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Seeing Through the Ring: Near-infrared Photometry of V582 Mon (KH 15D)

Arulanantham, Nicole A. and Herbst, William and Cody, Ann Marie and Stauffer, John R. and Rebull, Luisa M. and Agol, Eric and Windemuth, Diana and Marengo, Massimo and Winn, Joshua N. and Hamilton, Catrina M. and Mundt, Reinhard and Johns-Krull, Christopher M. and Gutermuth, Robert A. (2016) Seeing Through the Ring: Near-infrared Photometry of V582 Mon (KH 15D). Astronomical Journal, 151 (4). Art. No. 90. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20160603-130943808

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Abstract

We examine the light and color evolution of the T Tauri binary KH 15D through photometry obtained at wavelengths between 0.55 and 8.0 μm. The data were collected with A Novel Dual Imaging CAMera (ANDICAM) on the 1.3 m SMARTS telescope at Cerro-Tololo Inter-American Observatory and with InfraRed Array Camera on the Spitzer Space Telescope. We show that the system's circumbinary ring, which acts as a screen that covers and uncovers different portions of the binary orbit as the ring precesses, has reached an orientation where the brighter component (star B) fully or nearly fully emerges during each orbital cycle. The fainter component (star A) remains fully occulted by the screen at all phases. The leading and trailing edges of the screen move across the sky at the same rate of ~15 m s^(−1), consistent with expectation for a ring with a radius and width of ~4 au and a precession period of ~6500 years. Light and color variations continue to indicate that the screen is sharp edged and opaque at VRIJH wavelengths. However, we find an increasing transparency of the ring edge at 2.2, 3.6, and 4.5 μm. Reddening seen at the beginning of the eclipse that occurred during the CSI 2264 campaign particularly suggests selective extinction by a population of large dust grains. Meanwhile, the gradual bluing observed while star B is setting is indicative of forward scattering effects at the edge of the ring. The spectral energy distribution of the system at its bright phase shows no evidence of infrared excess emission that can be attributed to radiation from the ring or other dust component out to 8 μm.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/0004-6256/151/4/90DOIArticle
http://iopscience.iop.org/article/10.3847/0004-6256/151/4/90/metaPublisherArticle
http://arxiv.org/abs/1602.01877arXivDiscussion Paper
ORCID:
AuthorORCID
Cody, Ann Marie0000-0002-3656-6706
Stauffer, John R.0000-0003-3595-7382
Rebull, Luisa M.0000-0001-6381-515X
Agol, Eric0000-0002-0802-9145
Marengo, Massimo0000-0001-9910-9230
Winn, Joshua N.0000-0002-4265-047X
Gutermuth, Robert A.0000-0002-6447-899X
Additional Information:© 2016 The American Astronomical Society. Received 2015 October 3; accepted 2016 February 2; published 2016 March 9. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. It has also made use of the 1.3 m telescope operated by the SMARTS consortium at Cerro Toloto Interamerican Observatory in Chile. We are grateful for funding from the CT Space Grant Consortium that partially supported this research. We are grateful to Wesleyan undergraduate student Rachel Aronow for her help with this project.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Connecticutt Space Grant ConsortiumUNSPECIFIED
Subject Keywords:open clusters and associations: individual (NGC 2264) – protoplanetary disks – stars: individual (KH15D) – stars: pre-main sequence
Issue or Number:4
Record Number:CaltechAUTHORS:20160603-130943808
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160603-130943808
Official Citation:Nicole A. Arulanantham et al 2016 The Astronomical Journal 151 90
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:67653
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 Jun 2016 20:31
Last Modified:01 Nov 2019 21:20

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