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27 April 2024 |
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A Thermal Infrared Imaging Study of Very Low-Mass, Wide Separation Brown Dwarf Companions to Upper Scorpius Stars: Constraining Circumstellar Environments | | Vanessa Bailey
; Philip M. Hinz
; Thayne Currie
; Kate Y. L. Su
; Simone Esposito
; John M. Hill
; William F. Hoffmann
; Terry Jones
; Jihun Kim
; Jarron Leisenring
; Michael Meyer
; Ruth Murray-Clay
; Matthew J. Nelson
; Enrico Pinna
; Alfio Puglisi
; George Rieke
; Timothy Rodigas
; Andrew Skemer
; Michael F. Skrutskie
; Vidhya Vaitheeswaran
; John C. Wilson
; | | Date: |
4 Feb 2013 | | Abstract: | We present a 3-5um LBT/MMT adaptive optics imaging study of three Upper
Scorpius stars with brown dwarf (BD) companions with very low-masses/mass
ratios (M_BD < 25M_Jup; M_BD / M_star ~ 1-2%), and wide separations (300-700
AU): GSC 06214, 1RXS 1609, and HIP 78530. We combine these new thermal IR data
with existing 1-4um and 24um photometry to constrain the properties of the BDs
and identify evidence for circumprimary/secondary disks in these unusual
systems. We confirm that GSC 06214B is surrounded by a disk, further showing
this disk produces a broadband IR excess due to small dust near the dust
sublimation radius. An unresolved 24um excess in the system may be explained by
the contribution from this disk. 1RXS 1609B exhibits no 3-4um excess, nor does
its primary; however, the system as a whole has a modest 24um excess, which may
come from warm dust around the primary and/or BD. Neither object in the HIP
78530 system exhibits near- to mid-IR excesses. We additionally find that the
1-4um colors of HIP 78530B match a spectral type of M3+-2, inconsistent with
the M8 spectral type assigned based on its near-IR spectrum, indicating it may
be a low-mass star rather than a BD. We present new upper limits on additional
low-mass companions in the system (<5M_Jup beyond 175AU). Finally, we examine
the utility of circumsecondary disks as probes of the formation histories of
wide BD companions, finding that the presence of a disk may disfavor BD
formation near the primary with subsequent outward scattering. | | Source: | arXiv, 1302.0582 | | Services: | Forum | Review | PDF | Favorites | |
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