GLT計画の進捗	  と	  今後の日本と台湾の協力への期待	

ASADA, K. (ASIAA)
On behalf of Greenland Telescope Project TeamIn collaboration with ASIAA, SAO/CfA, MIT Hystack Observatory and NRAO

Milestones of Greenland Telescope Project2009: VLBI group was formed, and its primary target is mm/submm VLBI
2010: ASIAA and SAO/CfA, submitted Expression of Interest
to NSF in US for the use of ALMA
2011:	  We	  were	  selected as the recipient and initial inspectionof the telescope was done at VLA site.	  	  First	  trip	  to	  	  	  	  	  	  	  	  	  	  	  	  Greenland	  to	  deploy	  the	  radiometer.	  
2012:	  Disassemble	  the	  antennas.	  	  2013	  -­‐	  2014:	  RetroﬁBng	  the	  telescope.	  
2015:	  Complete	  retroﬁBng	  the	  telescope.	  	  	  	  	  2016:	  TargeHng	  to	  ship	  the	  telescope	  to	  Thule,	  that	  is	  the	  gate	  port	  of	  Greenland,	  	  	  	  	  and	  reassemble	  the	  telescope	  and	  plan	  to	  have	  ﬁrst	  light	  at	  there.	  	Our intension
No rotating BH

Maximum rotating BH

In optically thin flow

In optically thick andgeometrically thin disk

Takahashi 2004

Apparent Size of BH
SourceSgr A*M 87

Cen A

BH Mass

0.045 × 108 M◉

66 (35) × 108 M◉

0.45 × 108 M◉

Distance

0.008 Mpc

16.7 Mpc

3.4 Mpcrs

11 µas

8 (4) µas

0.3 µasSize of Shadow

52 µas40 (20) µas

1.5 µasResoluHon	  ∝	  λ	  /	  D	λ:	  wavelength	  D:	  baseline	

c.f.	  If	  λ	  is	  1	  mm	  (300	  GHz)	  and	  D	  is	  4000	  km,	  	  	  resoluHon	  is	  50	  uas.	  	  	Submm	  VLBI	  is	  the	  only	  way	  to	  achieve	  this	  angular	  resoluHon	  in	  near	  future	  !!	

Logistics of Greenland- Peak of the Greenland ice cap (3,200 m) at 72°35'46.4"N 38°25'19.1”W- Sponsored by the NSF, operated by CH2M Hill Polar Services (CPS)- Camp population: 5 (winter) up to 50 (summer)- Air National Guard provides LC-130 aircraft, twin otter aircraft or traverse.
- Network: Satellite link
We will move 8 km north (downstream of the wind) from current Summit
to avoid contamination and pollution at current Summit.

Expected uv coverage
PdBI	
IRAM 30 m	
LMT	uv coverage for M 87 with Greenland station, SMA,ALMA, SMT, LMT and IRAM 30m. The Baselinewith GL is red.

It will provide 9,000 km baseline,
and it corresponds to 20 uas at 345 GHz!!

Site testing at Summit Camp @ 2011
Our radiometer at the site	So	  far,	  similar	  to	  	  the	  ALMA	  site.	

Disassembly of antenna @ 2012

Retrofitting of telescope

Plan for 2016 and beyond

Readiness for VLBI equipments
SIS	  &	  LNA	  90°	  Phase	  Shi_er	  Bias	  connector	  15K	  plate	  (ALMA)	  110K	  plate	  300K	  plate	  Cold	  OpHcs	  Horn	  &	  Lens	  (ALMA	  Band	  3)	  OMT	  (ALMA	  Band	  3)	  LNA	  &	  Isolator	  High	  Pass	  Filter	  (HPF,	  Cut-­‐oﬀ	  84GHz)	  Double	  Balanced	  Mixer	  IF	  output	   WR10	  LO	  Vacuum	  Through	  (ALMA	  Spec)	  4k	  plate	  Magnets	  15k	  plate	  110k	  plate	  300k	  plate	  Freq.Tripler	  (WR3.4)	  	  JCMT for mm/submm VLBIJCMT	  legacy	  Proposal:	

Strong	  interests	  on	  mm/submm	  VLBI	  from	  the	  community	  in	  Japan,	  Korea,	  China,	  Taiwan.	

NAOJ-ASIAA submm VLBI data workshop- Under the framework of EHT, we had a workshop to transfer the skill to reduce
submm VLBI data in this Aug at ASIAA.
- ASIAA provided minimum but necessary resources (cluster and working env.)
to reduce submm VLBI data- We	  are	  happy	  to	  provide	  this	  funcHon	  to	  community	  in	  the	  	  	  	  	  	  	  	  	  	  	  collaboraHon	  with	  NAOJ/VLBI	  group	  for	  ALMA	  CY4.

M 87 symposium

hip://events.asiaa.sinica.edu.tw/workshop/20160523/index.php	

Job opportunities-­‐	  EACOA	  Fellowships:	  Due	  Nov.	  15th	  -­‐	  ASIAA	  postdoctoral	  Posi?ons:	  Probably	  Due	  Dec.	  15th	  Job opportunities
2015/09/24 10:08

5TWD/JPY

30

1時間

4時間

1日

1週

1月

15

TWD/JPY, 月,

リアルタイム

始値 3.7299 高値 3.7589 安値 3.6309 終値 3.6612

NT$	  <-­‐>	  JPY	  50	  %	  increase	!

10年

5年

3年

1年

3月

1月

7日

1日

%

ログスケールauto-­‐	  EACOA	  Fellowships:	  Due	  Nov.	  15th	  -­‐	  ASIAA	  postdoctoral	  Posi?ons:	  Probably	  Due	  Dec.	  15th	  Summary-­‐	  GLT	  is	  progressing	  -­‐	  Proposal	  to	  prepare	  for	  ALMA	  CY4.	  
-­‐	  Please	  consider	  to	  come	  to	  ASIAA	  as	  the	  visitor	  and/or	  employee,	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  especially	  young,	  middle	  age,	  and	  senior	  persons.	  	Estimated Opacity at Thule by Scott	  	  	  	  	  	  	  	  	  	  	  	  	  tau225	  10	  %	  	  	  	  	  0.096 	  	  25	  %	  	  	  	  	  0.12	  50	  %	  	  	  	  	  0.17	
86	  GHz	230	  GHz	345	  GHz	c.f.	  current	  submm	  VLBI	  observaHons	  have	  been	  conducted	  at	  around	  tau	  ~	  0.2-­‐0.4	  for	  some	  sites.	

MaserOur	  maser	  is	  at	  SPT,	  and	  	  Solid	  Fringe	  are	  detected	  with	  APEX	  !!	  
Risk:	  Low	

ASIAA DiFX correlator
Mk4/DiFX fourfit 3.8 rev 787

M87.yatnor, 085-0525_LOW, eL
CARMARL - SMTOL, fgroup B, pol LL
Fringe quality

97.9
SNR
Int time 480.000
0.147
Amp-123.7
Phase
1.6e-07
PFD
Delays (us)SBD 0.011574
MBD 0.011365
Fringe rate (Hz)0.188827
0.00Ion TEC
Ref freq (MHz)229345.0000
AP (sec) 1.000

Amp. and Phase vs. time for each freq., 12 segs, 40 APs / seg (40.00 sec / seg.), time ticks 60 sec

g26us
Exp.
3428
Exper #
Yr:day 2013:085
Start 052500.00
Stop 053300.00
FRT 052900.00
Corr/FF/build
2015:067:064447
2015:098:052752
2013:095:030006
RA & Dec (J2000)
12h30m49.4234s+12˚23’28.044"

UValidity
Le L

U/Le
Le:L
e:Le
Le
L228881.00 228913.00 228945.00 228977.00 229009.00 229041.00 229073.00 229105.00 229137.00 229169.00 229201.00 229233.00 229265.00 229297.00 229329.00 Freq (MHz)-176.7Phase-174.4-93.0-106.8-114.9-92.6-117.2-162.5-149.0-104.3-145.1-86.2-168.8-39.2-126.6
0.2
Ampl.
0.1
0.2
0.1
0.1
0.2
0.3
0.1
0.2
0.3
0.1
0.2
0.2
0.1
0.1
66.9
Sbd box
30.5
57.0
54.2
35.1
66.7
66.4
9.8
66.1
65.8
60.9
66.6
95.2
27.0
73.9
0/480
0/480
APs used
0/480
0/480
0/480
0/480
0/480
0/480
0/480
0/480
0/480
0/480
0/480
0/480
0/480
00
PC freqs
000000000000000
PC freqs
00000000000000:00:0
PC phase
0:00:00:00:00:00:00:00:00:00:00:00:00:00:00:0Manl PC
0:00:00:0
0:0
0:00:00:0
0:0
0:00:00:0
0:00:01000
1000
PC amp
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
1000
B08LL
B00LL
Chan ids
B01LL
B09LL
B02LL
B10LL
B03LL
B11LL
B04LL
B12LL
B05LL
B13LLB06LL
B14LL
B07LL
Tracks
B08LL
B00LL
Chan ids
B01LL
B09LL
B02LL
B10LL
B03LL
B11LL
B04LL
B12LL
B05LL
B13LL
B06LL
B14LL
B07LL
TracksGroup delay (usec)
Sband delay (usec)
Phase delay (usec)
Delay rate (us/s)
Total phase (deg)ph/seg (deg)amp/seg (%)
ph/frq (deg)amp/frq (%)

RMS
29.5
76.4
31.6
49.1

-1.90550127874E+03-1.90550106989E+03-1.90551264519E+03
1.04469632261E-01-220.0
Theor.
24.2
42.2
27.3
47.6

e: az 113.2 el 45.6 pa -48.5
Control file: cf_3386_low

Apriori delay (usec)
Apriori clock (usec)
Apriori clockrate (us/s)
Apriori rate (us/s)
Apriori accel (us/s/s)

Amplitude
Search (1024X64)
Interp.
Inc. seg. avg.
Inc. frq. avg.

0.147 +/- 0.019
0.127
0.129
0.201
0.157

L: az 116.4 el 53.6 pa -50.0-1.90551264369E+03
3.5459399E+00
8.0000000E-06
1.04468808930E-01
1.17235183890E-05

Resid mbdelay (usec)
Resid sbdelay (usec)
Resid phdelay (usec)
Resid rate (us/s)
Resid phase (deg)1.13650E-02
1.15738E-02-1.49857E-06
8.23331E-07-123.7+/+/+/+/+/-

1.5E-04
2.2E-03
1.8E-07
6.4E-10
14.6

Pcal mode: MANUAL, MANUAL
Pcal period (AP’s) 9999, 9999
Pcal rate: 0.000E+00, 0.000E+00 (us/s)
sb window (us)-0.250Bits/sample: 2
SampCntNorm: enabled
mb window (us)-0.016
Sample rate(MSamp/s): 64
dr window (ns/s) -0.002
Data rate(Mb/s): 1920
nlags: 64
t_cohere infinite ion window (TEC) 0.00

u,v (fr/asec) -1574.794 2048.920

Input file: /asiaa/home/asada/EHT2013_5/1234/085-0525_LOW//eL..yatnor

Output file: Suppressed by test mode

All-123.7
0.2
66.5

0.250
0.016
0.002
0.00

iterative interpolator

Correlated	  with	  ASIAA	  DiFX	  correlator	
Baseline:	  CRAMA	  –	  SMTO	  Frequency:	  230	  GHz	  Source:	  M	  87	  Date:	  2013/3/26	  DuraHon:	  480	  sec	  BW:	  480	  MHz	

Submm VLBI as a tool to study BH
Doeleman et al. 2008

Doeleman et al. 2012

Size ~ 40 µas ~ 4 rs !!	

Sgr A*Size ~ 40 µas ~ 5 rs !!	

Vir A* (M 87)

Submm VLBI is feasible and promising to image the shadow of BH !!