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

Chines nese An Antarc rctic ic Observ ervat atory ory -- -- Latest Developments for DATE5 Sheng-Cai Shi & TeSIA Team Purple Mt Observatory, CAS, China Key Lab of Radio Astronomy, CAS, China

Out utlin line • Introduction • DATE5 Telescope • THz Superconducting Receivers • THz Superconducting Imaging Array • Conclusions

Where is Dome A? Basi asic fac acts abou about D Dom ome A e A  Altitude: 4093m (60km × 10km) Dome A  Lowest temp: - 83℃  A plateau of small fluctuation  1300km from China’s Zhongshan station  Extremely good THz/IR windows

The Dome A Site and Recent Development (from L.F. Wang) Major Relevant Features • 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 observations, seeing ~ 0.3 arcsec) • Low temperature (good for IR observations) • Aurora • High relative humidity • Difficult to access • Less dark time

Dome A FTS & Results Transmission~0.4 @ 1.5THz

Dome A Observatory – Roadmap 2006- Site Survey & 2008 Small Telescope 2009- +Site Testing & Middle-size 2011 Telescope 2011- Dome A 5m THz 2.5m Opt/NIR 2015 Observatory DATE5 KDUST Phase I 2016- Dome A 6-8m 2025 15m THz Observatory Opt/NIR Phase II

Dome A 5m THz Telescope (DATE5) Antenna enna Rx S Subsy syst stem em Subsys bsystem em Quasi Quasi Fronten Fr ontend Unit Unit IF IF Unit Unit (4GHzx8) Anten Antenna na Optic Optics （ H350 & 0 & H H200 ） (4GHzx 4GHzx8) FFTS FFTS zx8) LO Units LO Units （ H350 H350- & & H200 H200-ab) Remot ote C e Cont ntrol ol S Subsy syst stem em Antenna enna Cassegrain Diamet eter er 5m, with rms accuracy <10 µ m Recei eiver er 1x4 superconducting SIS & HEB mixer preliminary design of Band nd 350 µ m & 200 µ m DATE5 IF B F BW 4GHz x 4 beams x 2 bands FOV OV 5′ × 5′（ 200 µ m ） Pointi nting ng ≤2"

Major Science Cases for DATE5  Galaxy formation and evolution  Life cycle of stars/interstellar medium  Origin of planetary systems ULIRGs LIRGs Z Credit: DATE5 science team

Quasi-Optics & Rx of DATE5 H350 band: 350 band: 1x 1x4 S 4 SIS @ 350 350 µ m H200 band: 200 band: 1x 1x4 H 4 HEB @ @200 200 µ m IF bandw bandwidth: 4G 4GHz x x 8 Freq eq res esol olution on: <100k 100kHz insi in side vie view All integ ntegrated i in a n a 4K 4K cryos ostat tat

1.4THz Supercond HEB Mixer 0.65~ 5~1. 1.45T 5THz H200 HEB mixer Nb NbN film t thickness ~ ~5.5nm H200 HEB mixer chip 5.5 nm 5.5 nm NbN SiOx TEM image of the HEB Si microbridge

1.4THz Supercond HEB Mixer Trec=2000K @0.85THz 0 simulated-H simulated-E measured-H Trec=650K measured-E Normalized power(dB) -10 @1.26THz -20 -30 -5 0 5 Angle(degree) Measured and simulated near-field and Noise temperatures (uncorrected) far-field beam patterns @ 0.85THz measured @ 0.85THz & 1.26THz

0.85THz Supercond SIS Mixer 1x4 beam H350 SIS mixer H350 waveguide SIS mixer circuit

A 2GHz Bandwidth FFTS Allan v var ariance ti time: ~ e: ~ 2000 2000s Diagram of the algorithm of the FPGA- Diagram of 2GHz-bandwidth FFTS based 32k channels FFTS Dyna namic r range ange: ~ 30d 30dB A 2GHz-bandwidth FFTS

THz QCL Integrated with HEB SRON/TUDelft PMO MIT … 3.5THz 3rd DFB QCL (by MIT) THz HEB by SRON Combined THz QCL & HEB with a Gas Cell for the detection of 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) Measured 3.5THz Y.Ren, et al., Appl. Phys. Lett. , 101111 (2012) methanol line

Development of 4K Cryocooler of Low-Power Consumption 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 Latest cooling result SHI HI RDK RDK-205D 05D 0.5W 0.5W @ @ 4.2K 4.2K 5W 5W @ 40K @ 40K

THz Superconducting Imaging Array (TeSIA) THz HEB by SRON TeSIA Det etec ector or TES or MKIDs Quasi- TES/ LT RT Arra rray si size ze 32x32 optics MKIDs MUX MUX Band and 350 µ m Sensit itiv ivit ity BGLP, 1x10 -16 W/Hz 0.5 0.3K/4K Cryocooler DAQ/ Control

TeSIA Developed with TES TES Array (8x8 @ SQUID ASIC RT electronics 850um) w ith TDM SQUID PCB TES 8x8 0.3K 1/4K 4K 300K ASIC

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

Ti & NbSi Superconducting TES Ti TES G=170~ 280 pW/K NEP dark ≈6.5e -17W/Hz 0.5 60 NbSi bSi TES 288 mK 40 Current ( µ A) G=345 pW/K 20 NEP dark ≈5.4e -17W/Hz 0.5 0 0 2 4 6 8 Voltage ( µ V)

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

Measured 8x8 TiN MKIDs Measured S21 vs T & P Typical Q~10 4

Prototype To Be Tested on POST QMC Dewar M4 M3 Windows Lens Array M5 HDPE Lens 1 HDPE Lens 2

A Newly Built Clean Room Facility Mask Aligner ICP Etcher Sputtering Cluster 0.06 Nb on SiO 2 Resistance (ohm) 0.04 0.02 0.00 8.5 9.0 9.5 10.0 10.5 Temperature (K)

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 µ m (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 µ m ) will be demonstrated on POST in 1~2 years.

Ac Acknow owle ledgm gment CAS & NSFC funding for DomeA Projects CCAA, Polar Institute (China) & PLATO Team (NSWU) for the deployment & operation of 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 …