Chines nese An Antarc rctic ic Observ ervat atory ory -- -- - - PowerPoint PPT Presentation

Chines nese An Antarc rctic ic Observ ervat atory

• ry
• - Latest Developments for DATE5

Sheng-Cai Shi & TeSIA Team Purple Mt Observatory, CAS, China Key Lab of Radio Astronomy, CAS, China

• Introduction
• DATE5 Telescope
• THz Superconducting Receivers
• THz Superconducting Imaging Array
• Conclusions

Out utlin line

Dome A

Basi asic fac acts abou about D Dom

• me A

e A

 Altitude: 4093m (60km×10km)  Lowest temp: -83℃  A plateau of small fluctuation  1300km from China’s

Zhongshan station

 Extremely good THz/IR windows

Where is Dome A?

• Low water content (good for THz observations, and

precision photometry)

• Low scintillation error (good for precision photometry)
• Continuous observing (good for time domain astronomy)
• Low atmospheric boundary layer (good for high spatial
• bservations, seeing ~ 0.3 arcsec)
• Low temperature (good for IR observations)
• Aurora
• High relative humidity
• Difficult to access
• Less dark time

Major Relevant Features

The Dome A Site and Recent Development (from L.F. Wang)

Transmission~0.4 @ 1.5THz

Dome A FTS & Results

Dome A Observatory – Roadmap

2006- 2008

Site Survey & Small Telescope

2009- 2011 2011- 2015 2016- 2025

+Site Testing & Middle-size Telescope Dome A Observatory Phase I Dome A Observatory Phase II

2.5m Opt/NIR KDUST 5m THz DATE5 6-8m Opt/NIR 15m THz

preliminary design of DATE5

Antenna enna Cassegrain Diamet eter er 5m, with rms accuracy <10µm Recei eiver er 1x4 superconducting SIS & HEB mixer Band nd 350µm & 200µm IF B F BW 4GHz x 4 beams x 2 bands FOV OV 5′×5′（200µm） Pointi nting ng ≤2"

Quasi Quasi Optic Optics

Antenna enna Subsys bsystem em Rx S Subsy syst stem em

Fr Fronten

• ntend Unit

Unit （H350 & 0 & H H200） IF IF Unit Unit (4GHzx 4GHzx8) LO Units LO Units （H350 H350- & & H200 H200-ab)

Remot

• te C

e Cont ntrol

• l S

Subsy syst stem em

Anten Antenna na

FFTS FFTS (4GHzx8) zx8)

Dome A 5m THz Telescope (DATE5)

Credit: DATE5 science team

 Galaxy formation and evolution  Life cycle of stars/interstellar medium  Origin of planetary systems

Z ULIRGs LIRGs

Major Science Cases for DATE5

All integ ntegrated i in a n a 4K 4K cryos

• stat

tat

H350 band: 350 band: 1x 1x4 S 4 SIS @ 350 350µm H200 band: 200 band: 1x 1x4 H 4 HEB @ @200 200µm IF bandw bandwidth: 4G 4GHz x x 8 Freq eq res esol

• lution
• n: <100k

100kHz

in insi side vie view

Quasi-Optics & Rx of DATE5

H200 HEB mixer TEM image of the HEB microbridge H200 HEB mixer chip

1.4THz Supercond HEB Mixer

5.5 nm 5.5 nm Si NbN SiOx

Nb NbN film t thickness ~ ~5.5nm

0.65~ 5~1. 1.45T 5THz

1.4THz Supercond HEB Mixer

• 5

5

• 30
• 20
• 10

Normalized power(dB) Angle(degree)

simulated-H simulated-E measured-H measured-E

Measured and simulated near-field and far-field beam patterns @ 0.85THz Noise temperatures (uncorrected) measured @ 0.85THz & 1.26THz

Trec=2000K @0.85THz Trec=650K @1.26THz

1x4 beam H350 SIS mixer

0.85THz Supercond SIS Mixer

H350 waveguide SIS mixer circuit

Diagram of 2GHz-bandwidth FFTS Diagram of the algorithm of the FPGA- based 32k channels FFTS

A 2GHz Bandwidth FFTS

A 2GHz-bandwidth FFTS Dyna namic r range ange: ~ 30d 30dB Allan v var ariance ti time: ~ e: ~ 2000 2000s

Combined THz QCL & HEB with a Gas Cell for the detection of 3.5THz methanol line

3.5THz 3rd DFB QCL (by MIT) THz HEB by SRON

Measured 3.5THz methanol line

• Y. Ren, et al., App. Phys. Lett., 97, 161105 (2010)
• Y. Ren, et al., App. Phys. Lett, 98, 231109 (2011)
• Y. Ren, et al., Appl. Phys. Lett. 100, 041111 (2012)

Y.Ren, et al., Appl. Phys. Lett. , 101111 (2012)

SRON/TUDelft PMO MIT …

THz QCL Integrated with HEB

Development of 4K Cryocooler of Low-Power Consumption

Latest cooling result

Developed jointly with SHI Shanghai, with the help of SHI Japan Goal: 1) ~3kW power consumption, 2) able to operate at low temperatures about -20°C and to store at low temperatures about -40°C

SHI HI RDK RDK-205D 05D 0.5W 0.5W @ @ 4.2K 4.2K 5W 5W @ 40K @ 40K

THz HEB by SRON

THz Superconducting Imaging Array (TeSIA)

Det etec ector

• r

TES or MKIDs Arra rray si size ze 32x32 Band and 350µm Sensit itiv ivit ity BGLP, 1x10-16W/Hz0.5

TeSIA

Quasi-

• ptics

TES/ MKIDs LT MUX RT MUX 0.3K/4K Cryocooler DAQ/ Control

TeSIA Developed with TES

TES 8x8 PCB SQUID ASIC RT electronics 1/4K 4K 300K 0.3K

ASIC SQUID TES Array (8x8 @ 850um) w ith TDM

Ti & NbSi Superconducting TES

Measured R-T for Ti (l) & NbSi (r) devices

Ti & NbSi Superconducting TES

Ti TES G=170~ 280 pW/K NEPdark≈6.5e-17W/Hz0.5

2 4 6 8 20 40 60 288 mK Current (µA) Voltage (µV)

NbSi bSi TES G=345 pW/K NEPdark≈5.4e-17W/Hz0.5

TeSIA Developed with MKIDs

0.1~500MHz 4~8.5GHz MKIDs Array (8x8 @ 850um) w ith FDM

Measured 8x8 TiN MKIDs

Measured S21 vs T & P Typical Q~104

Prototype To Be Tested on POST

QMC Dewar Windows M5 M4 M3 Lens Array HDPE Lens 2 HDPE Lens 1

A Newly Built Clean Room Facility

8.5 9.0 9.5 10.0 10.5 0.00 0.02 0.04 0.06

Nb on SiO

2

Resistance (ohm) Temperature (K)

Mask Aligner Sputtering Cluster ICP Etcher

Conclusion

Atmospheric transmission from 0.75-15 THz measured directly ever at Dome A, which is a rather promising site for THz astronomy, First generation instrument for DATE5 telescope will be two heterodyne receivers, and a 32x32 superconducting imaging array at 350 µm (TeSIA) is under development, TeSIA is developed with TES and MKIDs, with TESs demonstrating a dark NEP better than 10-16 and MKIDs a reasonably high quality factor, Prototype imaging array (850 µm ) will be demonstrated

• n POST in 1~2 years.

Ac Acknow

• wle

ledgm gment

CAS & NSFC funding for DomeA Projects CCAA, Polar Institute (China) & PLATO Team (NSWU) for the deployment & operation

• f DomeA FTS

Blue Sky (Canada) and QMC (UK) for good cooperation in developing DomeA FTS Team for CAS’s Int. Collaboration Partnership Program (PMO, CfA, ...) APC/IAS/ASIAA for the fabrication of TES devices RIKEN for the fabrication of MKIDs devices …