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Stockholm University, Faculty of Science, Department of Astronomy. American Museum of Natural History, USA.
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Number of Authors: 7
2016 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 826, no 2, 165Article in journal (Refereed) Published
Abstract [en]

We have carried out two sets of observations to quantify the properties of SiO gas in the unusual HD 172555 debris disk: (1) a search for the J = 8-7 rotational transition from the vibrational ground state, carried out with the Atacama Pathfinder EXperiment (APEX) submillimeter telescope and heterodyne receiver at 863 mu m. and (2) a search at 8.3 mu m for the P(17) ro-vibrational transition of gas phase SiO, carried out with the Very Large Telescope (VLT)/VISIR with a resolution, lambda/Delta lambda, of 30,000. The APEX measurement resulted in a 3.3 sigma detection of an interstellar feature, but only an upper limit to emission at the radial velocity and line width expected from HD 172555. The VLT/VISIR result was also an upper limit. These were used to provide limits for the abundance of gas phase SiO. for a range of temperatures. The upper limit from our APEX detection, assuming an 8000 K primary star photospheric excitation, falls more than an order of magnitude below the self-shielding stability threshold derived by Johnson et al. (2012). Our results thus favor a solid-state origin for the 8.3 mu m feature seen in the Spitzer IRS spectrum of the circumstellar excess emission. and the production of circumstellar O I and Si I by SiO UV photolysis. The implications of these estimates are explored in the framework of models of the HD 172555 circumstellar disk.

Place, publisher, year, edition, pages
2016. Vol. 826, no 2, 165
Keyword [en]
circumstellar matter, stars: individual (HD 172555), submillimeter: planetary systems, techniques: spectroscopic
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-134448DOI: 10.3847/0004-637X/826/2/165ISI: 000381977900065OAI: diva2:1033848
Available from: 2016-10-10 Created: 2016-10-06 Last updated: 2016-10-10Bibliographically approved

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