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

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dc.citation.articleNumber90en_US
dc.citation.journalTitleThe Astronomical Journalen_US
dc.citation.volumeNumber151en_US
dc.contributor.authorArulanantham, Nicole A.en_US
dc.contributor.authorHerbst, Williamen_US
dc.contributor.authorCody, Ann Marieen_US
dc.contributor.authorStauffer, John R.en_US
dc.contributor.authorRebull, Luisa M.en_US
dc.contributor.authorAgol, Ericen_US
dc.contributor.authorWindemuth, Dianaen_US
dc.contributor.authorMarengo, Massimoen_US
dc.contributor.authorWinn, Joshua N.en_US
dc.contributor.authorHamilton, Catrina M.en_US
dc.contributor.authorMundt, Reinharden_US
dc.contributor.authorJohns-Krull, Christopher M.en_US
dc.contributor.authorGutermuth, Robert A.en_US
dc.date.accessioned2017-05-05T19:00:54Zen_US
dc.date.available2017-05-05T19:00:54Zen_US
dc.date.issued2016en_US
dc.description.abstractWe 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.en_US
dc.identifier.citationArulanantham, Nicole A., Herbst, William, Cody, Ann Marie, et al.. "Seeing Through the Ring: Near-Infrared Photometry of V582 Mon (KH 15D)." <i>The Astronomical Journal,</i> 151, (2016) IOP Publishing: https://doi.org/10.3847/0004-6256/151/4/90.en_US
dc.identifier.doihttps://doi.org/10.3847/0004-6256/151/4/90en_US
dc.identifier.urihttps://hdl.handle.net/1911/94202en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.titleSeeing Through the Ring: Near-Infrared Photometry of V582 Mon (KH 15D)en_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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