High‐Resolution Mid‐Infrared Imaging of the Asymptotic Giant Branch Star RV Bootis with the Steward Observatory Adaptive Optics System | Zendy

Beth Biller | Zendy; Laird M. Close | Zendy; A. Li | Zendy; John H. Bieging | Zendy; W. F. Hoffmann | Zendy; Philip M. Hinz | Zendy; Douglas L. Miller | Zendy; Guido Brusa | Zendy; Michael LloydHart | Zendy; F. Wildi | Zendy; D. Potter | Zendy; Benjamin D. Oppenheimer | Zendy

Open Access

High‐Resolution Mid‐Infrared Imaging of the Asymptotic Giant Branch Star RV Bootis with the Steward Observatory Adaptive Optics System

Author(s) -

Beth Biller,

Laird M. Close,

A. Li,

John H. Bieging,

W. F. Hoffmann,

Philip M. Hinz,

Douglas L. Miller,

Guido Brusa,

Michael LloydHart,

F. Wildi,

D. Potter,

Benjamin D. Oppenheimer

Publication year - 2005

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/426854

Subject(s) - strehl ratio , physics , astrophysics , asymptotic giant branch , adaptive optics , spectral energy distribution , full width at half maximum , point spread function , wavelength , point source , astronomy , galaxy , optics , stars

We present high resolution (~0.1"), very high Strehl ratio (0.97+-0.03)mid-infrared (IR) adaptive optics (AO) images of the AGB star RV Boo utilizingthe MMT adaptive secondary AO system. RV Boo was observed at a number ofwavelengths over two epochs (9.8 um in May 2003, 8.8, 9.8 and 11.7 um inFebruary 2004) and appeared slightly extended at all wavelengths. While theextension is very slight at 8.8 and 11.7 um data, the extension is somewhatmore pronounced at 9.8 um. With such high Strehls we can achievesuper-resolutions of 0.1" by deconvolving RV Boo with a point-spread function(PSF) derived from an unresolved star. We tentatively resolve RV Boo into a0.16" FWHM extension at a position angle of 120 degrees. At a distance of390(+250)(-100) pc, this corresponds to a FWHM of 60(+40)(-15) AU. We measure atotal flux at 9.8 um of 145+-24 Jy for the disk and star. Based on a dustthermal emission model for the observed IR spectral energy distribution and the9.8 um AO image, we derive a disk dust mass of 1.6x10^-6 Msun and aninclination of 30 to 45 degrees from edge-on. We discuss whether the dust diskobserved around RV Boo is an example of the early stages in the formation ofasymmetric structure in planetary nebula.Comment: 24 pages, 8 figures, accepted by Ap

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