NOVA submm R&D program A. Baryshev, R. Hesper, A. Khudchenko, J. Barkhof, M. Bekema, P. Dmitriev, K. Rudakov, V. Koshelets, F.P. Mena, R. Finger // SRON/RuG/NOVA/IREE/TUD/UCHILE.

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Presentation transcript:

NOVA submm R&D program A. Baryshev, R. Hesper, A. Khudchenko, J. Barkhof, M. Bekema, P. Dmitriev, K. Rudakov, V. Koshelets, F.P. Mena, R. Finger // SRON/RuG/NOVA/IREE/TUD/UCHILE

NOVA submm group University of Groningen NOVA submm group NOVA submm R&D

Atacama Large Millimeter/Submillimeter Array We developed and made ALMA band 9 and 5 and work on ALMA future developments ALMA array at 5000 m altitude 54 x 12 m diameter dish + 16 x 7 m diameter 30-950 GHz coverage, 10 bands NOVA submm R&D

ALMA science illustration Resolution and sensitivity better than HST HL Tauri © ALMA (ESO,NRAO, NAOJ) TW Hydrae © ALMA (ESO,NRAO, NAOJ) NOVA submm R&D

ALMA system Sky object Telescope SIS mixer Detector chip Front-end NOVA submm R&D

R&D Cycle example, ALMA band 9 example Implementation @ ALMA x 74 Small series production On time, within budget, To specifications Detector R&D Best in the world Receiver design And development NOVA submm R&D

Telescopes LLAMA Argentina APEX telescope CHAMP+ SEPIA FLASH ALMA, Chile, 5000m elevation Millimetron Space Mission/ Origins Space Telescope Large single dish (30M) & ALMA site Dome A?, JCMT?, CSO? Black hole cam/EHT NOVA submm R&D

Submm instruments development ALMA bands 5, 9 CHAMP+ at APEX heterodyne array 2 x 7 pixels in ALMA band 9,10 (650 GHz, 850 GHz window), upgrade just commissioned, guaranteed time APEX SEPIA receiver (ALMA band 9 2SB) APEX FLASH (800-950 GHz receiver) LLAMA (ALMA band 9 and band 5 + front-end AIV) EHT down converter Millimetron space mission/Origin Space Telescope APEX AMKID, a 20kPixel direct detector camera, dual frequency 350/850 GHz NOVA submm R&D

Submm instrument research direction ALMA future 2SB mixer band 9 upgrade Digital front end development Dual frequency receiver development Focal plane arrays Heterodyne detectors Cryogenic SIS detectors works best in submm 2SB SIS mixers (ALMA band 5, 6, 9, 10) Digital backend system Instrument and optics (dual band receiver) Integration IF (4-12 GHz) amplifiers Focal plane array technology HEB+QCL LO distribution and QCL phase locking Direct detectors Kinetic Inductance Detectors (KID)/spectrometers NOVA submm R&D

New 2SB RF block Upgrade ready! Upgrade ready! NOVA submm R&D R. Hesper et al, SPIE 2016 NOVA submm R&D

Digital 2SB Scheme NOVA submm R&D

Digital 2SB IF outputs: Sidebands/FPA … Frontend Digital Calibration/Digitizer system Fiber Optics To correlator 2SB sideband ratio correction Baseline flattening 10dB not a limit Digitization Beam combining FPA Total power spectrometer NOVA submm R&D

Focal plane array challenge FOCAL PLANE ARRAYS CHALLENGE Focal plane array challenge 100 PIXELS, SPACE 1000 PIXELS, GROUND 7 PIXELS NOW Heterodyne Focal Plane Array Workshop / Nanspeet 2017, NL NOVA submm R&D

This program To develop together effective technology for large arrays of Detectors (submm) Amplifiers and interface (1..4-12 GHz) Spectrometer chips & data processing Beam forming… Synergy with SKA MMIC amplifier development

AMKID dual color APEX direct detection camera LFA: 347 GHz ( 34 GHz width, from 330 to 364 GHz / HP width) HFA: 850 GHz (100 GHz width, from 800 to 900 GHz / HP width) squared field of view: > 15 x 15 arcmin2 number of pixels pixel spacing 1 Fλ hexagonal arrangement  3520 pixel in LFA  21600 pixel in HFA detectors operating with sensitivities dominated by the sky background good system stability that allows mapping of extended structures cooling: two 4K pulse-tube closed cycle systems He 10 sorption cooler (<300 mK) MPIfR, SRON, NOVA, TUD Guesten, Heyminck et al NOVA submm R&D

What we do here X 2

Final integration NOVA submm R&D

NOVA ALMA group + SRON APEX <- MMTRON Heterodyne submm instruments development Superconducting detectors ALMA band 9/5, CHAMP+ ALMA future: dual frequency (b9,b6) 2SB receiver (b9 upgrade) digital front-end /FPA ALMA b10, b6, b9 arrays Development -> LLAMA, EHT, ~CCAT, APEX FLASH, SEPIA NOVA ALMA group + SRON Direct detector Development CORE+, OST ~CCAT, MMTRON AMKID 16x16 ArcMin FOV 25kPixel, 350, 850 um APEX <- MMTRON SSB noise temperature 2SB SIS detector sideband ratio