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Keck Interferometer Observations of FU Orionis Objects
We present new K-band long-baseline interferometer observations of threeyoung stellar objects of the FU Orionis class, namely, V1057 Cyg, V1515Cyg, and Z CMa-SE, obtained at the Keck Interferometer during itscommissioning science period. The interferometer clearly resolves thesource of near-infrared emission in all three objects. Using simplegeometric models, we derive size scales (0.5-4.5 AU) for this emission.All three objects appear significantly more resolved than expected fromsimple models of accretion disks tuned to fit the broadband optical andinfrared spectrophotometry. We explore variations in the key parametersthat are able to lower the predicted visibility amplitudes to themeasured levels and conclude that accretion disks alone do not reproducethe spectral energy distributions and K-band visibilitiessimultaneously. We conclude that either disk models are inadequate todescribe the near-infrared emission or additional source components areneeded. We hypothesize that large-scale emission (tens of AU) in theinterferometer field of view is responsible for the surprisingly lowvisibilities. This emission may arise in scattering by large envelopesbelieved to surround these objects.
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Observation and Astrometry data
| Constellation: | Κύκνος |
| Right ascension: | 20h48m16.30s |
| Declination: | +44°04'35.9" |
| Apparent magnitude: | 8.787 |
| Distance: | 295.858 parsecs |
| Proper motion RA: | -10.1 |
| Proper motion Dec: | 6.8 |
| B-T magnitude: | 10.638 |
| V-T magnitude: | 8.94 |
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