S21B0052

Understanding the mechanisms of mass accretion and jet ejection is one of the key issues of star formation theories. However, observational studies are hampered by the limited angular resolutions of current telescopes, which are not sufficient to resolve structure and kinematics in the jet launching region. We are therefore pursuing an alternative approach to tackle this important issue: long-term monitoring of mass accretion and jet ejection for active young stars. Our observations since 2010 include (1) IFU imaging spectroscopy of extended jets using Gemini-NIFS; (2) optical high-resolution spectroscopy using CFHT-ESPaDOnS to observe gas kinematics very close to the star (≪0.1 AU); and (3) optical photometry to monitor changes in mass accretion rates with high time resolution. Following promising results to date, we propose to extend the approved intensive program with Gemini-NIFS (17B36I) for another three years (21B, 22B, 23B) to complete the project. The new data set will allow us to clarify the presence/absence of the time correlation between jet ejection and mass accretion onto the star, and therefore their physical link and the driving mechanism of the jet.

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