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Published September 21, 2014 | Published
Journal Article Open

Constraining the sub-au-scale distribution of hydrogen and carbon monoxide gas around young stars with the Keck Interferometer


We present Keck Interferometer (KI) observations of T Tauri and Herbig Ae/Be stars with a spatial resolution of a few milliarcseconds and a spectral resolution of ∼2000. Our observations span the K band, and include the Brγ transition of hydrogen and the v = 2 → 0 and v = 3 → 1 transitions of carbon monoxide. For several targets, we also present data from Keck/NIRSPEC that provide higher spectral resolution, but a seeing-limited spatial resolution, of the same spectral features. We analyse the Brγ emission in the context of both disc and infall/outflow models, and conclude that the Brγ emission traces gas at very small stellocentric radii, consistent with the magnetospheric scale. However, some Brγ-emitting gas also seems to be located at radii of ≳ 0.1 au, perhaps tracing the inner regions of magnetically launched outflows. CO emission is detected from several objects, and we generate disc models that reproduce both the KI and NIRSPEC data well. We infer the CO spatial distribution to be coincident with the distribution of continuum emission in most cases. Furthermore, the Brγ emission in these objects is roughly coincident with both the CO and continuum emission. We present potential explanations for the spatial coincidence of continuum, Brγ, and CO overtone emission, and explore the implications for the low occurrence rate of CO overtone emission in young stars. Finally, we provide additional discussion of V1685 Cyg, which is unusual among our sample in showing large differences in emitting region size and spatial position as a function of wavelength.

Additional Information

© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 June 23. Received 2014 June 23; in original form 2014 May 7. This work was supported by NASA Origins grant NNXX11AK57G. JAE is also grateful for support from an Alfred P. Sloan Research Fellowship. The ASTRA programme, which enabled the observations presented here, was made possible by the ASTRA team and by funding from NSF MRI grant AST-0619965. The authors also wish to recognize and acknowledge the cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

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Published - MNRAS-2014-Eisner-1916-45.pdf


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