Thayne  Currie,  Olivier  Guyon,  Nemanja  Jovanovic,  

Julien  Lozi,  Eugenio  Garcia,  Taichi  Uyama  

Imaging  and  Characterizing  Exoplanets    (and  Disks)  with  SCExAO:    

First  Results  and  Future  Prospects  

Directly-­‐Imaged  Planets  

(Marois et al. 2008, 2010; Kalas et al. 2008; Lagrange et al. 2010; Kraus & Ireland 2012; Sallum et al. 2015; Carson et al. 2013; Rameau et al. 2013; Kuzuhara et al. 2013; Currie et al. 2014; Quanz et al. 2013; Currie et al. 2015; Macintosh et al. 2015)

SCExAO  Project:    An  Extreme  AO  System  on  Maunakea  

   

•  Extreme  AO  Imager  for  Subaru    

•  S.R.  ~    90+%  at  H  band  (by  July  2016)  

•  1200  modes,  3.5  kHz,  1  ms  latency  

•  AddiQonal  Strengths:  excepQonal  site;  small  IWA  (1-­‐3  lambda/D)  capability  

                     

Extreme  AO  vs.  Site  CondiQons  GPIES  Contrasts,  ASDI,  Processed  with  KLIP    (R.  DeRosa,  J.  Wang)    Planet  DetecQon  SensiQve  to  Atmospheric  CondiQons?    

(from  TMT  site  tesQng  results)    

Extreme  AO  close  to  1  lambda/D  

T. Currie 2016, in prep

SCExAO:  Current  PSF  Quality  &  Contrast  

S.R.  ~  0.7    (0.9  in  short  exp)  

H  band/1.6  microns  

Emerging  Dark  Hole  (r  ~0.45—0.8”)  

SCExAO:  First  Science  Results  HD  1160  B:    

Young,  Low-­‐Mass  Substellar  Companion  

Garcia, Currie, & Guyon et al. (2016)

Garcia, Currie, & Guyon et al. (2016)

HD  1160  B  SED  Modeling  

HD  1160  B  SED  Modeling  •  Teff  =  3000-­‐3100  K,  log(g)  =  4—4.5,  M  ~  30-­‐90  Mj  •  Solar  Metallicity  

SCExAO:  First  Science  Results,  part  2  The  directly-­‐imaged  planet  kappa  Andromedae  b  

 

SNR  ~  105;  IWA  ~  0.37”  

(Currie,  Guyon,  et  al.  in  prog.)  

Kappa  And  b  SED  Modeling  •  Teff  =  1675—1950  K,  log(g)  =  3.8—4.25  favored  •  More  consistent  with  planet  interpretaQon,  not  massive  brown  dwarf  

SCExAO  SNRE  ~  5-­‐7  to  0.3”  

SEEDS/HiCIAO  SNRE  ~2-­‐5  to  0.5”  

SCExAO:  First  Science  Results,  part  3  The  HIP  79977  Debris  Disk  

Future Prospects: Exoplanet/Disk Characterization with SCExAO+CHARIS

JHK  integral  field  spectrograph  (delivered  to  Subaru  in  April  2016)  •  Low-­‐resoluQon  ‘discovery’  mode  (R  ~15-­‐20),  full  JHK  bandpass  •  High-­‐resoluQon  ‘characterizaQon’  mode  (R  ~  70-­‐90);  invesQgate  

exoplanet    clouds  (e.g.  Currie  et  al.  2011)  or  disk  composiQon  (e.g.  Rodigas  et  al.  2015)    

R80

New Exoplanet Survey (SEEDS v. 2.0?) Direct Imaging + Radial Velocity

SCExAO+CHARIS    Direct  Imaging    (good  seeing)  

IRD  Radial-­‐Velocity    (below  average  seeing)  

Speckle  Nulling  DemonstraQon  w/  SCExAO    (Goal:  1  kHz  acQve  speckle  control)  

-­‐  -­‐  speckle  nulling:  -­‐  A  replacement/complement  

to  ADI/SDI  at  small  lambda/D  

Martinache et al. (2014); Mazin et al. (2013)

Future Prospects: “Next-Generation Extreme AO” Capabilities

       -­‐  fast,  focal  plane  wavefront  sensing    MKIDS  detector  (MEC)  

       à  1e-­‐7  to  1e-­‐8  contrasts  at                    several  lambda/D  

Future  Prospects:    Imaging  Reflected-­‐Light  Planets  with  SCExAO+MEC  (early  2020s)  

1  Mj  at  1  AU  around  Vega  

20  Mj  Brown  Dwarf/Super  Jupiter  at  1  AU  around  Vega  

Discovery  Space  for  SCExAO/MEC  

Summary  •  SCExAO:  Subaru’s  Extreme-­‐AO  System:  

Key  Strengths:  best  site,  small  lambda/D  sensiQvity  

•  Performance:  closing  gap  with  leading  extreme  AO  systems  

 

•  First  Science:  Characterizing  the  atmospheres  to  HD  1160  B  and  kappa  And  b;  characterizing  debris  disk  around  HIP  79977  

•  Future  Prospects:  Direct  imaging/spectroscopy  survey;  next-­‐gen  extreme  AO;  imaging  planets  in  reflected  light