Mid-Infrared Substellar Companion Mass Limits for Nearby Planet-Host Stars

ORAL

Abstract

The sensitivity of the Infrared Array Camera on NASA's Spitzer Space Telescope at 4.5 $\mu$m provides the ability to use direct imaging to capture light from brown dwarfs expected to have peak emission in this band. Using PSF subtraction techniques, we can detect sources with better than 10$^{4}$ contrast at separations as close as 12 arcseconds. Potential substellar companions can be identified from their characteristically red colors between the 3.6 and 4.5 $\mu$m photometric bands. In a sample of 14 nearby stars already found to have planetary companions from radial velocity searches, we found no sources consistent with substellar-mass companion colors within 20 arcseconds of the stars. This corresponds to 4.5 $\mu$m upper limits for objects of 5 Jupiter masses at 1 Gyr age and 10 pc distance. I will present a description of the point spread function and artifact subtraction process necessary to achieve this result.

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Authors

  • Alan Hulsebus

    Iowa State University

  • John Gaddy

    University of Southern California, University of Chicago, University of Toronto, Argonne National Laboratory, Illinois Institute of Technology, University of Northern Iowa, Universite Aix-Marseille 1, Universite Montpellier 2, University of Missouri, University of Missouri, Department of Physics and Astronomy and the Missouri Research Reactor, University of Missouri, Department of Physics and Astronomy, University of Missouri, the Missouri Research Reactor, Columbia Univ, Univ of Northern Iowa, University of Charleston, NASA Goddard Space Flight Center, Iowa State University, University of Colorado, NOAO, University of Toledo, University of Massachusetts, Smith College, Observatory of Bordeaux, Spitzer Science Center, University of Chile, SAO

  • John Gaddy

    University of Southern California, University of Chicago, University of Toronto, Argonne National Laboratory, Illinois Institute of Technology, University of Northern Iowa, Universite Aix-Marseille 1, Universite Montpellier 2, University of Missouri, University of Missouri, Department of Physics and Astronomy and the Missouri Research Reactor, University of Missouri, Department of Physics and Astronomy, University of Missouri, the Missouri Research Reactor, Columbia Univ, Univ of Northern Iowa, University of Charleston, NASA Goddard Space Flight Center, Iowa State University, University of Colorado, NOAO, University of Toledo, University of Massachusetts, Smith College, Observatory of Bordeaux, Spitzer Science Center, University of Chile, SAO

  • John Gaddy

    University of Southern California, University of Chicago, University of Toronto, Argonne National Laboratory, Illinois Institute of Technology, University of Northern Iowa, Universite Aix-Marseille 1, Universite Montpellier 2, University of Missouri, University of Missouri, Department of Physics and Astronomy and the Missouri Research Reactor, University of Missouri, Department of Physics and Astronomy, University of Missouri, the Missouri Research Reactor, Columbia Univ, Univ of Northern Iowa, University of Charleston, NASA Goddard Space Flight Center, Iowa State University, University of Colorado, NOAO, University of Toledo, University of Massachusetts, Smith College, Observatory of Bordeaux, Spitzer Science Center, University of Chile, SAO