dc.contributor.author | Millan-Gabet, Rafael | |
dc.contributor.author | Che, Xiao | |
dc.contributor.author | Monnier, John D. | |
dc.contributor.author | Sitko, Michael l. | |
dc.contributor.author | Russell, Ray W. | |
dc.contributor.author | Grady, Carol A. | |
dc.contributor.author | Day, Amanda N. | |
dc.contributor.author | Perry R.B. | |
dc.contributor.author | Harries, Tim J. | |
dc.contributor.author | Aarnio, Alicia N. | |
dc.contributor.author | Colavita, Mark M. | |
dc.contributor.author | Wizinowich, Peter L. | |
dc.contributor.author | Ragland, Sam | |
dc.contributor.author | Woillez, Julien | |
dc.date.accessioned | 2016-05-19T13:29:31Z | |
dc.date.issued | 2016-07-26 | |
dc.description.abstract | We present near and mid–infrared interferometric observations made with the Keck Interferometer Nuller and near–contemporaneous spectro–photometry from the IRTF of 11 well known young stellar objects, several observed for the first time in these spectral and spatial resolution regimes. With AU–level spatial resolution, we first establish characteristic sizes of the infrared emission using a simple geometrical model consisting of a hot inner rim and mid–infrared disk emission. We find a high degree of correlation between the stellar luminosity and the mid–infrared disk sizes after using near–infrared data to remove the contribution from the inner rim. We then use a semi–analytical physical model to also find that the very widely used “star + inner dust rim+ flared disk” class of models strongly fails to reproduce the SED and spatially–resolved mid–infrared data simultaneously; specifically a more compact source of mid–infrared emission is
required than results from the standard flared disk model. We explore the viability
of a modification to the model whereby a second dust rim containing smaller dust
grains is added, and find that the two–rim model leads to significantly improved fits in
most cases. This complexity is largely missed when carrying out SED modelling alone, although detailed silicate feature fitting by McClure et al. (2013) recently came to a similar conclusion. As has been suggested recently by Menu et al. (2015), the difficulty in predicting mid–infrared sizes from the SED alone might hint at “transition disk”–like gaps in the inner AU; however, the relatively high correlation found in our mid–infrared disk size vs. stellar luminosity relation favors layered disk morphologies and points to missing disk model ingredients instead. | en_GB |
dc.description.sponsorship | The authors wish to acknowledge fruitful discussions with Nuria Calvet and Melissa McClure.
Part of this work was performed while X. C. was a Visiting Graduate Student Research Fellow at
the Infrared Processing and Analysis Center (IPAC), California Institute of Technology. The Keck
Interferometer was funded by the National Aeronautics and Space Administration as part of its
Exoplanet Exploration Program. Data presented herein were obtained at the W.M. Keck Observatory,
which is operated as a scientific partnership among the California Institute of Technology,
the University of California and the National Aeronautics and Space Administration. The Observatory
was made possible by the generous financial support of the W.M. Keck Foundation. The
authors wish to recognize and acknowledge the very significant 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. Data presented in
this paper were obtained at the Infrared Telescope Facility, which is operated by the University of
Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration.
We gratefully acknowledge support and participation in the IRTF/BASS observing runs by Daryl
Kim, The Aerospace Corporation. This work has made use of services produced by the NASA Exoplanet
Science Institute at the California Institute of Technology. M. S. was supported by NASA
ADAP grant NNX09AC73G. R. W. R. was supported by the IR&D program of The Aerospace
Corporation | en_GB |
dc.identifier.citation | Vol. 826 (2), article 120 | |
dc.identifier.doi | 10.3847/0004-637X/826/2/120 | |
dc.identifier.uri | http://hdl.handle.net/10871/21611 | |
dc.language.iso | en | en_GB |
dc.publisher | American Astronomical Society | en_GB |
dc.relation.url | http://hdl.handle.net/10871/30943 | |
dc.title | Confronting standard models of proto-planetary disks with new mid-infrared sizes from the Keck Interferometer | en_GB |
dc.type | Article | en_GB |
dc.identifier.issn | 1538-4357 | |
dc.relation.isreplacedby | 10871/30943 | |
dc.relation.isreplacedby | http://hdl.handle.net/10871/30943 | |
pubs.declined | 2016-05-19T09:09:58.89+0100 | |
pubs.deleted | 2016-05-19T09:09:58.89+0100 | |
pubs.merge-to | 10871/30943 | |
pubs.merge-to | http://hdl.handle.net/10871/30943 | |
dc.description | This is the author accepted manuscript. The final version is available from American Astronomical Society/IOP Publishing via the DOI in this record. | |
dc.description | The published version is in ORE at http://hdl.handle.net/10871/30943 | |
dc.identifier.journal | Astrophysical Journal | en_GB |