From the Rise of Metals to !
Water for Habitable Worlds!

NASA	  STDT:	  	  The	  Origins	  Space	  Telescope	

Itsuki	  Sakon	  (University	  of	  Tokyo),	  	  Origins	  Space	  Telescope	  (OST)	  STDT	  	  Origins	  Space	  Telescope	  STDT	Community	  Chairs:	  	  Margaret	  Meixner,	  STSCI,	  Asantha	  Cooray,	  UC	  Irvine	  NASA	  Study	  Center:	  	  Goddard	  Space	  Flight	  Center	  (GSFC):	  Ruth	  Carter,	  David	  Leisawitz,	  Johannes	  Staguhn,	  Michael	  Dipirro,	  	  Anel	  Flores,	  Joseph	  Howard,	  James	  CorseD,	  Andrew	  Jones,	  James	  Kellog,	  Louis	  Fantano	  NASA	  Head	  Quarters	  Program	  ScienIsts	  (non-­‐voIng):	  	  KarIk	  Sheth	  and	  Dominic	  Benford	  Ex	  oﬃcio	  non-­‐voIng	  representaIves:	  	  Susan	  Neﬀ	  &	  Deborah	  PadgeQ,	  NASA	  Cosmic	  Origins	  Program	  Oﬃce;	  Susanne	  Alato,	  SNSB;	  Douglas	  ScoQ,	  CAS;	  Maryvonne	  Gerin,	  CNES;	  Itsuki	  Sakon,	  JAXA;	  Frank	  Helmich,	  SRON;	  	  Roland	  Vavrek,	  ESA;	  Karl	  Menten,	  	  DLR;	  Sean	  Carey,	  IPAC	  Members	  appointed	  by	  NASA	  (>	  90	  applicaIons):	  Lee	  Armus,	  NASA	  IPAC;	  Cara	  BaQersby,	  Harvard-­‐Smithsonian	  CfA;	  Edwin	  Bergin,	  University	  of	  Michigan;	  MaU	  Bradford,	  NASA	  JPL;	  Kim	  Ennico-­‐Smith,	  NASA	  Ames;	  Gary	  Melnick,	  Harvard-­‐Smithsonian	  CfA;	  Stefanie	  Milam,	  NASA	  GSFC;	  Desika	  Narayanan,	  University	  of	  Florida;	  Klaus	  Pontopiddan,	  STSCI;	  Alexandra	  Pope,	  University	  of	  MassachuseUs;	  Thomas	  Roellig,	  NASA	  Ames;	  Karin	  Sandstrom,	  UC,	  San	  Diego;	  Kate	  Y.	  L.	  Su,	  University	  of	  Arizona;	  Joaquin	  Vieira,	  University	  of	  Illinois,	  Urbana	  Champaign;	  Edward	  Wright,	  UC	  Los	  Angeles;	  Jonas	  Zmuidzinas,	  Caltech	  Origins Space Telescope• 2020 Decadal• 9.3m single aperture• off-axis telescope with a primary composed of37 lightweight hexagonal segments• 5—600µm (TBD)• Actively cooled to <6K• Diffraction Limited at 20µmHerschel

SPICA

AKARI warm AKARI

SpitzerWarm Spitzer
2010

Origins

JWST
JWSTWFIRST
20202030

Science	  Cases	  for	  OST	Top 14 Killer Apps.
- The Rise of Metals- Water Content of Planet-Forming Disks- The First Dust
- Direct Detection of Protoplanetary Disk Masses- Super Earth Biosignatures And Climates- Water Transport to Terrestrial Planetary Zone
- Connection Between BH Growth and Star Formation Over Cosmic Time- Birth of Galaxies During Cosmic Dark Ages
- Galaxy Feedback from SNe and AGN to z~3- Thermo-Chemical History of Comets and Water Delivery to Earth- Star Formation and Multiphase ISM at Peak of Cosmic Star Formation- Magnetic Fields and Turbulence - Role in Star Formation- Galaxy Feedback Mechanisms at z<1- Survey of Small Bodies in the Outer Solar System	Baseline	  sets	  of	  Instruments	  studied	  for	  OST	Instrument	Wavelength	  Spectral	  Field	  of	  View	  Coverage	  (µm)	 ResoluIon	  (λ/Δλ)	 #	  SpaIal	  Pixels	

Typical	  Required	  SensiIvity	

Other	Low-­‐Res	  35	  to	  500	Spectrometer	

Low-­‐res	  ~	  500	  High-­‐res	  ~	  104	100	  per	  channel	

10-­‐21	  W/m2	  (spectral	  line)	

MulI-­‐channel	

High-­‐Res	  50	  to	  500	Spectrometer	

Low-­‐res	  ~	  8x104	  High-­‐res	  ~	  5x105	

100	

10-­‐21	  W/m2	  (spectral	  line)	

Photo-­‐counIng	

Heterodyne	  150	  to	  500	Spectrometer		  ~	  107	

10-­‐100		  2	  mK	  in	  0.2	   Polarized,	  	  km/s	  @1THz	 background	  limited	

Far-­‐Infrared	  Imager	35	  to	  500	

15	

100,000	

1µJy–10mJy	  	   5	  to	  10	  channels	  (confusion	  Polarimetry	  limit)	
Spectral	  line	  ﬁlters	Mid-­‐Infrared	  Imager,	  Spectrometer,	  Coronagraph	6	  to	  40	Imager	  ~	  15	  Spectrometer	  >	  500,	  2x104	

106	

Photometric	   Coronagraph	  ~	  1µJy@10µm	 10-­‐6	  	  @	  0.5”,	  10	  µm	  Transit	  Spectroscopy	From the Rise of Metals to !
Water for Habitable Worlds!

Mission	  Concept	  Studies	  for	  the	  2020	  Decadal	  Survey	  ;	  	  	  Mid-­‐Infrared	  Imager	  and	  Spectrometer	  (MISC)	  	  for	  the	  Origins	  Space	  Telescope	  (OST)	

Itsuki	  Sakon	  (University	  of	  Tokyo),	  Thomas	  L.	  Reollig,	  Kimberly	  Ennico-­‐Smith	  (NASA	  Ames)	  Taro	  Matsuo	  (Osaka	  University),	  Yuji	  Ikeda	  (Photocoding),	  Tomoyasu	  Yamamuro	  (Optcrao),	  Naofumi	  Fujishiro	  (Teikyo	  University),	  Keigo	  Enya	  (ISAS/JAXA),	  Olivier	  Guyon	  (Univ.	  of	  Arizona/	  NINS	  ABC),	  Takayuki	  Kotani	  (NAOJ),	  Jun	  Nishikawa	  (NAOJ)	  OST/MISC	  Team,	  Origins	  Space	  Telescope	  (OST)	  STDT	  	AcIvity	  and	  Schedule	
By	  Weekly	  OST	  STDT	  telecon	  (2016.4-­‐)	  	  By	  Weekly	  MISC	  Science	  Telecon	  (2017.3-­‐)	  Weekly	  MISC	  Instrument	  Telecon	  (2017.2-­‐)	  2016	  May	  :	  	  	  	  1st	  F2F	  STDT	  MeeIng	  (@NASA	  GSFC)	  2016	  Aug.	  :	  	  	  2nd	  F2F	  STDT	  MeeIng	  (@NASA	  GSFC)	  2016	  Nov.	  :	  	  	  3rd	  F2F	  STDT	  MeeIng	  (@Ball	  Aerospace)	  2017	  Mar.	  :	  	  	  4th	  F2F	  STDT	  MeeIng	  (@Spitzer	  Science	  Center)	  2017	  Jun.	  	  :	  	  	  5th	  F2F	  STDT	  MeeIng	  (@S.	  Dillion	  Ripley	  Center)	  2017	  Sep.	  :	  	  	  6th	  F2F	  STDT	  MeeIng	  (@Space	  Telescope	  Science	  InsItute)	
2017.	  Sep.;	  Complete	  Concept	  1	  study	  2017.	  Oct.;	  Independent	  Technical	  Review	  (ITR)	  at	  NASA	  GSFC	  2017.	  Dec.	  	  ;	  Interim	  Report	  submiUed	  to	  NASA	  HQ	

Mid-­‐Infrared	  Imager,	  Spectrometer	  and	  Coronagraph	  (MISC)	
Mid-Infrared Imager, Spectrometer,
Coronagraph (MISC) Team Members(from Science and Technology Definition Team,Ex-Officio Non-Voting Members, Internation ExOfficio Non-Voting Members)-Asantha Cooray (California, Irvine)-Deborah Padgett (GSFC)-Eric Nielsen (SETI Institute)-Itsuki Sakon (University of Tokyo) [Instrumentlead]-Joaquin Vieira (Illinois, Urbana Champaign)-Margaret Meixner (STScI)-Kimberly Ennico Smith (NASA/AMES) [Sciencelead]-Tom Roellig (NASA/AMES) [Instrument lead]-Klaus pontoppidan (STScI)(from NASA/Ames)- TBA(from LAM and related Institutes)-Denis Burgarella (Laboratoired'Astrophysique de Marseille)-David Le Miqnant (Laboratoired'Astrophysique de Marseille)- Frederic Zamkotsian (Laboratoired'Astrophysique de Marseille)(from JAXA and related Institutes)-Taro Matsuo (Osaka University)-Keigo Enya (JAXA)-Jun Nishikawa (NAOJ)-Takayuki Kotani (NAOJ)-Olivier Guyon (Subaru Telescope/
Astrobiology Center, NINS/Steward
Observatory, University of Arizona)-Yuji Ikeda (Photocoding)-Naofumi Fujishiro (Teikyou University)-Tomoyasu Yamamuro (Optocraft)-Naoshi Murakami (Hokkaido University)-Yuki Sarugaku (University of Tokyo)-Aoi Takahashi (ISAS/JAXA)-Koji Tsumura (Tohoku University)- And moreInstrument Science Goals andObjectives• Provide	  Mid-­‐Infrared	  (6-­‐38	  µm)	  CapabiliIes	  to	  Address	  the	  Following	  Science	  Goals:	  • Transit	  spectroscopy	  of	  exoplanets	  to	  look	  for	  biogenic	  compounds	  	  (#14)	  • The	  rise	  of	  metals	  (#19)	  • Water	  content	  of	  Planet	  Forming	  Disks	  (#9)	  • The	  ﬁrst	  dust	  (#27)	  • ConnecIon	  between	  black	  hole	  growth	  and	  star	  formaIon	  over	  cosmic	  Ime	  (#21)	  • Birth	  of	  galaxies	  during	  cosmic	  dark	  ages	  (#26)	  • Galaxy	  feedback	  from	  SNe	  and	  AGN	  to	  Z~3	  (#18)	  • Galaxy	  feedback	  mechanisms	  at	  z<1(#5)	  10	  • Jupiter/Saturn	  Analogues	  (#16)	  OST MISC Instrument Requirements
Technical	  Parameter	  Technical	  Requirement	  Technical	  Parameter	  Technical	  Requirement	  Wavelength	  Range	  (microns)	  6um-­‐38um	

N/A	  Detector	  Bandwidth	  Si:As	  :	  6-­‐16.3µm,	  Si:Sb:	  15.4-­‐38µm	  Photometric	  Accuracy	  	  	  	  	  –if	  available	  Angular	  ResoluIon	  <0.25”	  at	  10µm	  Transit	  Monitoring	  Cadence	  One	  measurement/10	  minutes	  Spectral	  Resolving	  Power	  3-­‐300	  (6-­‐38um),	  >1000	  (20-­‐38um),	  10000-­‐20000	  (10-­‐38um)	

Moving	  Target	  Tracking	  Yes,	  up	  to	  1”/second	  Spectral	  Line	  SensiIvity	  (5σ,	  1	  hr)	   2x10-­‐22	  W/m-­‐2	

SensiIvity	  to	  High	  Dynamic	  Range	   N/A	  for	  MISC	  science	  Targets	  ConInuum	  Point	  Source	  SensiIvity	  1µJy	  (@6um,	  R=100)	  10µJy	  (@30um,	  R=100)	  	PolarizaIon	  CapabiliIes	  No	  Broadband,	  Wide-­‐area	  Mapping	  Yes,	  if	  10	  sq.	  deg	  is	  wide	  angle	  Spectrometer	  RelaIve	  CalibraIon	  Accuracy	  3%,	  but	  10	  ppm	  	  λ<10	  µm,	  50	  ppm	  for	  λ>10µm	  for	  transits	Surface	  Brightness	  SensiIvity	  N/A	  Field	  of	  Regard	  (see	  note	  above)	  4	  pi	Instantaneous	  Field	  of	  View	  	  Not	  set	  by	  science	  Field	  of	  View	  Not	  set	  by	  science	

Coronagraphic	  Contrast	  1e-­‐7	  at	  0.5”	  at	  10µm	  Mapping	  Speed	  Not	  set	  by	  science	

Other	  CalibraIon	  /	  Gain	  stability	  [%]	  1%	11	  Mid-­‐Infrared	  Imager,	  Spectrometer	  and	  Coronagraph	  (MISC)	  (ver.20170613)	
(1) Mid-­‐Infrared	  Imager	  Spectrometer	  Module	  	  	  	  	  	  	  	  -­‐	  Wide	  Field	  Imager	  (WFI-­‐S;	  6-­‐19um,	  WFI-­‐L;	  18-­‐38um,	  R=3-­‐10,	  R=100-­‐300)	  	  	  	  	  	  	  -­‐	  Medium	  ResoluIon	  Spectrometer	  (MRS-­‐S;	  5-­‐10um,	  MRS-­‐M;	  9.5-­‐19µm,	  MRS-­‐L;	  18-­‐36um,	  R~1000)	  	  	  	  	  	  	  -­‐	  High	  ResoluIon	  Spectrometer	  (HRS-­‐S;	  12-­‐18um,	  HRS-­‐L;	  25-­‐38um)	  	  	  	  	  	  	  Detectors;	  	  4	  2kx2k	  Si:As,	  2	  1kx1k	  Si:Sb,	  1	  2kx2k	  Si:Sb	  	  	  	  	  	  	  Mechanisms;	  	  wave	  front	  correcIon	  systems	  (DM	  +	  TTM),	  6	  Filter	  Wheels	  (2	  for	  slit	  mirror	  changers,	  4	  for	  imagers	  and	  grisms	  for	  WFI)	  	  	  	  	  	  	  Others;	  IFU	  for	  MRS-­‐S,	  MRS-­‐M	  and	  MRS-­‐L,	  sharing	  the	  same	  FOV,	  	  	  	  	  	  	  	  	  	  WFI	  can	  be	  used	  as	  the	  slit	  viewer	  when	  doing	  spectroscopy	  with	  MRS	  and	  HRS	  	  	  	  	  (2)	  PIAACMC	  Coronagraph	  Module	  (COR)	  	  	  	  	  	  	  -­‐	  PIAACMC	  Coronagraph	  (COR-­‐S;	  6-­‐16um,	  COR-­‐L;	  15-­‐38um,	  R=3-­‐10,	  R=100-­‐300)	  	  	  	  	  	  	  	  Detectors;	  1	  2kx2k	  Si:As	  and	  1	  1kx1k	  Si:Sb	  	  	  	  	  	  	  Mechanisms;	  wave	  front	  correcIon	  systems	  (DM	  +	  TTM),	  4	  Filter	  Wheels	  (3)	  Transit	  Spectroscopy	  Module	  (TRA)	  	  	  	  	  	  	  -­‐	  densiﬁed	  pupil	  spectrometer	  (TRA-­‐S;	  5-­‐8um,	  TRA-­‐M;	  8-­‐14um,	  TRA-­‐L;	  14-­‐26um,	  	  	  	  	  	  	  	  	  	  	  	  R~300)	  12	  	  	  	  	  	  	  Detectors;	  3	  2kx2k	  Si:As	A	  Baseline	  design	  and	  speciﬁcaIon	  of	  OST/MISC	  	  (h#p://exoplanets.astron.s.u-­‐tokyo.ac.jp/OST/MISC/index_misc_case_A.html)	

Mid-­‐Infrared	  Imager,	  Spectrometer,	  Coronagraph	  (MISC)	

Instrument	  TRL’s	  and	  Heritage	  DescripIon	  Subsystem/	  Component	  TRL	  Heritage	  Deformable	  Mirror	

Component	  4	  SPICA/SCI,	  LAM	  Tip	  Tilt	  Mirror	

Component	

4	

SPICA/SCI,	  JWST/NIRCAM,	  TAO/MIMIZUKU	2K	  x	  2K	  Si:As,	  2K	  x	  2K	  Si:Sb	

Component	

2	

SOFIA/FORCAST,	  TMT/MICHI,	  TAO/MIMIZUKU	PIAACMC	  Coronagraph	

Subsystem	

3	8-­‐Octa	  Phase	  Mask	  for	  MIR(8-­‐36um)	  Component	  2	Binary	  Pupil	  Mask	  Coronagraph	

Component	

4	

SPICA/SCI	

Beam	  SpliUer,	  Band-­‐pass	  Filters	  (MulI-­‐
Layer	  Interference	  Filter)	  Component	  4	SPICA/MCS,	  TAO/MIMIZUKU	Image	  Slicer	

Subsystem	

4	SPICA/MCS,	  TMT/MICHI	  Immersion	  graIng	  (12-­‐18µm)	

Component	

4	SPICA/MCS	Immersion	  graIng	  (25-­‐38µm)	

Component	

2	

Densiﬁed	  pupil	  spectrometer	

Subsystem	

3	16