Table Of Content

Exploring the Formation and Evolution of Planetary Systems Proceedings IAU Symposium No. 299, 2013 (cid:13)c 2013International AstronomicalUnion Brenda Matthews & James Graham, eds. DOI:00.0000/X000000000000000X LEECH: A 100 Night Exoplanet Imaging Survey at the LBT Andrew Skemer1, Daniel Apai1, Vanessa Bailey1, Beth Biller2, Mickael Bonnefoy2, Wolfgang Brandner2, Esther Buenzli2, Laird Close1, Justin Crepp3, Denis Defrere1, Silvano Desidera4, Josh Eisner1, Simone Esposito5, Jonathan Fortney6, Thomas Henning2, Phil Hinz1, Karl-Heinz Hofmann7, Jarron Leisenring1,8, Jared Males1, Rafael Millan-Gabet9, Katie Morzinski1, Apurva Oza10, Ilaria 4 Pascucci11, Jenny Patience12, George Rieke1, Dieter Schertl7, Joshua 1 0 Schlieder2, Mike Skrutskie10, Kate Su1, Gerd Weigelt7, Charles E. 2 Woodward13, and Neil Zimmerman2 n 1Steward Observatory,Department of Astronomy,University of Arizona a 2Max Planck Institutefor Astronomy J 3Department of Physics, NotreDame University 2 4Osservatorio Astronomico diPadova, Istituto Nazionale diAstrofisica 5Osservatorio Astrofisico di Arcetri, IstitutoNazionale di Astrofisica ] 6Department of Astronomy and Astrophysics, University of California, Santa Cruz P 7Max Planck Institutefor RadioAstronomy E 8Institutefor Astronomy,Eldgenossische Technische HochschuleZurich . 9NASAExoplanet Science Institute,California Instituteof Technology h 10Departmentof Astronomy,University of Virginia p 11Department of Planetary Sciences, Lunar and Planetary Laboratory, Universityof Arizona - 12School of Earth and Space Exploration, Arizona StateUniversity o 13Minnesota Institutefor Astrophysics, University of Minnesota r t s a Abstract.InFebruary2013,theLEECH(LBTIExozodiExoplanetCommonHunt)surveybe- [ ganits100-nightcampaignfromtheLargeBinocularTelescopeatopMountGrahaminArizona. 1 LEECH neatlycomplementsotherhigh-contrast planetimaging effortsbyobservingstarsin L’ v band (3.8 microns) as opposed to the shorter wavelength near-infrared bands (1–2.3 microns). 1 This part of the spectrum offers deeper mass sensitivity for intermediate age (several hundred 8 Myr-old) systems, since their Jovian-mass planets radiate predominantly in the mid-infrared. 4 In this proceedings, we present the science goals for LEECH and a preliminary contrast curve 0 from some early data. . 1 Keywords. instrumentation: adaptiveoptics, (stars:) planetary systems, surveys 0 4 1 Discovering Adolescent Exoplanets: Most exoplanet imaging surveys operate in : v the near-infrared(H-band; 1.65 µm), which provides the best contrasts at small separa- i X tions. However, self-luminous exoplanets emit most of their light at longer wavelengths, and this becomes more important as exoplanets age and lose the residual energy from r a theirformation.Byoperatinginthemid-infrared(L;3.8µm)LBTIissensitivetoplanets aroundolderstars(seeFigure1).ThiswillallowLEECHtodiscoveradolescentexoplan- ets around nearby stars, complementing the young samples discovered by other surveys (seeFigure2),suchasGPI,SPHERE,SEEDS,andProject1640(Macintoshetal.2008, Beuzit et al. 2008, Tamura 2009, Hinkley et al. 2011) Connecting Planets with Disks: Using the two LBTI science camerasin parallel, LEECH and HOSTS (see paper by Defrere et al. in these proceedings) will search for giant planets and inner debris disks simultaneously. The LEECH and HOSTS samples 1 2 Andrew Skemer includeverynearbystarsthathavebeentargetedbyotherrelevantsurveys(Doppler-RV planetsearchesandouterdebrisdiskstudies).Combiningthisdata,willprovidethefirst comprehensive view of exoplanetary systems. Characterizing Exoplanet Atmospheres: Earlyobservationssuggestthatdirectly imaged planets have different colors and spectra than their field brown-dwarf analogs. By studying planets with LBTI’s broad wavelength coverage (1-13µm) and over a wide age range, LEECH will characterize the bulk atmospheric properties and evolution of extrasolar planets. Figure1.LEFT:AfirstlightimagefromLEECHwiththestarremovedandanartificialplanet inserted. The artificial planet is 13 magnitudes fainter than the star at a separation of 0.75”, equivalenttoa3Mjup planet 7.5 AUfrom a0.5 Gyrsolar typestarat 10 pc.LEECH’s ability toimage olderexoplanetsthanothersurveyswill extendourknowledgeofexoplanetevolution. RIGHT: ADI+PCA (KLIP) detection limits for a bright star with 2 hours integration time on 1 telescope (preliminary). Figure 2. Planet mass versus semi-major axis for the known exoplanets and planetary mass companions listed in www.exoplanet.eu shown as small circles for radial velocity detections, large circles for imaging, and stars for imaged planets around HR 8799, β Pic, and Fomalhaut. Themedian planetmass sensitivities areshown fortheGPIA-andF-starsample, theLEECH sample, and an A-star search (Vigan et al. 2012) with NaCo/NIRI. Both GPI and LEECH will explore the critical missing link between radial velocity searches and current AO imaging surveys. References Beuzit, J.-L., Feldt, M., Dohlen, K., et al. 2008, SPIE, 7014 Hinkley,S.,Oppenheimer, B. R., Zimmerman, N., et al. 2011, PASP, 123, 74 Macintosh, B. A., Graham, J. R., Palmer, D.W., et al. 2008, SPIE, 7015 Tamura, M. 2009, AIPC,1158, 11 Vigan, A., Patience, J., Marois, C., et al. 2012, A&A, 544, A9