is set during the prestellar stage.

Linking ice and gas in the Coronet cluster in Corona Australis