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Searching for Planets in “Holey Debris Disks”

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Searching for Planets in “Holey Debris Disks” Searching for Planets in ! “Holey Debris Disks”" Tiffany Meshkat, M. Kenworthy, V. Bailey, " K. Y. L. Su, P. Hinz, E. Mamajek " In Prep " Direct Imaging" • Goals:" – differentiate between formation mechanisms" – learn about the composition" • Very few directly imaged planets" HR 8799 bcde, Marois et al. 2008, 2010" Fomalhaut b, Kalas et al. 2008" exoplanets.org | 7/28/2014 10 1 0.1 Transits Radial Velocity Microlensing Direct Imaging Planet Mass [Jupiter Mass] Planet Mass [Jupiter 0.01 10-3 0.01 0.1 1 10 100 Separation [Astronomical Units (AU)] Completed direct imaging surveys" • NICI survey: Biller et al. 2013, Wahhaj et al. 2013, Nielsen et al. 2013" • NACO Large Program: Desidera et al. 2014, Chauvin et al. 2014" • IDPS: Vigan et al. 2012" • SEEDS: Brandt et al. 2014, Janson et al. 2013" • M star based surveys: Bowler et al. 2013, Delorme et al. 2013" Common direct imaging targets" • Massive stars" • Nearby, young" • Debris disk systems" • Etc…" Anything which makes the planet brighter Signposts for planets" HR 8799" cold outer belt" b" c" warm inner belt! e" d" Su et al. 2013" “Holey Debris Disks” Project" 1. Disk structure implies presence of companions" 2. If planets are found, use disk to constrain properties " Su et al. in prep" Facilities" • VLT NACO/APP coronagraph • LBTI LMIRCAM" • MagAO CLIO" • Gemini NICI" Su et al. in prep" Su et al. in prep" Two planets detected!" HD 95086 b" Rameau et al. 2013! H-band NICI/Gemini Data" • Very deep dataset (~3 hours)" " • March 2012" Dec (“) • Processed with # optimized PCA (Meshkat et al. 2014)" • Non-detection" # RA (“)" Which models are detectable?" T dwarf=11.6 mag" Cloud free=12 mag" Some clouds=12.5 mag" PCA Contrast Curve" " ] T dwarf" mag Cloud-free planet " Partly-cloudy planet " contrast H [ $ 5 H-L’ lower limit of 3.1±0.5 mag at 5σ Radius [arcsec]" Color-magnitude diagram" H-L’ < 3.1 mag at 5σ Meshkat et al. 2013" Color-magnitude diagram" H-L’ = 3.6 mag at 5σ Galicher et al. 2014" HD 95086 disk structure" Cold outer belt" Warm inner belt" 64 AU" 8 AU" ? b Su et al. in prep (see poster)" HD 95086 L’ Mass Limit Meshkat et al. in prep HD 106906 b J K L Clio S, Clio !Clio N 1" E Bailey et al. 2014! 4 5 3 0 2 1 −5 0 606W H L! ACS 2, NICI Clio 0 2 4 6 −10 −5 0 5 10 0.25 7.5 0.2 2013−04−04 2011−03−21 (if bkgd) (bkgd sources) 8 0.15 8.5 0.1 2004−12−01 0.05 (reference 9 2011−03−21 position) (if bkgd) contrast [mag] 0 σ 9.5 5 ! 2013−04−04 L Relative Dec [arcsec] −0.05 δ (HD 106906 b) 10 2011−03−21 −0.1 (HD 106906 b) 10.5 0 1 2 3 0.4 0.3 0.2 0.1 0 −0.1 separation [arcsec] δ Relative RA [arcsec] HD 106906 disk structure 115 AU ? 17 AU Bailey et al. 2014 HD 106906 L’ Mass Limit Bailey et al. 2014 Unanswered questions Cold outer belt Warm inner belt 64 AU 115 AU 8 AU ? ? 17 AU b HD 95086 HD 106906 Why the success? • L’-band • Apodized Phase Plate coronagraph • Well selected targets • Optimized Principal Component Analysis • Luck! Conclusions (so far) • Holey debris disks are good targets to search for planets (2 out of 15 targets) • Well characterized disks provide wealth of information once companions are found • Need GPI and SPHERE to reach better sensitivity limits around the remaining targets .
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