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

In molecular outflows from forming low-mass protostars, most oxygen isexpected to be locked up in water. However, Herschel observations have shownthat typically an order of magnitude or more of the oxygen is still unaccountedfor. To test if the oxygen is instead in atomic form, SOFIA-GREAT observed theR1 position of the bright molecular outflow from NGC1333-IRAS4A. The [OI] 63 umline is detected and spectrally resolved. From an intensity peak at +15 km/s,the intensity decreases until +50 km/s. The profile is similar to that ofhigh-velocity (HV) H2O and CO 16-15, the latter observed simultaneously with[OI]. A radiative transfer analysis suggests that ~15% of the oxygen is inatomic form toward this shock position. The CO abundance is inferred to be~10^-4 by a similar analysis, suggesting that this is the dominant oxygencarrier in the HV component. These results demonstrate that a large portion ofthe observed [OI] emission is part of the outflow. Further observations arerequired to verify whether this is a general trend.

Oxygen budget in low-mass protostars: the NGC1333-IRAS4A R1 shock observed in [OI] at 63 um with SOFIA-GREAT