The AstraLux Survey of Planet Host Multiplicity
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1 The AstraLux Survey of Planet Host Multiplicity Carolina Bergfors Max-Planck-Institut für Astronomie/ IoA Cambridge University of Cambridge, Institute of Astronomy, 17 July 2013
2 The AstraLux binary TEP host survey Daemgen et al High resolution Lucky Imaging survey for stellar companions to hosts of transiting exoplanets (TEPs) discovered in ground-based surveys 31 TEP hosts observed with the two AstraLux instruments The team: C. Bergfors (MPIA), S. Daemgen (ESO/U. Toronto), W. Brandner (MPIA), S. Hippler (MPIA), B. Biller (MPIA), M. Janson (U. Toronto/Princeton), N. Kudryavtseva (MPIA), K. Geissler (Stony Brook), T. Henning (MPIA), R. Koehler (MPIA/LSW Heidelberg), F. Hormuth (MPIA)
3 Outline AstraLux and Lucky Imaging Planet formation in binary star systems Why transiting exoplanet hosts? Survey results and implications
4 Lucky Imaging with High spatial resolution in the optical with medium-sized telescopes and with short instrumental overheads: Great for multiplicity surveys! Select and combine only a fraction of a large number (~10000) very short (~10ms) integrations to produce seeing limited resolution Pioneering work at the NOT (LuckyCam): Baldwin et al. 2001, Tubbs et al. 2002, Mackay et al ms Sum ms Shift & Add 50% selection 10% selection 1% selection Hippler, Bergfors, Brandner et al. 2009
5 The AstraLux instruments AstraLux Norte: Calar Alto 2.2m, Almería, Spain NTT AstraLux Sur: 3.5m New Technology Telescope, La Silla Camera head: Electron multiplying, thinned, back-illuminated px commercial CCD Up to 34 Hz frame rate with full FoV or several 100 Hz using subarrays FoV: 16 (Sur)/ 24 (Norte) Filters: SDSS i', z' l CAHA 2.2m AstraLux
6 AstraLux sensitivity Hormuth et al Janson et al. 2012
7 Some examples Janson et al. 2012
8 Science with AstraLux Mainly surveys for stellar companions, e.g. Binary planet host stars: Bergfors et al. 2013, Lillo-Box et al. 2012, Ginski et al. 2012, Schnupp et a. 2010, Narita et al. 2010, Daemgen et al M dwarf multiplicity: Janson et al. 2012, Bergfors et al (761 late-k to mid- M dwarfs) M subdwarfs: Lodieu et al Massive stars multiplicity: Peter et al. 2012, Maíz-Apellániz et al Also relative astrometry of binaries (orbits) and highspeed photometry
9 Planets in binary star systems >50 planets orbiting one binary/multiple component (S-type) >6 circumbinary planets (P-type)
10 Planet formation in binary systems Disk truncation, heating, distortion, lifetime (e.g. Artymowicz & Lubow (1994), Armitage, Clarke & Tout (1999),Nelson (2000)) Migration rate, mass growth (e.g. Kley (2000)) Planet-planet scattering, Lidov-Kozai effect (e.g. Kozai 1962, Ford & Rasio (2008)) Core Accretion vs. Gravitational Instability (e.g. Nelson (2000), Mayer et al. (2005), Boss (2006), Duchêne 2009) 2D numerical simulations Planet properties (frequency, mass, spin-orbit, etc.) and binary properties (separation, mass-ratio, eccentricity...) provide clues to planet formation in binary systems.
11 RV planet host surveys Giant planets are more common in single star systems than in AU binaries - Eggenberger et al. (2008, 2011) ns and detection limits. Dots are true companion Eggenberger et al The most massive planets in short-period orbits and those with the highest eccentricities belong to stars in binary systems - Desidera & Barbieri (2007)
12 Secondary eclipse: Thermal radiation from planet Transit: Rp/R*, a/r*, b Terminator transmission spectrum Transiting planets provide a wealth of information!
13 Blending by another star Apparent transit depth: ΔFobs=d/Ftot True transit depth: ΔF=d/FA Dilution correction: ΔFnew=(1+10 -Δm/2.5 )ΔFold May require a correction of stellar and planetary parameters (R p /R *, a/r *, b, M p ) of a few to several tens of per cent (see e.g. Daemgen et al. 2009, Buchhave et al. 2011, Lillo-Box et al. 2012)
14 What some other TEP host surveys found: ~20% of KOI s have a companion within 2" Lillo-Box et al. 2012, Lucky Imaging of 98 KOI s Adams et al. 2012, 2013, AO-imaging of 102 KOI s 28-35% of CoRoT candidates have companions bright enough to be false positives Guenther et al. 2013, AO-imaging & NIR spectroscopy of 25 CoRoT candidates
15 New candidate companions to TEP hosts 31 TEP hosts observed with the AstraLux instruments Daemgen et al candidate companions detected within ~1" and 2 at wider separations HAT-P-8 WASP-12 Bergfors et al Previously unknown companions to TrES-2, TrES-4, HAT-P-8, WASP-12 Confirmed CPM binaries: TrES-4, WASP-2
16 Bayesian analysis suggests that the CSF is similar to that of solar-type stars in general, but that the binary separation is on average larger for planet host stars Solar-type binaries, Raghavan et al AstraLux sensitivity Max prob.
17 WASP-12 AstraLux Sur Δi' = 3.79±0.10 z' = 4.02±0.07 Transit depth deeper by mmag Rp/R* increase ~1.5% (Maciejewski et al. 2013) Bergfors et al. 2011, 2013
18 WASP-12 Crossfield et al SpT M0/M1V Photometric dilution changes some eclipses and all transit depths by >1σ Subaru/MOIRCS 2.315μm narrowband IRTF/SpeX KMKO WASP-12b is hotter and slightly larger (1-2%) than previously thought
19 Summary Lucky Imaging with the AstraLux instruments is a very efficient method for surveying stars in search for faint, close companions Results from the AstraLux binary TEP host survey include the discovery of several previously unknown companion candidates and suggest that a close companion may affect planet formation negatively Blending by a binary companion or chance projection may require a correction of parameters derived from the transit light curve by several per cent and have severe implications for atmospheric characterisation
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