Large  Submillimeter
マスタ タイトルの書式設定
Telescope  (LST)  Basic  Concept
Ryohei Kawabe,  Tai  Oshima(NAOJ)
Kotaro  Kohno,  Yoichi  Tamura(U.  Tokyo)
LST  Working  GroupMm  &  Submm Astronomy  Science  Goals✦ Contributes  over  a  wide  variety  of  science:    e.g.,  Cosmology,  Early  Universe,  Active  Galactic  Nuclei,
Star  Formation,  Interstellar  Chemistry,  Solar  system  and  Planetary  Science;;  challenges  basic  problems  in  the    expanding,  accelerating,  and  diverse  universe  Inflation  &  Big  Bang

Present  age13.7  GyrFirst  Galaxies Large  Scale  Structure
1  Gyr2-­3  Gyr

ALMA  opens  new  era
✦ ALMA    will contribute  to  elucidating  galaxy  formation  and  planet  formation  with  exploiting  extreme  performance-­ High  Angular  Resolution,  ~  0.01  arcsec;;  sharp  radio  images    -­ High  Sensitivity  to  reach  the  early  universe  (also  thanks  to  very  unique  characteristic  of  submillimeter emission  in  SMG)      Hubble  Deep  Field  and  SCUBA  map

3

Gaps  in  Protoplanetary Disks

ALMA  Science  Goals✦ ALMA    will contribute  to  elucidating  galaxy  formation  and  planet  formation  with  exploiting  extreme  performance-­ High  Angular  Resolution,  ~  0.01  arcsec;;  sharp  radio  images    Dreams  come  true!
-­ High  Sensitivity  to  reach  the  early  universe  (also  thanks  to  very  unique  characteristic  of  submillimeter emission  in  SMG)      Hubble  Deep  Field  and  SCUBA  map

4

Gaps  in  Protoplanetary Disks

New  Era  of  Astronomy  will  come  in  the  decade  of  2020!
✦ Advent  of  ALMA
✦ TMT,  EELT  will  start  observations  in  2020
✦ JWST,  SPICA,  Millimetron will  be  launched✦ SKA,  low  radio  frequency   array✦ What  is  the  roles  of  ground-­based  mm/sub-­mm  single  dish  telescope(s)?
-­ Develop  new  discovery  space  complementary   to    ALMA  -­ Incubate  New  Ideas  for  cutting–edge  science  with  ALMA  and  other  big  telescopes

Future Plan  to  built  a new  50  m  class  mm/sub-­mm  single  dish  telescope  (at ALMA  plateau,  Chile)● Ultimate  Wide-­field  Survey(in  Cont.  &  Spectral  Lines)● Time-­domain  Science● Incubate  New  Ideas

Major  Roles  -­-­Develop  new  discovery  space  complementary  to  ALMA
Operation  for    ~30  years  to  exploit  synergies  with  ALMA,  SPICA  and  other  telescopes

NRO  45m    Telescope

Natural  Evolution

ASTE  10  m
Telescope  In  ChieBasic  Concept  :Tentative  Specifications✦ Large  Aperture:  Diameter  =  50  m  less  confusion,  confident  counterpart  ID,  high  sensitivity  for  line  emitter  search  and  point-­like  sources  &  transients  such  as  GRB
✦ Large  FOV
:  F.O.V  =  30  arcmin.  diameter,  Goal  =  1.0  degvery  high  cont.  survey  speed    ✦ Main  Frequency  Range  =  70  – 420  GHz  well  fit  to  Atm windows  &  “Major”  Science  Case
covers  up  to  ~  THz   with  the  limited  use  of  surface    to  maximize  synergy  with  ALMA)✦ total  surface  rms ≤45  μm (El  =  30-­80  deg)  with  Active  surface Control

AzTEC/ASTE  1.1mm  confusion  limited deep  survey
Field

ADF-­‐S

SXDF

SSA22

COSMOSGOODS-­‐S

Coverage(arcmin2)

909

954

973

2967

270

Depth	  (1σ,	
  
mJy)	
  

0.4-­‐0.80

0.5-­‐0.9

0.7-­‐1.3

1.2-­‐2.2

0.5-­‐0.7N	
  sources	
  (>3.5σ)

233

215

125

205

48

references

Hatsukade+	
   Ikarashi+	
  2011,	  Tamura+	
   Aretxaga+	
  2011,	
   Scott	
  +	
  2010,	
  2011,	
  MNRAS,	
   MNRAS,	
  415,	
   2009,	
  Nature,	
   MNRAS,	
  415,	
   MNRAS,	
  405,	
  
411,	
  102
3081
459,	
  61
3831
2260

0.5 deg

AKARI  Deep  Field  South(ADF-­S)SXDFSSA  22COSMOSCOSMOS

Merit  of  Large  Dishes  Source  Confusiona∝ D  -­1.4
Spatial  Resolution              ∝ D  -­ 1.0
Survey  Speedb∝ D2
Speed  of  pointed  obs.    ∝ D4
(for  point-­like  sources)

ASTE      CCAT      new  (50m)    new/CCAT
1
1/3.6          1/10
(1/2.6)    1
1/2.5          1/5                            (1/2)  1
6                  25(4)                136                600
(16)

a. See  Takeuchi,  RK,  Kohno+  2001
b. Evaluated  as  survey  area  covered  with  fixed  observing  time  and  depth,  e.g.,  in  unit  of  deg^2/hours

Basic  Concept  :Tentative  Specifications✦ Other  Detailed  Specification  &  Requirements
Sub-­mm  observations  at  λ<  ~  1  mm
available  for  ~  a  half  in
10  months(Feb.  &  Mar.  are  excluded)see  a  poster  by  Tamura-­san  or  the  LST  website    Collecting  Area

Largest  Active  Surface  Control  Required
45  μm rms needs  careful  thermal  design

2  m
2m  x  1m(or  larger)

Optical  Design  for  wide  FOVvery  preliminary

Richey-­Chretien  Optics  for  D=  50  m  main  reflector
Lyot-­Stop  at  Sub-­refrector:   Deffective ~  46.7  m
FOV  ~  0.7  deg.  in  diameter  at  850  micron  achievable  But…
-­ large  mirrors  Dsub-­ref   ~  6.2  m#3  mirror  ~  7  m  diameter-­ huge  RX  cabin  needed(big  impact  on  telescope
mechanical  structure?)-­ No  aperture  plane@main  reflector  Takekoshi,  Oshima +  Conceptual  Design
Double  Sector  Gears
Receiver  Cabin

Tertiary  &Forth  Mirrors
Collimator  Tower
The  First  Drawing  of  LST  Conceptual  Design
Image  Courtesy  of  Mitsubishi  Electric  Company    Elevator

Conceptual  Design#3,  &  #4  mirrors  limit  the  minimal  size  ofreceiver  cabin..

Top  View
Back  View

Image  Courtesy  of  Mitsubishi  Electric  Company    Chronology  of  LST(or  “ASTE-­II”)

Started  as  a  medium-­scale  future  plan  of  Nobeyama
Radio  Observatory  (45m/ASTE  telescopes)  in  2008/2009
Exchanged    basic  idea  with  JP  astronomy  community  and  outside  potential  future  collaborators  in  terms  of  science,  telescope  specification  and  instruments
Science  case  has  been  investigated  in  working  group  since  Jan.  in  2010  Proposed  the  tentative  plan  as  one  of  medium-­scale  plans  to  Science  Council  of  Japan  (SCJ)  in  2011
Discussed  in/Feedback  from  SCJ  and  NAOJ  steering  committee  of  Radio  Astronomy  etc.    
Concept  and  Science  case  been  updated  in  2014

Science  Goals
Exploring  Obscured  Star  Formation/Evolution  and  also  SMBH  in  the  Early  Universe,  and  also  Large  Scale  Structure(LSS)
Exploring  Star  and  Planet  Formation  &  Chemistry  in  our  Galaxy
Challenging  Time-­Domain  Science  via  GRB/Transient  Search    Confusion-­limited
Deep  Survey  (10-­100  deg^2)
Dusty  Star  Forming  Gals/
Proto-­QSOs
z~  7-­8  GRB
Up  to  z~  10(30?)

Resolve  CIB  in  3D

From  Space
JWST,  SPICA

LST

CMB  or  CMB-­pol  correlateswith  CIB  discrete  sources  via  ISWor  gravitational  lensing?

-­ Spatially  Resolving  CIB  to  DSFGs  down  to  LIRGs    -­ Redshift  Search  of  DSFGs
and  LSS  study  via  CO/[CII]  Tomography;;  can  we  findgalaxies  in  EoR?  
-­ Search  for  Dusty  Sources  (Proto-­QSOs)  powered  by
AGNs  via  CO-­SLED-­ Cosmic  SF  history  together  with  History  of  SMHB  formation/evolution  can  be  investigated-­ Dust/Metal  Production  Beam  Properties  forContinuum  camera:  D=  50  m  Band center

90 GHz3.3 mm

150 GHz2.0 mm

225 GHz
1.3 mm

275 GHz
1.1 mm

350 GHz0.86 mm

405 GHz0.74 mmCoverage[GHz]70-110125-175

200-250250-300

335-365

390-420[mm]

4.3-2.7

2.4-1.7

1.5-1.2

1.2-1.0

0.90-0.82

0.77-0.71

Beam size[arcsec]

16.5

9.9

6.6

5.4

4.2

3.7

Beam size: 1.2×λ/DConfusion-­limited  “Blank  Field”  Survey

LST-­Deep  :  comparable  for  z~  1-­2
>  10  times  deeper  for  z  >  3      VLASS-­Deep;;  0.8”-­ S-­band(2-­4  GHz)-­ 1.5  μJy (1σ)-­ 10  deg^2  -­ 3391  hours-­ N/deg^2  =  9200
LST-­Deep:  5”  beam-­ 1.1  mm  -­ 72  μJy (1σ)-­ 10  deg^2  -­ 870  hours(FOV=0.5  deg.)-­ N/deg^2  ~  20000

Case  1:  simultaneous  3  color  observations
1  deg diameter  FoV is  shared  by  3  bands  (30’  FoV each)  è equivalent  to  ~52’  FoV)
2mm (150GHz)

1.1mm  (275GHz)

860μm  (350GHz)

Beam  size

9.9”

5.4”

4.2”

FoV (diameter)

30’

30’

30’

Mapping  speed

65,100  arcmin2/mJy2/hr

8,000  arcmin2/mJy2/hr

1,730  arcmin2/mJy2/hr

18  deg2/mJy2/hr

2.2  deg2/mJy2/hr

0.48  deg2/mJy2/hr

Sensitivity  (5σ) for 1  deg2 map, 1  hour1.2  mJy

3.4  mJy

7.2  mJy

Sensitivity  (5σ) for 1  deg2 map, 1  min.

9.1  mJy

26  mJy

56  mJy

Confusion  limit  (5σ) #0.13  mJy

0.36  mJy

0.42  mJy

Time  to  a  confusion-­
limited  1  deg2 map

81  hours

87  hours  (1.9×104
sources  expected)

295  hours  (3.0×104
sources  expected)#  based  on  the  number  counts  by  Bethermin et  al.  (2012)  model,
30  beams  per  source.

Case  2:  Single  color  observations  (but  4× higher  mapping   speed)
Only  one  band  can  be  operational,  but  1  deg diameter  FoV2mm (150GHz)

1.1mm  (275GHz)

860μm  (350GHz)

Beam  size

9.9”

5.4”

4.2”

FoV (diameter)

60’

60’

60’

Mapping  speed

260,400  arcmin2/mJy2/hr

32,000  arcmin2/mJy2/hr

6,920  arcmin2/mJy2/hr

72  deg2/mJy2/hr

8.9  deg2/mJy2/hr

1.9  deg2/mJy2/hr

Sensitivity  (5σ) for 1  deg2 map, 1  hour0.6  mJy

1.7  mJy (~400  sources  expected)

3.6  mJy

Sensitivity  (5σ) for 1  deg2 map, 1  min.

4.6  mJy

13  mJy

28  mJy

Confusion  limit  (5σ) #0.13  mJy

0.36  mJy

0.42  mJy

Time  to  a  confusion-­
limited  1  deg2 map

20  hours

22  hours  (1.9×104
sources  expected)

74  hours  (3.0×104
sources  expected)#  based  on  the  number  counts  by  Bethermin et  al.  (2012)  model,  30  beams  per  source.

Galactic  Plane  Survey  LST-­Wide  &  Shallow
10x  shallower-­ 1.1  mm  than  Deep-­ 720  μJy (1σ)-­ 1000  deg^2  -­ 870  hours(FOV=0.5  deg.)-­ 5σ  M(H2)  mass  sensitivity  ~  10  Mjupiter for  d~  150  pc

Continuum-­ “Contamination”  cared
Ntot ~  10^6  (SMG)
N            >  1000  (lensed  SMGs)=>  Shallower  Survey  favorable
3  times  shallower  10  times  wider;;  ~10000  deg2
(core  mass  function  vs IMF)
CfA CO(1-­0)

Survey:Star  Forming
RegionAzTEC/ASTE 1.1  mm

BD  and  PMO  formed  via  (MC)  Core  Accretion?
LST  5”-­resolution  (600  AU  d=120  pc)    imaging
can  search  for  possible  BD/PMO  forming  cores    Spitzer  24micron:  six  YSOs  including  a  VeLLO (#5)

JHK  Composite  (25’  x  40’)    Oasa+  2015  in  prep.  

Galactic  Plane  Survey
spectral  line  case
Next  Generation  Heterodyne  Array  needed✦ LST  GPS  Survey:   Scaled  to  NRO  45m  GPS-­ the  same  line  set  -­ 10x  larger  number  of  beams  -­ 3x    more  sensitive  RX/Telesc (x  6  possibly  realistic)=>  1600  deg^2  with  120  hours  (same  rms)  ✦ NRO  45m  GPS;;  15  ”beam-­ CO(1-­0),  13CO(1-­0),  &  C18O(1-­0)  simultaneously-­ FOREST  4  beam  receiver-­ Planning  160  deg^2  area  with  1200  hours

Pilot  Observationsin  2013-­2014✦ NRO  Galactic  Plane  Survey✦ One  of  the  NRO  45m  Legacy  Project

Minamidani (NRO)  +✦ Revealing  the  missing  links  between  the  Galactic  structures  and  giant  molecular  clouds  through  the  observation  of  interstellar✦ L=10° -­-­ 50°,   198° -­-­ 236°;;  B=±1° (~  160  deg^2)✦ 12CO,   13CO,   C18O   (J=1-­0)✦ NRO   45m  Telescope✦ Angular   resolution:   15”  @  115GHz✦ Three-­year   Legacy   Project   @  NRO   :  2014  -­-­ 2016
✦ Total:   1200  hours
L=12° -­-­ 20°
B=-­1° -­-­ +1°
Red:   12CO(1-­0)
Green:   13CO(1-­0)
Blue:  C18O(1-­0)

Pilot  Observationsin  2013-­2014

8 deg.  X  2  deg

NRO  45m  GPS  Pilot  Observations
Filaments  and  Shells  anywhere

Δv ~  1  km/s
rms ~  0.4  K  (in  Ta*:  typical)  for  Δv ~  1  km/s
Ta*  peak  maps  were  used      Red:  12CO(1-­0)
Green:  13CO(1-­0)
Blue:  C18O(1-­0)

Spectral  Line  Survey  Speed(100  beams,  1  deg2,  0.3K@0.3km/s)
Line

Freq.

Tsys

Beam  (“)
(50m)

Time  
[hr]
(50m)

CO(3-2)13CO(3-2)
C18O(3-2)
CO(2-1)13CO(2-1)
C18O(2-1)
CO(1-0)13CO(1-0)
C18O(1-0)345.796330.588329.331230.538220.399219.56115.271110.201
109.782

140
199
239
91
89
89
130
77
76

4.4
4.6
4.6
6.6
6.9
6.9
13.1
13.7
13.8

10.5
20.2
28.5
2.6
2.4
2.3
3.2
0.8
0.8

Source  Elevation:  68°,  PWV  =  0.913mm,  Dual  polarization

Rich  Science  of  LSTSZ  Cosmology-­ blind  search
Galaxy  Formation   for  high-­z  SZ  cluster Chemical  Evolution&  Evolution,  LSS:  From  core  to  disk  viaCO  &  [CII]  emitter
Spectral  line  survey
Wide-­Field  Search  Imaging
Nearby  galaxies
Large  Survey  of  Milky  Way/SFRs-­e.g.,    CMF  vs IMF
Mm/sub-­mm  VLBI-­ time-­variability  ofaccretion  disk/jet  structure

Time-­domain  Science
GRB  &  Transient-­ GRB  physics-­ diagnostic  of  EoR
-­ unknown  physics(NS  merger  as  GW)

Observing  Frequency  Range  of  LSTPWV:  0.3  mm

New  Telescope
Target  Freq.  Range
0

200

400

Expand  up  to  1  THzwith  Limited-­Use  of  Surface    800

Required  Frequency  Range  of  Each  Science  Case
Wide  Field  Survey
CO  Tomography[CII]  Tomography
SZ  cosmology
Nearby  Galaxies
Line  Survey
Star/Planet  Formation
Mm/submm VLBI

1  THzKey  Instruments
Wide-­Field  Instruments   as  keys  for  Science   Goals  Multi-­chroic (or  single  color)  wide-­field   Camera(s)covering  2,  1.1,  0.85,  (+0.45,  0.35  mm)  Multi-­pix  Imaging  Spectrometer;;   e.g.,  “Super(Hyper)   -­DESHIMA”  with  200  (70)  -­420  GHz  &  Npix (#  of  beams)  of  >  300  (~  1000)  for  [CII]/CO  Tomography
Multi-­band   Heterodyne   Receiver  +  Ultra-­wideband   Spectrometers     (for  line  survey)
Heterodyne   Arrays;;  e.g.,  100,  230,  350,  490  GHz25  -­ ~  100  beams?      LST            LST  from  nowTentative  Goal  in  coming  3-­4  years-­ Propose  LST  as  one  of  big-­scale  plans  to  Science  Council  of  Japan  in  ~  2017  Preparation  for  the  new  proposal-­ Killer  science  should  be  more  sharpened,  also  wide  variety  of  science  case  will  be  planned:
Feedback  to  Telescope  Spec  &  Requirements-­ Planning  telescope  design  study  &  R&D  :planning  in  2015,  R&D  starts  in  2016          -­ Continue  to  exchange  ideas:  collaboration  in  e.g.,  detector  developments,  ..  
Start  construction  from  ~  decade  of  2020
(possibly  immediately  after  completion  of  TMT)

Summary✦ The  Advent  of  New  Decade  of  Discovery  2016-­ start  full  ALMA;;  0.01  arcsec resol
2020-­ TMT,  EELT,  JWST,  SPICA  ..
2020-­ CCAT,  SKA..
2025(?)-­ LST✦ LST can  open  wide-­filed  and  time-­domain  science  in  mm/sub-­mm  wavelengths,  and  can  allow  cutting-­edge  science  via  census  of  universe✦ Also  can  pick  up  very  interesting/extraordinary  sources  for  ALMA  (+TMT/EELT   etc.)  high-­spatial  resolution  imaging,  and  can  enhance   ALMA  science    LMT  50  mlatitude=  19  
deg
45  m
100  GHz
LST~  50  mlat=  -­21  deg

Large  Single  Dishes  in  the  ALMA  Era,
~  2020-­2040
IRAM  
30  m
300  GHzCCAT  25  m

1  THzSPICA  
~  3  mSynergies  withtelescopes  in  space

SPICA/ISAS/JAXA,ESA

LiteBIRD/KEK,   ISAS/JAXA
Inflation  to  Dark  AgeSatellite
Technology

Origin  of  Life
Cosmic  SF
Mm  to  FIRImaging  Spectroscopy
Camera/Detectors
CMB  Secondary
CMB  and  LSS/Dark  matter

LST/JP  Univ.  &NAOJ&  ALMABack-­upAdvantage  of  Singe  Disk  +  Cont.  Camera

Noise  level  achieved  with  SD

Science  Goals  of  LST:  examples
Census  of  SMGs;;  Obscured  Star  Formation-­part  1  -­ Establishing   a  large  sample  of  dusty  forming  galaxies  (SMGs)  at  z=1-­5  (peak  of  cosmic  star  formation)  down  to  SMGs with  “lower”    SFR~  100  Msun/yr
CO  +  [CII]  Tomography;;  Obscured  Star  Formation-­part  2-­ Large  Scale  Structure  (LSS)  up  to  z  ~  5  (or  7?)  -­ CO  Luminosity  Functions  &  CO  SLEDs  for  various  sources  (SBs  &  AGNs)  Census  of  high-­z SZ  clusters  as  high-­mass  end  of  LSSCensus  of  Cores  and  Clumps  in  our  galaxy    Spectral  Line  Survey  for  varisou kinds  of  object;;  disk..
Dynamical  Structure  of  Jets  and  Accretion  disks  (VLBI)

CO/[CII]  Tomography
Science  Goals

Y.Tamura,  K.  Kohno+

LSS  (Large  Scale  Structure)  up  to  z~7CO  Luminosity  Function  at  each  redshift shell;;  L   CO3-­2*
CO  SEDs &  Diagnostics  of  Power  sources  Redshift Space  Distortion  (RSD)  at  z~2  with  10^4  galaxies      Byproduct;;  galaxies  in  EoR might  be  detected  in  [CII]  Survey  Example;;  6  deg^2  Survey  with  D~50m  &  1000  hours-­ Feasibility  study  based  on  S-­cubed  SAX  by  Obreschkow +  2009    -­ assuming  use  of  future  Imaging  Spectrometer  (“Super-­DESHIMA”)  with  300  pix  &  Freq.  coverage  of  70  – 400  GHz
-­ Estimated  Number  Count;;  #  of    detectable  gals  >  10^4  at  z~2  -­ [CII]  can  be  detected  at  z  ~  4  to  7  (EoR)  at  200-­400  GHzSZ  Cosmology;;  Two  Major  Goals
Kitamura,  Komatsu+
High  Spatial  Resolution  Deep  Imaging  of  SZ  clusters-­ resolve  a  core  scale  of  100  kpc and  cover  a    cluster  scale,  10  Mpc
-­ allow  us  to  investigate  the  masses  of  clusters  and  structure  (shock  structure,  energy..)Blind  Search  for  high-­z SZ  cluster  up  to  z ~  2-­ provide  a  large  sample  of  high-­z SZ  clusters,  not  well-­understood-­ allows  to  understand  the  high-­mass  end  of  LSS  at  z  ~  2,  where  Cosmic  SF  activity  start  to  decrease  sharply  toward  z~0.  

Requirements  to  new  telescopehigh  spatial  resolution  =>    10”  at  z~2  &  150  GHz  ,  and  requires  D  ~  50m  Wide  Field  of  View              =>        FOV  of  >  20  arcmin.  

Chemical   Evolution  from  Protostellar Cores
to  Protoplanetary Disks
Yamamoto+

Strategy        (1)  Unbiased  Spectral  Line  Survey  with  a  large  single  dish(2)  Discovery  of  Peculiar  or  Interesting  Objects  (3)  Detailed  Study  of  Chemical  and  Physical  Structure  with  ALMA
(4)  Modeling  and  Comparison  with  Observations
Global  Fit  of  Spectrum    Requirements  to  new  single  dish(1)    High  Sensitivity  =>  Large  Aperture  and  state-­of-­art  RX(2)    Wide  Freq.  Coverage  =>  mm  to  sub-­mm,  good  atm.  
(3)    Large  Instantaneous  Bandwidth  =>  Large  Correlator sys.    
(4)    Reliable  Observations  =  >  Calibration,  Pointing  Accuracy  Large  Surveys  of  Milky  Way  Galaxy
Onishi +Wide-­filed  Survey   or  nearby   Star  forming  regions
Survey   of  Galactic  Plane  Requirements  high  spatial  resolution  for-­ identifying  clumps  at  d~  10  kpc =>    needs  30-­50m  class  telescope  (0.3pc  ~  6”)  -­ investigating  structure  of  envelopes  from  0.1  pc  down  to  1000  AU  =>  (1000  AU  ~  6”  at  d~  150  pc)

Large  Surveys  of  Milky  Way  Galaxy
Onishi +✦ AzTEC/ASTE  1.1  mm  Survey  of  nearby  SF  regions-­ ~20  deg^2  with  5-­20  mJy with  100  hours-­ 4  σ H2  mass  sensitivity  ~  0.05  Msun for  d=150  pc✦ Survey  Speed  (deg^2/hour  with  a  fixed  depth)  ∝ npixD2
D=10  m(ASTE)      =>      D=  35m  npix =  100  (AzTEC)                      1101000                                        10                                                              100                                            10^4                                    100                                                          1000
✦ Example  of  Deeper  Survey  with  new  telescope
Depth  &  #  of  PixelsObserving  time

Survey  Areaσ=  1  mJyNpix =  104

1000  hours

2000  deg2;;  Nearby SF  Regions  with  4σ  mass  ~  0.01  Msun=>  includes  >105-­6 SMGs=>  includes  >103  lensed  SMGs  like  SPT    SMGsMm/submm VLBI  with  LST

Honma +
• BH  shadow  will  be  hopefully  imaged  with  sub-­mm  VLBI  including  ALMA,  sowhat’s  next  ?
• Target  :  “To  trace  dynamic  structure  around  black  holes”
Time  variability  of  accretion  disks  and  jet  roots  around  BHswill  provide  us  the  first  and  unique  opportunity  to  directly  test  the  theories  of  accretion  disk  /  jet  acceleration,  and  also  general  relativistic  effects.
Expected time-­scale
Sgr A*  hours
M87a  few  days
Blazar jets days  to  months

SZ  Cosmology;;  Two  Major  Goals
Kitamura,  Komatsu+
High  Spatial  Resolution  Deep  Imaging  of  SZ  clusters-­ resolve  a  core  scale  of  100  kpc and  cover  a    cluster  scale,  10  Mpc
-­ allow  us  to  investigate  the  masses  of  clusters  and  structure  (shock  structure,  energy..)Blind  Search  for  high-­z SZ  cluster  up  to  z ~  2-­ provide  a  large  sample  of  high-­z SZ  clusters,  not  well-­understood-­ allows  to  understand  the  high-­mass  end  of  LSS  at  z  ~  2,  where  Cosmic  SF  activity  starts  to  decrease  sharply  toward  z~0.  

Requirements  to  new  telescopehigh  spatial  resolution  =>    10”  at  z~2  &  150  GHz  ,  and  requires  D  ~  50m  Wide  Field  of  View              =>        FOV  of  >  20  arcmin.  

?

ALMA
Receiver  Bands

Cyc-­II
Cyc-­?

Cyc-­IIASTE-­II  also  covers  the  same
frequency  range  (except  b-­1)

Cyc-­?
PWV=0.3  mm

The   first  y ear  of  ALMA   Science    12-­15   Dec.  201247