Gas Inside the 97 AU Cavity around the Transition Disk Sz 91
Author
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Canovas, H.
Author
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Schreiber, M. R.
Author
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Cáceres, C.
Author
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Ménard, Francois
Author
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Pinte, Christophe
Author
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Mathews, G.
Author
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Cieza, L.
Author
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Casassus Montero, Simón
Author
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Hales, A.
Author
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Williams, J. P.
Author
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Román, P.
Author
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Hardy, A.
Admission date
dc.date.accessioned
2015-06-16T19:32:33Z
Available date
dc.date.available
2015-06-16T19:32:33Z
Publication date
dc.date.issued
2015-05-20
Cita de ítem
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The Astrophysical Journal, 805:21 (11pp), 2015 May 20
en_US
Identifier
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doi:10.1088/0004-637X/805/1/21
Identifier
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https://repositorio.uchile.cl/handle/2250/131141
General note
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Artículo de publicación ISI
en_US
Abstract
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We present ALMA (Cycle 0) band 6 and band 3 observations of the transition disk Sz 91. The disk inclination and
position angle are determined to be i = 49◦
. 5 ± 3◦
. 5°and PA = 18◦
. 2 ± 3◦
. 5 and the dusty and gaseous disk are
detected up to ∼220 and ∼400 AU from the star, respectively. Most importantly, our continuum observations
indicate that the cavity size in the millimeter-sized dust distribution must be ∼97 AU in radius, the largest cavity
observed around a T Tauri star. Our data clearly confirm the presence of 12CO (2–1) well inside the dust cavity.
Based on these observational constraints we developed a disk model that simultaneously accounts for the 12CO and
continuum observations (i.e., gaseous and dusty disk). According to our model, most of the millimeter emission
comes from a ring located between 97 and 140 AU. We also find that the dust cavity is divided into an innermost
region largely depleted of dust particles ranging from the dust sublimation radius up to 85 AU, and a second,
moderately dust-depleted region, extending from 85 to 97 AU. The extremely large size of the dust cavity, the
presence of gas and small dust particles within the cavity, and the accretion rate of Sz 91 are consistent with the
formation of multiple (giant) planets.